We all knows synths, they make those weird and wonderful electronic sounds we like in so many records from the 1980's right? Yet what are they? When does a keyboard become a synthesiser? Who invented them? And were they sent here by the devil to destroy guitar music?
The history of the synthesiser is a little hard to work out, as how exactly they differ from any other electronic instrument is a matter of much debate. Electronic-eccentric, Wolfgang von Kemplen invented a machine the mimicked human speech back in the 1700's when he wasn't busy building terrifying chess computers, yet not many people would recognise it as a synth in the cool electro-pop wizard sense. The first example of something resembling the modern synth can probably be traced back to around 1930's when The Warbo Formant Organ was invented in Germany by Harald Bode at around the same time as Hammond were releasing the Novachord.
The aforementioned Harald Bode was a key figure in the development and growth of the instrument, inspiring the soon to be legendary Robert Moog to enter the picture in the 1960's. Among the first owners of the Moog was a certain Micky Dolenz, and it was The Monkees who released the first album featuring the instrument, proving a synth alone can't make you sound cool.
These early, and wonderful, analogue synths would go onto be taken over by their digital descendants in the 1970's, ushering in new-wave, synth-pop and Gary Numan. After those heady-synthy days, music kind of got so electronic that the boundaries between synth and computer got blurred. The synth had taken over, the robots had won and the world was never going to be quite the same again. All hail our bleepy-bloopy leaders!
Boston-based songwriter Tony Bullets is a fascinatingly modern purveyor of bedroom-pop songs. His music seems to be completely unaffected by traditional ideas of genre, style or boundaries. The influences are vast; there's nods to the creative beat making of hip-hop, fused with wobbly melodic influences and a lo-fi, bedroom-pop melancholy.
Today, Tony has put together a mixtape for us featuring some of his favourite uses of synths and guitars in the same track, featuring the likes of Mild High Club, Sidney Gish and Inner Wave.
This one drew me in as soon as I hit play, but what really got me was how beautifully the synth, guitar, and vocalist work together during the chorus. And the breakdown at the end needs no description. That junk is marvelous.
Bower is another song where all of the instruments feel very conscious of each other. The space between the chords in the main riff is used so well that it feels like the bass and guitar are having a chat. I also love the reverb on the vocalist, it really makes the song float.
Lately I'm very into loungy vibes and Kokopeli is at the top of that list as one of my favorite swaying songs. The keys are nothing short of hypnotizing and the distorted organ during the chorus has such magical quality to it as it comes in during the key change/modal shift or whatever it is. Very pretty song.
The atmosphere in this song is so sparkly and beautiful. The ride, bells, and guitar all work together to keep up a sort of chiming that continues throughout the song and it has that chorusy sea sick guitar sound that I'm a sucker for.
I could write pages about this song and how much I love what's going on in it. The shift from the guitar being on the upbeat and driving the song forward in the first verse to being right on the 1 in the bridge as the ghostly delayed backup vocals come in just feels right. But my favorite thing about this song is probably how successfully the synthesizer in the chorus emphasizes the quirky sorrow of the vocals.
Sidney Gish is an exceptional lyricist and I feel like it wouldn't do her music justice not to mention it whether or not it needs that intro, but this song in particular is my jam. It's just very playful and very funky. The vocals really hold it down over a very diverse rhytmic section, but my favorite part about this one is the way that it opens up with the fluttering arpeggiated synth that comes in during the drum break.
Spish's album Building a Family is one of my favorite indie releases of 2017 and Bodie is definitely a standout. I love a good story in a song and Bodie feels a lot like a film score, it's captivating. The vocals shamble back and forth with such a heavy hearted vibe and the instruments follow beautifully. The use of strings and bends in the outro of the song also really solidify the vibe. It's all very poetic, 10/10 doctor's would recommend.
Team feels like two pretty distinct songs to me, and the second half is also awesome, as is everything on Saturation 3, but I'm pretty focused on the first half because It's one of the most powerful examples of the singer songwriter side of Brockhampton. It's performed by and I assume written by Bearface and is one of the most incredible evolutions of space I've heard in a song in a long time. From It's beginnings with a single guitar and vocalist to It's climactic ending I love every tone in this song.
Wow is out now. Click HERE for more information on Tony Bullets.


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...&ref=nb_sb_noss_1 PrepareForTakeOff - good thinking!
07:50 AM - yamahacrazy quoted PrepareForTakeOff in post Re: What spark plugs fit the 03 R6???
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Tom Hanchett is something of a local celebrity around Charlotte, in terms of community historians.
When I sat down with him in Arepas Grill, a traditional Venezuelan spot on Old Pineville Road, we were in the midst of our conversation when someone approached Hanchett to introduce themselves. Proclaiming himself a fan, the man was excited to meet Hanchett and exclaimed that he was a big fan of the historical work he has been involved in since first coming to Charlotte in 1981.
Hanchett himself was excited that we were in a traditional Venezuelan restaurant in a city that historically had very little Latinx immigration. He said Charlotte is a city of reinvention, and we're in the middle of a reinvention right now that's bringing more culture to a burgeoning city.
"This reinvention is bringing people from all over the U.S., from all over the world, and suddenly we have in this block, a Venezuelan restaurant, an African market, an Argentinian place with amazing empanadas," he happily said.
In the lead-up to Charlotte's 250th birthday, Queen City Nerve sat down with Hanchett to talk about Charlotte constantly reinventing itself, the impact of newcomers to the city and the celebration of our beloved Queen City.
Q.C. Nerve: How does Charlotte fit into the vision of the New South?
Tom Hanchett: What we said in the Levine Museum of the New South is that if you boil the whole "New South" thing down to one word it's "reinventing." The New South as a term started to happen right after the Civil War. Slavery was gone, the South's economy was in a mess, basically the region had to reinvent itself, and everybody was watching. So it had to be sincere about it. And that keeps happening. We've gone from slavery to segregation, which was a major reinvention. From slavery to segregation to civil rights to where we are now. We've gone from fields to factories to finance.
Here, we've grown every single decade since the railroads came in the 1850s. And that means that we've been too busy building new stuff for anything to get old enough for anyone to think was historic. I'm partly a historian but I think I'm a little contrarian. People don't respect something or want to know the story of it. And in Charlotte, there's tremendous history because people built one big honkin' city here and figuring that out and helping people get turned on to it makes me feel useful and happy.
Charlotte has a lot of "transplants" in the city now, has that always been something Charlotte's been known for?
This has been a city that has welcomed newcomers from the very beginning. In the New South period, one key moment was when the first cotton mill got built. It wasn't built by a Charlottean, it was built by a guy named R. M. Moates, who came here from someplace else and ended up partnering with somebody in Charlotte and they built the building that's still there. It's a historic landmark, on the corner of Graham and 5th Street.
Charlotte has always been a place that welcomes newcomers, that pulled newcomers in. Another great example of that is this guy namedHugh McColl who grew up on a cotton farm down in Bennettsville, South Carolina, came up here was a young trainee at a bank. They had just merged two banks to make something called NCMB and he kind of worked his way up through NCMB until he led the place and reinvented American banking. He created Bank of America here in the '90s, he's another example of someone like me, who was a newcomer who was able to find something useful to do in partnership with the community, and the community embraced him.
So, in the spirit of the Queen City's 250th birthday, what about our history should we embrace as we move forward?
It's kind of typical of Charlotte that there has been a good effort on celebration, but it hasn't really swept the city's culture like it might in more history-oriented communities. This is part of the New South is embracing the future, running toward the future with open arms. I've been kind of quietly proud of charlotte and CLT250 effort.
Let's make something of this. It's an opportunity for us to do what is really hard if you're a person on the make, if you're an ambitious person, if you're a person really engaged in the day-to-day making of a new world which so many folks are here for. Whether you're in a corporate world or the parent track or building a nonprofit, whatever. The tasks right in front of you seem more important than sitting down for an afternoon and having some birthday cake.


If it's not every week, it's every two weeks that we hear reports of a healthcare security breach and despite the healthcare regulations, we still have health systems that don't seem to take data protection seriously enough or health systems that don't build a security program into their businesses to ready against potential hacking.
We hear breach statistics in almost every article, circling the twittersphere, on every slide deck, on every webinar, or at every conference. But just once more, let's look at why healthcare is a target.
In 2014, there were four times as many breaches in the healthcare sector than any other industry. Other industries include education, banking, financial, and government sectors. Some have suggested that the reason hackers are turning their efforts to the healthcare industry is because other industries are getting better at securing their data.
However, in healthcare, the profit potential is another factor.
Hacking healthcare data is a lucrative practice; health data is worth more on the black market than any other data set. It makes sense that so many healthcare organizations are a target, but that's also what makes this alarming. That, and it's incredibly easy to hack with the lack of healthcare security practices we have in place today.
Grab a blank sheet of paper and draw a box. Let's say this "box" is your health system. List what security program you have in place today. Write the estimated amount of patient data you have stored. This is who you are protecting. Are your security efforts sufficient? For healthcare, I'm going to guess no because most organizations don't even know where most of their data lives! Okay, now list what you could do to improve your program. Now if every CIO shared this piece of paper, what would it look like? It might look a lot like a checklist: risk assessment, technical testing, security controls review, information security review, performance monitoring, and governance.
We could "checklist" our way to "security" or even add a little governance in our program to show that we are meeting regulation with meaning, but if the threats keep coming, and we can't keep up, so does the need for not just improvement, but security transformation and a security culture.
It's your health system, your organization, your security team, its actionable practices, a continuous process improvement, cyber security. It's creating security longevity, a dedicated security trainer, a security culture, and a functioning business unit. It is your mindset.
A CISO is critical within a healthcare organization and never more so than now. Healthcare's complex data extends far and wide; from patients and wearables, to clinicians and employees accessing sensitive data on mobile devices. Not having a CISO in a sizable health system will not sit well with OCR should you be selected for audit. It is a first implementation step if you do not have one.
Implementing your security team outside of the IT Dept.
Security has become bigger than the IT department and requires a transformation from a technical asset to a business process that needs it's own team and perspectives, and should act as risk advisors. A CISO, like the CIO, must understand the business. And an effective security program has the understanding of security outcomes, creates an evolution process, collaboratively documents business process, quantifies security risks, and automates the process.
Establish a senior risk advisory council that consists of senior level executives that includes the CISO…and actually meet! These meetings develop procedures and best practices and record votes, which builds culture. Together, create your program and build in more of an understanding that, when making decisions, you look at the risks associated with the decisions. This team should become more cognizant that culture will help better execute your strategy.
What are the goals of the program and how do you get there? Build a new privacy and security roadmap that drives toward program advancement and a defensible resource plan such as cyber security preparedness. Ideas include the placement of a security staff member to stay on the 'front lines' of cyber threats, developments in policy, technology trends, and also have a dedicated team member to provide employee education and training on a quarterly basis. They are key players on your team that help fight against phishing and social engineering and also trending technologies.
Grow your security team to ready for potential hacking and establish a program with enough staff to consistently work in the future with rejuvenating processes in effort to prepare for tomorrow. As of today, most health systems are not proactive and some have the mindset that they'd rather just budget for when they do encounter a breach instead of protecting patient data. It's flat out wrong. Also, when a breach does occur, scrambling to hire additional skillsets is hard to find on short notice. Build early, grow your team in advance.
*HIMSS reported in their cyber security study that 62% of respondents said there were too many new threats to keep track of.
Keeping pace with threats and technological trends is almost impossible, but is essential to your organization security practices and key in fighting against hacktivists. Just as in sports, when you're focused on your goal, you're ready for what comes at you creating performance. Sometimes you win and sometimes you're outperformed. Either way you're lessening the impact and will only get better. This is the mindset healthcare security executives should be practicing.
The current model risk assessment is inefficient and does not create ongoing visibility. As health systems use risk assessments and technical testing to assess our program, we need to provide our health systems with a better, more informed risk assessment. In order to meet compliance audits, it's best to use an independent third-party to ensure adequate compliance and professional visibility. However, your health system risk posture cannot be formulated or determined by a third-party, only you or your executives can establish a risk profile.
Keeping pace with cybersecurity, phishing attacks and the latest business and technology trends requires an information security team overhaul.
Now is the time to engage in awareness and readiness in your security program. We are seeing the largest incidences in healthcare breaches than we have ever seen before and at a pace we can't keep up with. An evolving security program will level up security processes, making them high priority to the business as an ongoing process. Not only that, but also continually re-evaluates to ensure effectiveness. This and being on the 'front lines' when it comes to your program effectiveness, helping you become more resilient across the security ecosphere.
We have to take value in taking our programs beyond no program at all. For example, we cannot defend against phishing if only 5% of our workforce is defending against it.


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https://www.barrons.com/news/scientists-hunt-for-genetic-key-to-virus-vulnerability-01588782003
Scientists Hunt For Genetic Key To Virus Vulnerability
Amélie BOTTOLLIER-DEPOIS
Why are some people barely affected by coronavirus, while others become gravely ill even though they are young and healthy?
Scientists are searching for answers in patients' genes, looking for mutations that affect their immune response in the hope of finding new treatments.
As more people become infected with the virus, a rough profile of a severely-affected patient has emerged: older, with underlying illnesses and more likely to be male.
But that is far from the full picture.
Intensive care units around the world have also treated a minority of people who are under 50 with no underlying medical problems.
These roughly five percent of patients are the ones that interest geneticist Jean-Laurent Casanova.
"Someone who could have run the marathon in October 2019 and yet in April 2020 is in intensive care, intubated and ventilated," he told AFP.
Casanova, director of the human genetics of infectious diseases laboratory jointly based at the Imagine Institute in Paris and Rockefeller University in New York, wants to find out if they have rare genetic mutations.
"The assumption is that these patients have genetic variations that are silent until the virus is encountered," he said.
Casanova co-founded the COVID Human Genetics Effort, which is seeking to study the genome of these severely-ill younger patients in places like China, Iran, Europe, North America and Japan.
The group is also looking at people who do not become infected despite repeated exposure.
Their research is among a huge global effort involving dozens of labs scouring the genomes of COVID-19 patients for variations that might explain why some people get sicker than others -- and potentially help develop anti-viral therapies.
Gene mutations have been found to make people more vulnerable to a range of infectious diseases, from influenza to viral encephalitis.
They can sometimes also offer protection.
In the mid 1990s researchers discovered that certain rare mutations of a single gene (CCR5) effectively stopped people from becoming infected with HIV.
The discovery gave researchers a greater understanding of the way the virus worked and paved the way for the development of new treatments.
In the past, whether a person became seriously ill with a particular disease was often put down to "bad luck", said Jacques Fellay, a professor of human genomics of infectious diseases at the Federal Polytechnic of Lausanne.
"Today, we have the capacity to go and dissect the genome of these people and see if they have a rare mutation which could make them particularly susceptible" to the new coronavirus, he told AFP.
But differences in immune response are often caused by multiple genetic factors, Fellay said, likening the body's defence mechanism to a mechanical watch.
"There can be a grain of sand in the cogs. Among a group of patients, each of these grains of sand can be different, but produce the same result", he said.
This complexity means "we need to have a very large sample and collaboration, and the ability to repeat the observation to be confident about the results," said Mark Daly, director of the Institute for Molecular Medicine Finland.
Daly is one of the scientists behind the COVID-19 Host Genetics Initiative, a large-scale global collaboration involving some 150 research centres.
The project aims to recruit at least 10,000 patients and share findings.
Researchers hope to have "very useful information" by the summer, he said, although the timeline is by no means guaranteed.
Ideally the work would lead to treatments.
"There are a huge number of medicines available that target specific genes," Daly told AFP.
"If we find a genetic clue that points us to a gene that already has a medication developed, then we could simply repurpose the drug."
But the process could be much more complicated.
Researchers may find mutations in genes that have not had drugs developed for them -- potentially lengthening the time to create a treatment, said Fellay.
Or worse, they may find that the mutations are not "actionable", or that interventions would create too many side effects.
Discovering the genetic mutations behind immune responses to COVID-19, then, is only the beginning.
"Genetics is a tool for exploring biology, but the resulting treatment, there is nothing genetic about it," he said.
abd/klm/pg/jv

redpajama_set_name: RedPajamaCommonCrawl


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Japan Material International Scholarships 2022
Jun 8, 2022 Material International Scholarships
~ Material International Scholarships ~
Tokyo Institute of Technology is now accepting applications from suitably qualified students for their Material International Scholarships. It is a fully-funded scholarship for all students.
Tokyo Institute of Technology is a national research university, one of the top Public universities in Tokyo, Japan ranked 56th in QS Global World Rankings 2021.
The institute contributes to civilization, peace, and prosperity in the world.
Institute of Technology aims at developing global human capabilities par excellence through pioneering research and education in science and technology, including industrial and social management.
It is working to promote world-class research by encouraging international collaborative projects and building an international research environment.
Aim and Benefits of Material International Scholarships
The Tokyo Institute of Technology will select the winning students and will provide them a sum of 100,000 YEN per month for the duration of their study.
Requirements for Material International Scholarships
The applicants must be international students with communicable Japanese proficiency.
See also Apply Now: Kansas State University Future Student Scholarships 2023-2024
Flinders University Mendelson Scholarships 2022


A Book Review of The Fix-It Man by Dimity Powell.
It's an unfortunate fact of life that children often begin to learn about loss and grief from an early age, and it can difficult for parents and carers to know how to handle it.
The Fix-It Man is a lovely picture book that offers a gentle way for adults to discuss loss, love, and grief with their child.
The story focuses on a young girl who has a sick mother, and believes that her father can fix everything. But sadly, when her mother passes away, she realises that mending a broken heart isn't a simple thing to do. Together with her dad, she finds a way to cope with their loss.
I read this book to my two younger daughters and they (and I) were so touched by it. We had a discussion afterwards about the story, and I answered questions that they both had about losing a loved one.
They both loved the illustrations (the book is illustrated by Nicky Johnston), and went back over the pages as we were having our talk.
I think that this is a fantastic book for those wanting to help teach their child about loss.


I looked forward to my birthday every summer with great anticipation.
We'd choose our favorite foods or menu or meal.
And we'd choose chocolate or white or yellow cake. Because as Julia Child says, "A party without a cake is just a meeting.
My mother would bake up the cake in a 9×13 Pyrex and we'd whip frosting and layer across the top.
The absolute best part to me.
Every year we picked out Wilton edible hard candy icing decorations to place on top of our cake.
I loved gazing at those pressed plastic packages inside the grocery store aisle. Yellow rose flowers or red? Did I want one that said Happy Birthday? Which one was my top-of-the-list-favorite this year? Decision made, we'd trek to the checkout.
With the cake baked and frosted, we'd open the candy icing decoration package and carefully work through the process of dampening the back of the paper so we could peel off the molded shapes.
Deciding where I wanted to place each particular candy on the canvas expanse of vanilla frosting.
Fast forward across a few years and I find myself celebrating forty this month, and a friend celebrated with me by baking and decorating, a gorgeous and delicious, white birthday cake, complete with frosting flowers and a carefully numbered 40 on top.
It was a fun surprise and late evening as I snuggled in my chair with my feet tucked under me, I contemplated that it had been a very long time since anyone had baked me a birthday cake.
It doesn't matter that I don't always have a birthday cake anymore, made by someone else.
Yet, it was super fun! And definitely delicious! Somewhere through the years of birthday cakes and choosing chocolate or yellow or white, my absolute favorite choice became white cake. I love me a moist, white birthday cake or wedding cake slice!
Perhaps we grow up and we grow out of traditions.
Sometimes 900 miles separates you from your mama. Perhaps the years roll around so quickly, we can hardly believe it's time for cake again.
But there's one thing I don't think any of us outgrow no matter what we tell ourselves.
How meaningful it is when someone we love blesses us with an act of kindness.
The cake WAS delicious and beautiful. But the sacrifice of time and effort on the part of my friend was even more beautiful. She's busy. She has littles and a lovely home and a husband and several of her own siblings and many things filling her to-do list.
Kindness comes in so many forms.
The blessedness of kindness wears so many faces.
It's in baked birthday cakes.
Years ago, by my mother. This year, by my friend. It's in the taking time to let your daughter choose that treasured candy cake topper package, clutching it eagerly through the grocery checkout line.
The blessing of kindness takes form in birthday packages filled with forty gift items. It's called red roses as well as wildflower bouquets. It's as simple as picking up my phone and sending a happy day text. It's in asking your friend how they would like to celebrate and what would bless them. It's slipping your hand inside another's and squeezing out I love you. It's giving of time and taking time. It's the email, the happy mail.
Basically, the blessing of kindness is in looking deeper and realizing the sacrifice and care and time given on my behalf by another who was willing to take the time, make the time, bake the cake, choose the flowers, arrange the flowers, write the note, tap out the text, speak the words, do the thing, little or big, to make my life happier.
Not a bit of it is insignificant.
Children delight in birthdays and celebration, and also, innocently take for granted the work and kindness and love put into them. They haven't grown into the wisdom and age of seeing it.
I certainly haven't perfected it or cleared away the smokiness of the glass I look through, yet the older I get the better I see it. The easier it is to pause and look deeper, longer, harder.
To see underneath the swirl of the frosting and TAKE NOTE of the kindness flowing through every second of every stroke.
To notice it in every dotted "i" and every ink smudge on the envelope.
To glimpse it in each painstakingly placed Perler bead. Bead after bead laid upon the form, then pressed and heated by a little person's mama to melt and meld into a fish shape and become a gift!
To detect it in every tap it took to send the text through.
To note it every time I pull a paper straw out of the package included in my gift of forty items.
To spy it in the pointy edges of the succulent my daughter placed on my kitchen island for me.
To feel it flow from the edge of the sheet lifted up by my man for me to more easily climb into bed.
To appreciate the effort and care in the brownies dropped off at my door.
To whisper grateful over the time put in by a friend to organize an outing and celebrate with me.
To hear it in every note of the birthday melody recording left on my voicemail. Aged voice and lisping words joined together in beautiful harmony.
To catch it AND feel it in shared laughter spilling out in happy notes.
To touch it as I slit open the envelopes I found in my mailbox.
And here's the thing I think about kindnesses and blessings. They multiply. We take them in and we're compelled to pass them on. As I become more aware, I can't help but spill it out onto others.
Sharing and caring and passing it forward brings another whole wave of smiles and blessing.
These things we never, never outgrow.
This is so enjoyable to read!! I love how you put words together.
Thank you so much! It was fun to remember!!! Thank-you for making life fun!
what a wonderful post. you are so right about kindness coming in so many forms. I love Julia Chillds quote. I look forward to every December. This year I will be 60. Woohoo what a wonderful number. And life has its way of changes. We have gone through so many in the last 2 years. But what blessings all. Thank you for sharing today.
I love your line about giving an 'I love you' through a hand- in-hand squeeze.
This is such a sweet post. It reminds me of my family's own birthday tradition when Mama would cook whatever we wanted. It was never fancy, but it was one of the best meals of the year.
Great post. I'm glad I found it today (via the Tell His Story linkup).
Thank you so much for coming by and for your kind words! Good memories are such a blessing!
How true that kindness takes on many different looks every day!
Beautiful cake! Happy birthday! What a blessing to learn we never outgrow the gift of kindness.


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The  was a terrorist bombing that occurred on 23 October 1972. It was undertaken by a group which would soon be known as the East Asia Anti-Japan Armed Front, though this name was not decided on until later in the same year.

The targets
The Fusetsu no Gunzo, literally the Wind and Snow Group, is a bronze monument produced by the Japanese sculptors Shin Hongo and Meiji Honda located in Tokiwa Park in Asahikawa, Hokkaido. It depicts four Japanese colonists surrounding an elderly Ainu and was a project marking the 80th anniversary of the city and the 100th anniversary of Hokkaido's formation. The Institute of Northern Cultures is the Ainu cultural research center of Hokkaido University.

The Institute of Northern Cultures is an institute of Hokkaido University concerned with the research of Ainu culture.

The East Asia Anti-Japan Armed Front considered these two targets symbols of Japan's imperialistic aggression against the "Ainu Moshiri" or Ainu homeland, and decided to blow them up. Masashi Daidoji in particular, the Hokkaido-born leading member of the plotters, had a special interest in the Japanese-Ainu conflict.

They set 23 October as the date of the bombing. This was the date on which Ainu chief Shakushain, who started Shakushain's Revolt, was murdered by the Matsumae Clan.

The bombing
They split into two groups and arrived in Hokkaido on 23 October 1972. They each proceeded directly to their site and set the explosion for 11:30 PM. Both bombs exploded on time, and the Fusetsu no Gunzo was destroyed but the Institute of Northern Cultures escaped with relatively minor damage.

In 1977 the Fusetsu no Gunzo was restored and it remains in place to the present day.

References

Bibliography
 Ryuichi Matsushita『狼煙を見よ 東アジア反日武装戦線"狼"部隊』
 (読売新聞社・戦後ニッポンを読む、1997)
 (河出書房新社・松下竜一その仕事22、2000)

1972 in Japan
October 1972 events in Asia
Terrorist incidents in Japan in 1972
1972 crimes in Japan

redpajama_set_name: RedPajamaWikipedia


Enjoy this smooth and creamy delight any time of the day with the distinctive taste of Irish Cream. All the joy of your favourite creamy liqueur at just 2 calories per cup! Try Irish Cream with frothy milk, serve over ice or add it to a protein shake for a pre-workout superboost!


KANSAS CITY, MO – April 5 (SEND2PRESS NEWSWIRE) — Lumen Software, a leader in AJAX / LAMP+ middleware, announced today it will release Lumenation v6.0 and its SDK LightBulb free to users. The user role based middleware environment / framework, coupled with Lumen's mature AJAX z-Windows engine, provides developers with the ability to rapidly create scalable, high end browser based applications.
Lumenation provides a cohesive user role based environment and framework developers need to rapidly build highly scalable, robust commercial grade applications. The middleware includes the Lumenation Interactive Desktop System (LIDS) and Lumen Interactive Components (IC's), which utilize Lumen's AJAX z-Windows engine, delivering fat client functionality in a browser. The platform offers secure roles based access to applications and disparate databases utilizing an array of administrative tools which greatly simplify and automate all aspects of user, application, journaling and other management processes required by any application or solution.
A few of the features developers and organizations alike will benefit from include the interactive "presentation" of legacy data, managed simultaneous database access (Oracle, MySQL, DB2, Microsoft), local / remote secure file management, a complete system data dictionary, localization and more. In Lumenation's next release, users will have the ability to access and manage the base computer's applications and files.
Lumen Software provides a Lumenation / LAMP+ stack installation process directly from the company's website for Novell SuSE, RedHat and other distributions, benefiting both new users and experienced Linux veterans. With JAVA in place for the larger organizations and Lumenation positioned to fill in the rest of the market, Linux now has the power to put choices back into the hands of users worldwide.
Lumen Software is a world leader in browser based technologies and author of Lumenation, a LAMP+ based enterprise environment / framework which utilizes Lumen Software's z-Windows AJAX desktop and graphical engine. The Company provides a cohesive role based environment / framework organizations need to collaborate, deliver web based applications, manage content and rapidly build commercial grade applications.
Linux is a registered trademark of Linus Torvalds. All other third-party trademarks are the property of their respective owners.


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We're proud to host another type of "life science" tenant at Menlo Park Labs: beautiful Italian honey bees and beehives from Alvéole, the urban beekeeping company. Thousands of our new colleagues joined the existing bee population on campus in early 2020 to pollinate the urban flora that surrounds us during the summer. At the end of the season, we harvest their honey in a sustainable way and share it with our community.
The global bee population is in serious danger, and that means our entire food system is too. We partnered with Alvéole to help protect this vital part of our ecosystem. Alvéole has worked with hundreds of companies and schools on beekeeping projects across the U.S. and Canada to nurture and grow the bee population. Their work is creating greater ecological awareness, allowing city dwellers to reconnect with nature and heighten their sense of responsibility towards the environment.
Worried about stings? Don't be. Bees aren't really interested in humans. They have one goal, and one goal only: to collect nectar and pollen from flowers within a three-mile radius of their hive, and bring it back to ensure the colony's development. The Italian bees in our hives are also extremely docile and known to be good neighbors.
We offer Menlo Park Labs tenants numerous opportunities to get involved with our urban beekeeping project, including workshops, learning events and more.
If you would like to hear more about the Alveolee bee hives, please visit alveole.buzz/en/
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Evergreens absorb and diffuse noise from traffic and industrial activity.
1 Are Evergreen Trees Effective in Reducing Traffic Noise?
One of the important contributions evergreens can make to landscaping is the abatement of noise. While exact correlations between planting evergreens and reducing decibels of environmental noise remain in question, there is general agreement that evergreens, often in conjunction with other noise-abatement measures, soften, diffuse and diminish irritating noises from traffic, industrial activity or even the neighbors. Use evergreen trees and shrubs to create a quieter and more restful outdoor environment in your yard.
Studies by the United States Federal Highway Administration suggest that, while solid barriers such as walls, earth berms and buildings insulate neighboring residential areas from noise more effectively than plants, natural plantings have two major affects on the perception of noise. One is measurable noise reduction, estimated at between 3 and 5 decibels per 100 feet of thickness of a planted barrier. Other studies document greater noise reduction from placing a planted barrier close to the source of the noise rather than close to the source of perception. According to arborist Andrew Johnson, noise generated by traffic under 40 miles an hour can be reduced by planting a 20- to 50-foot-wide buffer within 20 to 50 feet of the traffic lane closest to the property being buffered. A similar barrier must be 65 to 100 feet wide to abate noise from traffic traveling faster than 40 mph. Combining evergreen planting with raised earth berms increases abatement potential.
The most powerful impact of evergreen planting for noise-abatement appears to be psychological, according to the U.S. FHWA. Visual screening of noise sources reduces their perceived impact. Getting noise sources out of sight as well as out of hearing is a strategy employed by residential, industrial and transportation planners at all levels. The State of California has gone so far as to make a Noise Element feature a legal requirement for all general development urban and rural plans. Together with a required Landscape Element, planning must address using plantings that are fire resistant, pest resistant and high in habitat value as well as useful for noise and noise-perception screening.
Several characteristics distinguish plants that function effectively in a sound-buffering plan. Since a noise-impacted residence may be located above the noise source, plant height is important to creating an effective barrier. Other valuable qualities include thick fleshy leaves, abundant branches and branches that reach to the ground, so that a planted screen does not lose its effectiveness when plants grow. Above all, year-round durability makes a major contribution to noise buffering.
Numerous evergreens fulfill the criteria, but long life and easy maintenance are best assured by choosing trees and tall shrubs native to your area and climate zone. Natives possess strong resistance to pests and need less water and fertilizer than non-native plants. In areas where fire resistance is an issue, native plants may be required for certain areas. Your community's general plan may require or restrict the varieties of evergreens you can use for noise and other screening.
California native evergreens include cypresses and pines. Native pines, among them ponderosa, knobcone, bishop, Monterey and gray pine, grow to mature heights of between 40 and 50 feet. Cypresses, including tecate and piute, grow to between 15 and 30 feet and are often well suited to dry locations. Plants that can be treated like multistemmed trees or large woody shrubs include Pacific wax myrtles, which can grow to 15 feet in height and a similar width and are valued as soil nitrogen-fixers. Manzanitas form a large family of tough bushy native evergreen shrubs ranging in size from 3 to 10 feet. Combining native evergreen trees with an under layer of evergreen shrubs can increase the density of your buffer at the trunk area of potentially tall trees.
Beal, Janet. "Evergreen Sound-Buffering Trees." Home Guides | SF Gate, http://homeguides.sfgate.com/evergreen-soundbuffering-trees-29999.html. Accessed 25 April 2019.


The use of sensors to monitor individuals' wellbeing is set to take off agreed Roy Grant of York Council, Mark Low of Pinacl Solutions and Karantis 306's Nick Hampson, in the recent CLGdotTV discussion on care in the home.
PwC UK drones lead Elaine Whyte, Dedrone's Amit Samani and Tris Dyson of Nesta discuss the economic and social potential of drones and whether public anxieties might be allayed through regulation and control by public authorities.
In typical 'smart city' discussions, agreed our panel, most of the people around the table are from organisations and represent sectors like education, energy, retail, and transport, and in these discussions, people are reduced to personas like 'commuter' or 'consumer'.
Jason Kitcat (Essex CC) Richard Farrell of Netcall and Sleuth Co-op's Hilary Simpson discuss how local authorities might overcome challenges of legacy systems, digital skill shortages and the persistence of old-style procurement.


text:
Jerusalem Post WORLD NEWS
US: Baggage handlers sneak drugs, guns onto plane
Two airline baggage handlers used their employee uniforms and identification cards to carry a duffel bag loaded with guns and drugs into a plane's passenger cabin, bypassing security screeners, according to court documents. Passengers on the Delta flight from Florida to Puerto Rico were in little danger despite more than a dozen guns being on board, because at least two federal air marshals were also on the plane, a Transportation Security Administration spokesman said Thursday. TSA spokesman Christopher White declined to address the security breach or whether the marshals knew that guns were on the plane. He said multiple marshals were on the plane, but declined to specify how many. Thomas Anthony Munoz, 22, was arrested when he got off the plane in San Juan, while Zabdiel J. Santiago Balaguer, 22, was arrested late Tuesday and remained in custody Thursday in the Orange County Jail.


" As parents, we are impressed with the way the school has a really good community feel to it. Our particular highlights have included Sports Day, the fete, school camp, concerts... And of course the wonderful plays that include all the children!
" I just wanted to say how much I enjoyed and appreciated the newsletter from the catering team. It was lovely to get such detail about what goes into the preparation of the children's meals. It is obvious that much thought and effort goes into making the mealtimes nutritious and tasty. Being sent copies of the menus too, was very helpful. It makes it so much easier when talking to my young daughter about (or trying to find out!) what she had for lunch.
" I just wanted to say a big thank you to all the staff involved in today's Science Day... They (Jess and Charlie) loved moving around the school from one activity to another and a particular highlight seems to have been a mummified teacher at the end of the day!


Down a very narrow lane between Georges Hill and Halston Street, this commercial premises may started out as a schoolhouse before being used for sometime as a parish hall for St.
A fine old pub façade which still shows the location of the original corner entrance. This is now blocked up and converted to two windows but the original decorative corbells on the signage still exist.
A former National School, the small building is now the home of the Greek Orthodox congregation in Dublin.
A fine presbytery house sited next to its church. Now facing across the public park created on the site of Newgate Gaol.
Large stone-faced commercial building with a rather grim facade.
Formerly the Motor Tax office, now empty, and possibly awaiting demolition. Abhorantly ugly development that was slated for demolition and redevelopment into an even more horrible building.
In 2004, VHI appointed McCauley Daye O'Connell to prepare a design to create a new high quality contemporary extension to its existing VHI Headquarters which incorporated Scot's Church and also provides much needed additional office floor space.


text:
Q: WebClient accessing page with credentials I am trying to access a webpage on a same domain / same asp.net application, that is password protected. Credentials are the same both for webpage firing this call and webpage being accessed.
Here is the code, and I don't know why I always end up with a login form html code?
using (WebClient client = new WebClient())
{
    client.QueryString.Add("ID", "1040"); //add parameters
    //client.Credentials = CredentialCache.DefaultCredentials;
    //I tried to add credentials like this
    client.Credentials = new NetworkCredential("username", "password");

    string htmlCode = client.DownloadString("http://domain.loc/testpage.aspx");
}

A: I suspect that the web page that you are trying to access uses Forms Authentication. This means that you will have to provide a valid authentication cookie if you want to be able to access protected resources. And in order to obtain a valid authentication cookie you will have to first authenticate yourself by sending a POST request to the LogOn page which emits the cookie. Once you retrieve the cookie you will be able to send it along on subsequent requests on protected resources. You should also note that out of the box WebClient doesn't support cookies. For this reason you could write a custom cookie aware web client:
public class CookieAwareWebClient : WebClient
{
    public CookieAwareWebClient()
    {
        CookieContainer = new CookieContainer();
    }
    public CookieContainer CookieContainer { get; private set; }

    protected override WebRequest GetWebRequest(Uri address)
    {
        var request = (HttpWebRequest)base.GetWebRequest(address);
        request.CookieContainer = CookieContainer;
        return request;
    }
}

Now you could use this client to fire off the 2 requests:
using (var client = new CookieAwareWebClient())
{
    var values = new NameValueCollection
    {
        { "username", "john" },
        { "password", "secret" },
    };
    client.UploadValues("http://domain.loc/logon.aspx", values);

    // If the previous call succeeded we now have a valid authentication cookie
    // so we could download the protected page
    string result = client.DownloadString("http://domain.loc/testpage.aspx");
}

Obviously due to the ViewState crapiness of ASP.NET you might need to send a couple of other parameters along your logon request. Here's what you could do: authenticate in a web browser and look with FireBug the exact parameters and headers that need to be sent.

redpajama_set_name: RedPajamaStackExchange


Mamelodi Sundowns coach Pitso Mosimane says he expected the Champions League showdown against Moroccan side Wydad Casablanca to be a highly charged affair and the match lived up to his expectations at the Lucas Moripe Stadium on Saturday night.
The Brazilians won the match 2-1 courtesy of a brace from Themba Zwane but it was marked by emotions and tension between the two sides.
"Unfortunately when we played them here last year we made mistakes' but this time we had ink in our system'" he said.
"The mentality was very good.
"We played the way they always play at home and let's be honest' we were the better team on the pitch.
"To be honest' the score is not a true reflection of the game because we had so many opportunities to seal it and I was not happy because I knew it could come back to bite us.
The win enabled the Brazilians to get their Champions League campaign back on track after a poor start to the group stages that saw them let a lead slip to lose 2-1 to Lobi Stars of Nigeria at the Nnamdi Azikiwe Stadium in Enugu last week.
"We want nice football to get people to the stadium and also to watch on television but the Champions League sometimes is not about nice football'" Mosimane said.
"Guys are maturing' they played this game the way it was supposed to be played and it is about results.
"We scored two goals and it could have been different.
"But it also shows the quality of Wydad because they scored from nowhere.
"It is not the same game you saw against Maritzburg and I am sure you know what is going to happen to us when we go to Morocco and it is the last match but we are ready for that.


text:
\section{Introduction}

It is widely accepted now that solar active regions (ARs) are a manifestation of emerged portions of subphotospheric toroidal magnetic flux \citep{Parker1955}. The magnetic field that forms active regions is generated somewhere in the convection zone (CZ) in the processes collectively called the solar dynamo. The conditions in the tachocline at the base of the CZ allow the magnetic flux being amplified by stretching and wrapping of magnetic field lines by the differential rotation (the so-called ``$\Omega$ effect'') and the action of turbulent convection ($\alpha$-effect) \citep[e.g.,][]{Babcock1961,Ossendrijver2003,Charbonneau2005,Charbonneau2010,Charbonneau2014,Brun2015,Ferriz-Mas1994,Ferriz-Mas2007}.
In addition to amplification, the magnetic field get organized into a concentrations referred to as flux tubes, in which the individual field lines are linked together by wrapping around other field lines. While the exact mechanisms leading to formation of flux tubes are not well-understood yet, the concept is used widely in representing the
dynamics and properties of strong magnetic fields on the Sun. After the flux tube is formed, one of its portion
may become unstable and start rising to the surface due to buoyancy \citep{Parker1975,Fan2004}. The process starts when the magnetic pressure inside the magnetic flux tube becomes comparable to the gas pressure, i.e. when the magnetic field inside the tubes reaches certain threshold value of about 10\textsuperscript{5} G \citep[e.g.][]{Caligari1995}.
In a simplified picture, the rising part of a flux tube forms co-called $\Omega$-loop with upper part moving to the surface, and its footpoints remaining tied to deep
layers of the convection zone.
Crossing the visible  layer of the solar
atmosphere (photosphere), these magnetic tubes manifest themselves in observational phenomenon called solar active regions (ARs).
The dynamo can also act in the bulk of the CZ or even in a near-surface shear layer \citep[e.g.,][]{Krause.Raedler1980,Brandenburg2005,Stein2012,Nelson2014}. Other mechanisms may also play role
in the formation of strong magnetic flux. For example, \citet{Brandenburg2016} showed that the
bipolar magnetic regions can be formed due to negative effective magnetic pressure instability
from thin magnetic flux tubes that presumably exist throughout the stratified CZ. Alternative
mechanisms of formation of sunspots (and active regions) at/near visible solar surface by the
photospheric dynamo had also been proposed
\citep{Gurevich.Lebedinsky1946,Akasofu1984,Henoux.Somov1987,Henoux.Somov1991}, but currently,
those mechanisms are unable to reproduce several major observational properties of sunspot groups
(e.g., Hale polarity rule and latitudinal behavior of tilt angles of sunspot groups) and thus,
are not widely accepted.

In past studies, considerable attention was paid to the observational aspects of development (emergence) of new ARs. \citet{Zwaan1985} and \citet{Brants1985} found that during the initial stage of the emergence a strong transverse magnetic field of the rising magnetic tube apex is observed. This was later confirmed by \citet{Lites1998} who also found ``a low canopy of weak horizontal magnetic field arches over the emergence zone''. As active region develops, small-scale features with magnetic fields of opposite polarities appear near its central part and move to opposite ends of the emerging flux region to form rapidly-growing footpoints of future AR \citep{Zwaan1985,Centeno2012}.
The magnetic field strength in the emerging flux elements is about several hundred gauss, and the strength increases up to kilogauss range when they become vertically oriented \citep{Lites1998}.

Recent numerical modeling indicates that when an $\Omega$-loop
reaches near surface layers, it expands
significantly and emerges in a less coherent pattern, similar to the observed evolution of
emerging regions.
The whole AR may be formed of several $\Omega$-loops, each one emerges individually
\citep{Otsuji2011,Abramenko2017}. As a rule, the same polarities of these $\Omega$-loops
gradually merge together to form the AR's footpoints. For a comprehensive observational
description of AR's formation and evolution, see reviews by \citet{vanDrielGesztelyi2015} and
\citet{Cheung2017}. Movie of emergence of a small active region based on Hinode
observations can be found at \url{https://www.youtube.com/watch?v=oFF7xdcEMFg}.

The process of magnetic flux formation and rising through the CZ is inaccessible for direct observations. Helioseismology can detect rising magnetic structure inside the CZ \citep[e.g.][]{Birch2013}, however this approach still provides limited data on magnetic fields \citep{Chen2017}. This is why our knowledge on magnetic flux emergence from the bottom of the CZ almost completely relies on theoretical deductions and numerical simulations.
\citet{Schuessler1979} performed two-dimensional magnetohydrodynamic (MHD) simulations of flux
emergence from the base of the CZ and found that the differential rotation is a suitable
mechanism for magnetic field amplification. He also concluded that the rising flux tube
eventually distorts and fragments into two vortex rolls. This may cancel the lifting
force of magnetic buoyancy that was considered in detail by \citet{Longcope1996}. Studies of
thin toroidal flux tube emergence by \citet{Choudhuri1987} and \citet{DSilva1993} showed that
the Coriolis force may be responsible for ARs' tilt. These findings were confirmed in 3D
numerical simulation of emerging flux loops evolution by \citet{Fan1993}. The authors also
simulated the asymmetry of the leading and of the following polarities that is widely observed in
real AR: the leading sunspot tends to be more coherent than the following one \citep[e.g.]
[]{McIntosh1981,Tlatov.etal2015}. Similar results were obtained by \citet{Caligari1995} who
treated the dynamics of emerging magnetic flux tubes using the thin flux tube approximation
proposed by \citet{Spruit1981}. \citet{Emonet1998} carried out numerical MHD simulations of a
twisted magnetic tube rising inside a stratified medium. They found that the twist of magnetic
tube can suppress the fragmentation of the tube into two vortex rolls described by
\citet{Schuessler1979} and \citet{Longcope1996}.

\citet{Archontis2004} proposed the ``two-step'' emergence model of the magnetic flux tube rising from the upper layers of the solar interior into the solar corona. The model was elaborated later by \citet{Toriumi2011}. In the framework of the model, at the first step magnetic flux tube rises through the CZ due to magnetic buoyancy and slows down as it reaches just below the photosphere where the background plasma pressure falls dramatically. A horizontal layer of unmagnetized plasma trapped between the solar surface and the magnetic flux tube prevents further rising. The magnetic flux tube expands significantly in the horizontal direction, its rise halts. At the second step, horizontal sheet of magnetic flux breaks into the photosphere and further into the corona either due to magnetic buoyancy instability or due to buffeting by plasma convective motions \citep{Archontis2004,Norton2017}. \citet{Toriumi2013} predicted a divergent horizontal flow of the trapped plasma from the emerging site that was later observationally confirmed by \citet{Toriumi2014}.

\citet{Cheung2007} and \citet{Cheung2008} carried out radiative 3D MHD simulations of emerging magnetic flux from the near-surface layer of the CZ into photosphere. Magnetic flux of the simulated tubes did not exceed 1.55$\times$10\textsuperscript{20} Mx. By taking into account compressibility, radiative transfer and partial ionization, the authors simulated the flux tube undulations that were associated with interaction between the granular convection cells and the flattened magnetic sheet.

\citet{Cheung2010} presented first radiative MHD simulations of AR emergence from the uppermost 7.5 Mm of the CZ. The simulations were carried out with the MURaM code \citep{Vogler2005, Rempel2009} that takes into account realistic equation of state. Similar study was performed by \citet{Rempel2014}, this time authors extended the model by including a retrograde flow in the flux tube and by using larger computational domain. In both works, a semitorus-shaped magnetic flux tube was advected into the computational domain through the bottom boundary. The most pronounced features of AR's emergence, such as horizontal expansion of magnetic flux tube, undulating field lines between the opposite polarities, leading and following polarities asymmetry and its coalescence from small-scale magnetic features were simulated. Interestingly, \citet{Rempel2014} showed that completely untwisted magnetic flux tube is able to rise through the uppermost 15.5 Mm of the CZ and to form sunspots.

The reader can see that most simulations consider either the uppermost layers of the CZ and solar atmosphere or the Sun's interior from the bottom of the CZ to several tens of Mm below the photosphere. This is a consequence of a density variation by 6 orders of magnitude with the CZ depth from the bottom to the top and, as a result, of significant variations of time and length scales \citep{Cheung2010}. This difficulty was overcome by \citet{Chen2017} who carried out the state-of-the-art simulations of an emergence of a magnetic flux bundle generated at the bottom of the CZ. Instead of advecting an ideal semi-torus tube through the bottom boundary of the computational domain, authors introduced magnetic and flow fields obtained near the top boundary of convective dynamo simulation by \citet{Fan2014}. This allowed \citet{Chen2017} to perform a more realistic simulation that could be compared to observable ARs, which led to the following conclusions:
\begin{enumerate}
\item{} The magnetic flux bundle rises as almost a coherent structure. Approaching the solar surface, the flux bundle fragments into small granular-size magnetic elements. The elements emerge individually and coalesce into a large flux concentration.
\item{} Asymmetry of leading and following polarities are explained by stronger vertical magnetic field of the leading spot inside the CZ that is caused by a combination of vertical motions of plasma inside rising flux tube (due to drainage from loop top) and the prograde flow inside he emerging flux bundle.
\item{} Emergence of magnetic flux is controlled by convective upflows inside the CZ, i.e. the rising speed of a magnetic tube is determined by the mean upflow speed of plasma in convective cells.
\end{enumerate}

Additional reviews on magnetic flux tube emergence can be found elsewhere \citep[e.g.,][]{Fan2004,Fan2009,Archontis2012,Cheung2014}.

In our present study, we focus on a flux emergence rate $R(t)=d\Phi(t)/dt$, where $\Phi(t)$ is
the total magnetic flux of the emerging flux bundle, and its relation with other magnetic
parameters.
\citet{Otsuji2011} carried out a statistical study of 101 flux emerging regions ranging from
small magnetic dipoles of 2.6$\times$10\textsuperscript{17} Mx to strong ARs of 6.7$\times$10
\textsuperscript{21} Mx. They found that the flux emergence rate is proportional to the peak
total magnetic flux, $\Phi\textsubscript{max}$:
\begin{equation}
R=d\Phi(t)/dt\propto\Phi_{max}^\kappa
\label{eq1}
\end{equation}
By fitting their $d\Phi(t)/dt$ versus $\Phi\textsubscript{max}$ scatter plot, \citet{Otsuji2011} obtained that the power-law index $\kappa$ in \eqref{eq1} equals 0.57.
The authors also derived the value of the power-law index $\kappa$ in the framework of a very simplified model. The model considered emergence of a flattened magnetic flux tube with a constant rise velocity. Since the plasma $\beta$ in the photosphere is almost 1 and the magnetic pressure $B^2/8\pi$ is almost constant, the magnetic flux density inside the tube was supposed to be constant irrespective of the spatial size or total magnetic flux of the flux tube. In such a case, the relation between the peak flux and flux emergence rate is described by equation \eqref{eq1} with the power-law index $\kappa$=0.5.

Even more emerging events, namely 224, were analysed by \citet{Khlystova2013} during the first 12
hours of emergence. Although \citet{Khlystova2013} did not evaluated the power-law index
$\kappa$ in her $d\Phi(t)/dt$ versus $\Phi\textsubscript{max}$ relation, a scatter plot in
fig.~8 of her article allowed \citet{Abramenko2017} to estimate the value of $\kappa$ to be of
about 0.4.

\citet{Fu2016} studied the influence of emerging magnetic flux on the flaring activity of the
pre-existed ARs. They determined the flux emergence rate of 116 ARs, although did not carry out
any analysis of these values. Interestingly, \citet{Fu2016} found that about half of the regions
exhibited a two-step emergence behavior when the flux emergence rate was relatively low at the
initial stages of the emergence and significantly increased as the emergence proceeded.
\citet{Norton2017} analysed the magnetic flux variations of 10 emerging ARs separately in leading
and following sunspots. The observations also covered the decaying phase where possible. The
authors concluded that the flux emergence rate of the leading spot in AR is on average higher
than that of the following spot. Combining their results and others reported previously,
\citet{Norton2017} evaluated the power-law index $\kappa$ to be 0.36. \citet{Abramenko2017}
measured the flux emergence rate for 36 ARs. Their $d\Phi(t)/dt$ versus
$\Phi\textsubscript{max}$ relation fitting resulted in the power-law index $\kappa=0.69\pm 0.10$
for the whole ARs sample.

The flux emergence rate, often reported in Mx~hr\textsuperscript{-1}, usually varies from units
to tens of 10\textsuperscript{19} Mx~hr\textsuperscript{-1} for emerging magnetic bundles of
different magnetic fluxes. Observed and simulated rates are in a good agreement, and we refer
reader to an excellent detailed review of this issue made by \citet{Norton2017}. However, there
are still some points that need to be clarified. \citet{Abramenko2017} noted that the flux
emergence rate of ARs of almost the same total magnetic flux can differ significantly. This
implies that the flux emergence rate also depends on some other properties of an AR rather than
on its maximum total unsigned flux only.

The aim of this work is to find possible relations between different parameters of emerging ARs using a statistically significant sample of events. We especially focus on physical quantities that can affect the flux emergence rate of an AR. The most promising quantity in this context (except $\Phi\textsubscript{max}$) is the magnetic tube's twist. A number of theoretical studies, which simulated magnetic flux tube emergence \citep[e.g.][]{Moreno-Insertis1996, Emonet1998, Magara2001, Murray2006, Toriumi2011}, suggest that higher initial twist of a magnetic tube may result in a higher flux emergence rate. Briefly, twist of the magnetic tube prevents its fragmentation by the plasma convective flows and formation of vortex rolls mentioned above \citep{Schuessler1979, Longcope1996}. \citet{Toriumi2011} argued that insufficient twist of a magnetic tube can lead to a ``failed emergence'' when the flux tube expands too widely beneath the photosphere, looses its buoyancy and becomes unable to break through the surface. In general, \citet{Cheung2007} showed that the ability of magnetic flux tube to emerge through the surface depends on the tube's twist. Currently, there are no observational studies to support or disprove the existence of relation between the magnetic flux tube's twist and its flux emergence rate. The present study is an attempt to fill this gap.

\section{Data reduction and calculation of active-region parameters}

We employ solar magnetic field measurements by the Helioseismic and Magnetic Imager \citep[HMI,][]{Schou2012, Scherrer2012} on board the Solar Dynamics Observatory \citep[SDO, ][]{Pesnell2012}. Among other products, SDO/HMI provides full-disc 4096$\times$4096 pixel line-of-sight (LOS) magnetograms with the spatial sampling of
0.5$\times$0.5 arcsec$^2$ pixel size
and a 720 second cadence.

To create a series of patches of AR LOS magnetic field maps we applied the following procedure.
The boundaries of the desired AR were manually selected at the full-disc magnetogram. By a cross-
correlation technique, the AR was kept inside the bounding box at the consecutive (both back and
forth in time) full-disc magnetograms as long as the centre of the bounding box was located at
the central meridian distance (CMD) less than 60\degr.

The AR's magnetic field inside the box were extracted and saved to patches along with the
coordinates of the box boundaries. At the following steps, these coordinates were used to derive
the information on the AR position on the solar disc.

The total unsigned flux of an AR $\Phi(t)$ was calculated as a sum of absolute magnetic flux density in pixels multiplied by pixel's area corrected for projection. We summed only those pixels whose absolute magnetic flux density values were more than 18 Mx~cm\textsuperscript{-2}, i.e. threefold exceeded the noise level of LOS 720s magnetograms \citep{Liu2012}. Assuming the magnetic field to be predominantly radial the total unsigned flux of each patch was corrected for the foreshortening by dividing by the cosine of the angle between the line-of-sight and the radial direction at the patch centre (the $\mu$-correction). The reliability of the estimation of the radial magnetic field $B_{r}$ from the LOS component $B_{los}$ by the $\mu$-correction is related to how radial the real magnetic field is. This issue was analysed by \cite{Leka2017} who compared different technique of $B_{r}$ approximation from $B_{los}$. They considered $B_{r}$ derived from the SDO/HMI vector magnetic field measurements to be a true radial field. The authors found that the $\mu$-correction provides the best estimation of the total unsigned flux in ARs from the $B_{los}$ component for $\cos(\mu)\gid0.5$ \citep[see Fig.~11 in ][]{Leka2017}. In early stages of magnetic flux emergence, the emerging site is comprised mostly of plage areas in which the magnetic field is close to radial.
In later stages, when the horizontal field of sunspots develops, $\mu$-correction method will underestimate the
total magnetic flux. However, based on \citet{Leka2017}, the effect of this underestimate on total unsigned flux
of active region is relatively small.

The SDO/HMI team also provides the Spaceweather HMI Active Region Patches \citep[SHARPs,][]{Bobra2014,
Hoeksema2014} derived from full-disc HMI data. To produce SHARPs, a feature-recognition algorithm
\citep{Turmon2010} automatically identifies and tracks ARs at full disc magnetograms. SHARP
products contain maps of AR's LOS and vector magnetic fields, continuum intensity, Doppler
velocities, etc. In addition, a number of AR indices such as the total unsigned flux,
characteristic twist parameter, mean vertical current density, and others are computed from the
vector magnetic field in AR patches.  The SHARP vector magnetic filed data were used to calculate
exclusively twist of magnetic flux tubes for two reasons. First, many SHARP patches enclose more
than one AR, i.e., in such a case, we cannot attribute any AR parameter derived from this patch
to a certain AR. Second, SHARP tracking algorithm often starts to track emerging AR after the
actual emergence onset, i.e. we can lose information at the very beginning of the emergence.

Note that we did not use the SDO/HMI vector magnetic field data to calculate the ARs' total unsigned fluxes. The main reason is a relatively high noise in full-vector measurements. Absolute magnetic flux density below 220 Mx~cm\textsuperscript{-2} in vector magnetograms should be considered as a noise \citep{Bobra2014}. \cite{Norton2017} found that the noise in the SDO/HMI Stokes vector profiles varies with increasing centre-to-limb observing angles. This causes a ``mexican hat'' trend in the total unsigned flux curve (see fig.~5 in \citealt{Hoeksema2014} and fig.~4, panel A4 in \citealt{Bobra2014}) as an AR crosses the solar disc. \cite{Norton2017} suppressed this trend by using a high noise threshold of 575 Mx~cm\textsuperscript{-2}. However, this decision led to an underestimation of the magnetic fluxes. We cannot follow \cite{Norton2017} and increase the threshold since we intend to add to our analysis weak ARs that do not form sunspots.

There are two more minor points against using vector magnetic field measurements for $\Phi(t)$ calculations in this work. First, \cite{Leka2017} argued that the total unsigned flux derived from the vector magnetograms is overestimated due to higher noise in the transverse magnetic field. This noise is summed by its absolute value and makes some contribution to the total unsigned magnetic flux. In our case, this contribution might be significant for weak ARs. Second, as we mentioned above, SHARP tracking algorithm often starts to track an AR after its actual emergence onset. Using vector magnetic field measurements would require padding such SHARP series with additional patches in order to create a homogeneous data series covering the whole AR emergence process. To create these patches, one have to deal with full-disc vector magnetograms that consume four time more memory space compared to LOS magnetograms.

\begin{figure*}
	\includegraphics[width=\linewidth]{figure1.eps}
	\caption{a - Variations of the total unsigned magnetic flux $\Phi(t)$ (black curve) of AR NOAA 12266 (HMI SHARP 5075). Blue and red curves show the best piece-wise linear fitting of the $\Phi(t)$ curve during the emergence onset and peak magnetic flux, respectively. Intersection of the segments of these fittings (pointed by gray arrows) determines $t_{emerg}$ and $t_{max}$, see text. b - LOS magnetogram of the patch of AR NOAA 12266 taken by SDO/HMI at $t_{emerg}$ on 2015 January 17 at 12:36 UT. Initial imprints of AR emergence are visible at the centre of the patch. c - LOS magnetogram of the patch of AR NOAA 12266 taken by SDO/HMI at $t_{max}$ on 2015 January 19 at 12:00 UT. Red crosses denotes the positions of flux-weighted centroids of opposite polarities. The field-of-view of the patches is 150\arcsec$\times$75\arcsec. The magnetograms are scaled from -500 Mx~cm\textsuperscript{-2} (black) to 500 Mx~cm\textsuperscript{-2}.}
\label{fig1}
\end{figure*}

Using a series of extracted by ourselves $B_{los}$ patches, for each AR we determined the following parameters:
\begin{enumerate}
\item{}
\textit{Time of the emergence onset, $t_{emerg}$.} To determine the time of the emergence onset we performed a two-segment piecewise continuous linear fitting of the $\Phi(t)$ curve in the interval where the total unsigned flux started to increase (blue curve in Fig.~\ref{fig1}a). The first (left-hand in Fig.~\ref{fig1}a) segment had to be horizontal while the second one could have arbitrary slope. We define the intersection point of the segments as a time of the emergence onset.
\item{}
\textit{The time of AR's maximum magnetic flux, $t_{max}$} was determined as a time when the emergence halts and the $\Phi(t)$ curve reaches its maximum value. Similar to the previous point, we determined this time as an intersection of two segments of the piece-wise continuous fitting of the top of the $\Phi(t)$ curve (red curve in Fig.~\ref{fig1}a). In this case, the second (right-hand) segment had to be horizontal.

\item{}
\textit{The maximum total unsigned magnetic flux} or peak magnetic flux of an AR, \textit{$\Phi_{max}$}  was computed as a difference between the value of $\Phi(t)$ at the emergence onset and the value of $\Phi(t)$ during the $t_{max}$: $\Phi_{max}=\Phi(t_{max})-\Phi(t_{emerg})$. To decrease the uncertainty, we use the averaged values of $\Phi(t)$ at the horizontal segments of the piece-wise linear fittings.
\item{}
\textit{The averaged flux emergence rate, $R_{av}$} was computed as
the maximum total unsigned flux of an AR divided by the total interval of the flux growth
\begin{equation}
R_{av}=\Phi_{max}/(t_{max}-t_{emerg}),
\label{eq2}
\end{equation}
\item{}
\textit{The normalized flux emergence rate, $R_{n}$}. Previous studies \citep[e.g.][]{Otsuji2011,Abramenko2017,Norton2017}
revealed that the flux emergence rate depends on the peak flux of an AR with stronger ARs exhibiting higher absolute flux emergence rate as
compared to weak ones. To mitigate this effect and to treat the strong and weak ARs as a single ensemble, we introduce the normalized flux
emergence rate, $R_{n}$

\begin{equation}
R_{n}=R_{av}/\Phi_{max}^{\kappa}.
\label{eq13}
\end{equation}

$R_{n}$ is a measure of flux emergence rate that is independent of the peak magnetic flux of an AR. As it will be shown in Sec.~\ref{sec_all_vs_phimax} a value $\kappa=0.5$ can be adopted. Formally, the units of $R_{n}$ in this case are Mx\textsuperscript{1/2}~h\textsuperscript{-1}. For simplicity, we will measure $R_{n}$ in arbitrary units.
\item{}
\textit{Longitude of the emergence onset}. We adopt the heliographic Stonyhurst longitude \citep{Thompson2006} of the centre of an AR patch at the time of the emergence onset as the longitude of the emergence onset. All the heliographic coordinates were calculated with the World Coordinate System (\textsc{WCS}) routines provided in the \textsc{SolarSoft IDL}.
\item{}
\textit{Longitude and latitude of an AR at $t_{max}$, $LON_{max}$ and $LAT_{max}$}. For each AR patch we calculated the flux-weighted centroids of each polarity at $t_{max}$

\begin{equation}
(x_{\pm}, y_{\pm})=\bigg( \frac{\sum{x~B_{\pm}}}{\sum{B_{\pm}}}, \frac{\sum{y~B_{\pm}}}{\sum{B_{\pm}}} \bigg),
\label{eq3}
\end{equation}
where $B_{\pm}$ is the magnetic flux density in each pixel and $x$,$y$ are pixels' coordinates. The sign +~(-) denotes calculation only over positive (negative) polarity. To decrease the influence of quiet-Sun fields, we only used pixels with absolute values exceeding 300 Mx~cm\textsuperscript{-2}. We define the heliographic latitude and longitude of the centre of the line connecting the flux-weighted centroids as $lat_{max}$ and $lon_{max}$, respectively.
\item{}
\textit{The opposite polarity centroids separation, $d$} (or the footpoint separation between the opposite polarity centroids) is calculated as
\begin{equation}
d =  R_{\sun}\gamma,
\label{eq4}
\end{equation}
where $R_{\sun}$ is the solar radius and $\gamma$ is angular separation of two opposite polarity centroids
(in radians, angle between two lines drawn from centre of the Sun to the centre of each centroid).
\item{}
\textit{Tilt, $\theta$}. ARs are usually tilted with respect to the solar parallels with leading polarities tending toward the equator. This rule, first described by \citet{Hale1919}, became later known as Joy's law. Non-zero tilt angle is supposed to come from the Coriolis vortices that twist a magnetic flux bundle rising up through the CZ.
We calculate tilt of an AR as an angle between the line connecting the centroids of opposite polarities -- the axis of an AR -- and the local parallel passing through the centroid of the leading polarity (Fig.~\ref{fig1}c). Tilt is positive when measured in the counter-clockwise direction. Under these conditions, ARs obeying Joy's law will have positive (negative) tilt of units to several tens degrees in the southern (northern) hemisphere. If one adds an additional requirement that the leading polarity field should follow the Hale polarity rule \citep{Hale1925}, this would lead to a new definition of Joy's law, in which anti-Hale ARs would exhibit tilt angles of about $\pm180\degr$ \citep[cf. fig.~1a in][]{Li.Ulrich2012}.

\item{}
Finally, to compute twist, $\alpha$, of an AR, we used SHARP vector magnetic field data acquired at $t_{max}$ and remapped to Lambert cylindrical equal area projection \citep{Bobra2014,Hoeksema2014}. With $\mathbf{j}=\nabla\times\mathbf{B}$ and $\mathbf{B}$ denoting electric current density and magnetic field vector, respectively, in the framework of force-free field, the electric current could
be expressed as a product of scalar or pseudo-tensor quantity $\alpha$ and magnetic induction, {\bf B}:
\begin{equation}
\mathbf{j}=\alpha\cdot\mathbf{B}
\label{eq6}
\end{equation}
In the past, $\alpha$ was used as a measure of magnetic twist in an AR \citep{Seehafer1990,Pevtsov1994}. We calculated an averaged over the whole AR flux-weighted twist $\alpha_{av}$ \citep[e.g. ][]{Hagino2004}
\begin{equation}
\alpha_{av}=\frac{\sum j_{z}(x,y)B_{z}(x,y)}{\sum B^2_{z}(x,y)}.
\label{eq7}
\end{equation}
The summation in equation \eqref{eq7} was performed only over pixels with magnetic field strength exceeding 300 Mx~cm\textsuperscript{-2} \citep[cf. ][]{Liu2014b}.
Following \cite{Abramenko1996}, we calculated electric current density as
\begin{equation}
j\textsubscript{z}=\oint_L\mathbfit{B}\textsubscript{t}\textrm{d}\mathbfit{r},
\label{eq8}
\end{equation}
where $\mathbfit{B}\textsubscript{t}$ is the horizontal magnetic field vector (relative to
solar surface) and $L$ is a contour that encloses an area of $5\times5$ pixels around the central point where the z-part of the electric current density $j\textsubscript{z}$ was determined.
\end{enumerate}

\section{Results and discussion}

In total, we detected more than 600 ARs emerged at the visible solar disk between 2010 May and 2017 December 31. From this initial dataset we identified 423 ARs, which satisfy the following criteria: i) both the AR's emergence onset and magnetic flux peak must be observed within 60\degr\ from the central meridian; ii) SHARP data on the AR vector magnetic field must be available at the time $t_{max}$ of the peak magnetic flux; iii) the times of the emergence onset and of peak magnetic flux can be clearly identified. In this final sample, the maximum total unsigned flux of ARs varies in the range 0.36--25.3$\times$10\textsuperscript{21}~Mx. All calculated parameters of ARs as well as its HARP numbers are listed in a table provided as a supplementary material.

\begin{figure*}
	\includegraphics[width=\linewidth]{figure2.eps}
	\caption{Relations between peak total unsigned magnetic flux $\Phi_{max}$ and averaged flux emergence rate, $R_{av}$, (a), maximum flux emergence rate, $R_{max}$, (b), opposite polarities separation, $d$ (c), ratio $R_{max}/R_{av}$ (d), tilt, $\theta$, (e), and averaged twist, $\alpha_{av}$, (f) for the entire sample of 423 ARs. Black solid lines in panels a, b, c displays the best linear fittings to the data. ARs located in the northern (southern) hemisphere are drawn in blue (red) color in panel $e$. Note that tilts for ARs located in the northern hemisphere are plotted with inverted sign in panel e. To better visualize the results, 16 outliers in panel e are excluded in the plot.}
\label{fig2}
\end{figure*}

\subsection{Dependence on maximum unsigned flux}
\label{sec_all_vs_phimax}

Fig.~\ref{fig2} shows correlation between peak total unsigned magnetic flux and other parameters. The average emergence rates as well as the polarity separation are strongly correlate with $\Phi_{max}$. Rank correlation coefficients and the probability of chance correlation are: R$_{av}$ -- 0.72 (10$^{-32}$)
and $\rm d$ -- 0.86 (10$^{-32}$). As these two parameters are not independent of each other, strong correlation between $\Phi_{max}$ and R$_{av}$ is most likely the result of correlation between $\Phi_{max}$ and polarity separation ($\rm d$). Indeed, the R$_{av}$ residuals (not shown) after subtracting a fitted dependence between $\Phi_{max}$ and $\rm d$ (Fig.~\ref{fig2}c) do not show any correlation with $\Phi_{max}$.

Fig.~\ref{fig2}a shows a scatter plot of $R_{av}$ versus $\Phi_{max}$ in a double logarithmic scale. The best linear fitting to the distribution (black line) yields a power-law

\begin{equation}
R_{av}=0.43\Phi_{max}^{0.48\pm 0.02},
\label{eq10}
\end{equation}
where $\Phi_{max}$ is in units of 10\textsuperscript{21} Mx and $R_{av}$ is in 10\textsuperscript{20} Mx~h\textsuperscript{-1}. The power-law index is close to the theoretical value $\kappa=0.5$ obtained by \cite{Otsuji2011}. Recall that \cite{Otsuji2011} evaluated their power law index in the frame of an oversimplified emergence model assuming nearly constant magnetic flux within the tube (irrespective of the total magnetic flux or spatial size of the magnetic tube) and a constant rise velocity of the tube.

The opposite polarity centroids separation, $d$, versus $\Phi_{max}$ scatter plot is shown in Fig.~\ref{fig2}b. The best linear fitting to this scatter plot results in the following relation:
\begin{equation}
d=C\Phi_{max}^{\kappa_{1}}\propto\Phi_{max}^{0.36 \pm 0.01}.
\label{eq12}
\end{equation}
\cite{Otsuji2011} inferred that the analytical power-law index $\kappa_{1}$ in \eqref{eq12} $\kappa_{1}=2(\gamma-1)/(5\gamma-4)$, where $\gamma$ is the adiabatic index. With $\gamma=5/3$ for ideal gas and $\gamma\sim4/3$ for the near solar surface layers, $\kappa_{1}$ in \eqref{eq12} equals 0.30 and 0.25, respectively. By fitting their $d$ versus $\Phi_{max}$ scatter plot, \cite{Otsuji2011} derived the power-law index $\kappa_{1}=0.27$. Our power-law index $\kappa_{1}=0.36 \pm 0.01$ exceeds the value reported by \cite{Otsuji2011}. We suppose that this discrepancy can be explained by a different measurements criterion: \cite{Otsuji2011} defined $d=d_{max}$ as the \textit{maximum observed separation} while we consider $d$ as a distance between the opposite polarity centroids observed during the \textit{maximum observed total unsigned magnetic flux} of an AR. It was confirmed that a lag is observed between peak flux and peak separation distance in emerged magnetic bipoles, with latter trailing \citep{vanDrielGesztelyi2015,Kosovichev2008,WallaceHartshorn2012}. Of course, the mentioned discrepancy can be, at least in part, a result of specific details of AR parameter measurements in this work and in the analysis by \cite{Otsuji2011}.

Fig.~\ref{fig2}c shows the relation between tilts, $\theta$ and peak fluxes, $\Phi_{max}$. To better visualize the relation, we plotted $\theta$ with inverted sign for ARs located in the northern hemisphere (blue dots), i.e. in Fig.~\ref{fig2}c ARs obeying Joy's law have positive tilt regardless of the hemisphere where they are located. One can see that strong ARs, in general, obey Joy's law and have tilt of about ten degrees while weaker ARs exhibit scatter of tilt in a wide range of angles. The similar results were obtained by \citet{Illarionov2015} who analysed distribution of tilt angles for large and small magnetic dipoles \citep[see fig.~1 in][]{Illarionov2015}. Although tilt of an AR varies during the emergence phase \citep[e.g. ][]{vanDrielGesztelyi2015}, we can conclude that by the time of reaching its peak flux an AR has tilt expected by Joy's law.

Averaged twist of an AR, $\alpha_{av}$ versus $\Phi_{max}$ is shown in Fig.~\ref{fig2}d. There is no evident correlation between these two parameters. Nevertheless, weak ARs seem to exhibit greater absolute twist compared to strong ones. A model of helicity accumulation in magnetic flux tubes developed by \citet{Choudhuri2004} predicts that ``smaller sunspots should statistically have stronger helicity (i.e., higher values of twist''. It was observationally confirmed by \citet{Liu2014b}, however their sample consisted of only 28 emerging ARs. It seems that our results and results of \citeauthor{Liu2014b} do not contradict each other.

\subsection{Flux emergence rate versus twist}

The $R_n$ versus $\alpha_{av}$ scatter plot for the entire sample of 423 ARs is shown in Fig. \ref{fig4}a. There
is no obvious correlation, however, it seems that ARs emerging with low normalized rate tend to exhibit lower
value of twist. This tendency is confirmed by the best linear fitting of the $R_n$ versus $\alpha_{av}$ relation
(black solid line in Fig. \ref{fig4}a).

The relation between $R_n$ versus $\alpha_{av}$ shown in Fig.~\ref{fig4}a might be contaminated by influence of
noise in the calculated twist. Indeed, the current density in weak field areas is dominated by noise due to
uncertainties in the azimuth disambiguation procedures \citep{Hoeksema2014}. Although the thresholding keeps only
strong field pixel during the calculation of $\alpha_{av}$ by equation \eqref{eq7}, this noise can still dominate
at the borders of well-determined AR structures due to finite length of the integration contour in \eqref{eq8}.
Consequently, the noise contribution to the twist value might be significant for weak small ARs.

Therefore, we further reduce our sample to 110 strong ARs with peak magnetic flux exceeding $5 \times 10^{21}$ Mx.
In such a case, the tendency shown in Fig. \ref{fig4}a is more pronounced in the $R_n$ versus $\alpha_{av}$
plot for strong ARs in Fig. \ref{fig4}b. Although there is no obvious direct relation between the normalized flux
emergence rate and twist, the majority of the data points lie above the dashed line in Fig. \ref{fig4}b
suggesting that ARs exhibiting high twist emerge at higher flux emergence rate. This suggestion is in a general
agreement with the theoretical predictions
\citep[e.g.][]{Moreno-Insertis1996,Emonet1998,Magara2001,Murray2006,Toriumi2011}.

\begin{figure}
	\includegraphics[width=\linewidth]{figure3.eps}
	\caption{Relation between the normalized flux emergence rate and twist for the entire sample of ARs (a) and for strong ARs with $\Phi_{max} > 5 \times 10^{21}$~Mx (b). Black solid line in panel a displays the best linear fitting to the distribution. The dashed line in panel (b) is drawn to show that the majority of data points lie above this line. The same dashed line is overplotted in panel (a) to emphasize that the majority of points from the whole ARs sample lie above this line as well.}
\label{fig4}
\end{figure}

\section{Conclusions}

We used the measurements of the SDO/HMI magnetic field taken over 8 years to reveal possible relations between
different parameters of emerging ARs. In total, our sample consisted of 423 ARs emerging and growing to its peak
magnetic flux within 60\degr from the central meridian.

We confirmed the results of previous studies concerning the power-law relation between the flux emergence rate and peak magnetic flux of an AR. The power-law indices derived in previous works were scattered in the broad range from 0.36 in \citet{Norton2017} to 0.57 in \citet{Otsuji2011} to 0.69 in \citet{Abramenko2017}. However, the theoretical value of 0.5 obtained by \citet{Otsuji2011} was not supported observationally. In this work, using the largest so far sample of emerging ARs, we found that the power law index $\kappa$ equals 0.48$\pm$0.02 for the averaged flux emergence rate that agrees (within uncertainties) with the theoretical value of 0.5.

The opposite polarity centroids separation also scales as a power law of the peak magnetic flux, although our power law index 0.36$\pm$0.01 is higher than that obtained in the previous works. We attribute this discrepancy to different measurement routines.

Although the tilt of emerging ARs varies during the emergence phase \citep{vanDrielGesztelyi2015}, our results suggest that by the end of the magnetic flux growth an AR exhibits the tilt angle expected by Joy's law. In accordance with previous studies, the tilt angle of weak ARs is more scattered compared to strong ARs.

The observationally obtained relation between the flux emergence rate and twist of magnetic tube shows that AR's twist sets a lower limit for the flux emergence rate. Our results suggest that more twisted magnetic tubes will emerge at higher flux emergence rate while less twisted ARs might exhibit either high or low flux emergence rate. Seemingly, there exist additional mechanisms that causes ARs of the same twist and magnetic flux to emerge with different rates.
We can suppose that those mechanisms could be attributed to the interaction between plasma convective motions and rising magnetic flux bundles. As a simple qualitative model, turbulent motions of high-density plasma inside the convection zone could fragment emerging flux bundle into several magnetic flux tubes \citep[see fig.~1 in][]{Zwaan1985}. Each tube reaches the solar surface and emerge at a different time with some delay \citep[see 'Conclusions and Discussion' section and figs.~7,8 in][]{Abramenko2017}. As a result, the duration of the whole emergence process increases leading to decrease of the averaged flux emergence rate. As another option, since the rising velocity of emerging magnetic flux is determined by the plasma upflows in convective cells \citep{Chen2017}, the emergence rate could be randomly affected by the lifting velocities of the plasma portions that carry the magnetic flux to the surface.

\section*{Acknowledgements}
The authors appreciate the referee's comments on improving this paper. SDO is a mission for NASA's Living With a Star (LWS) programme. The SDO/HMI data were provided by the Joint Science Operation Center (JSOC). The study was supported by Russian Science Foundation (Project 18-12-00131).

redpajama_set_name: RedPajamaArXiv


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Created by dmcgarry on 13 October, 2010.
EDXLSharp is a C# / .NET 3.5 implementation of the OASIS Emergency Data Exchange Language (EDXL) family of standards. This set of libraries can be used to generate, read, and validate CAP, DE, HAVE, RM, SitRep, and TEP messages. Licensed under the Apache 2.0 License. EDXLSharp is Free and Open Source Software (F/OSS). EDXL Sharp is part of a collaborative research project of The MITRE Corporation. The MITRE Corporation is a not-for-profit organization chartered to work in the public interest. As a national resource, we apply our expertise in systems engineering, information technology, operational concepts, and enterprise modernization to address our sponsors' critical needs. (http://www.mitre.org).


text:
Auction Tips
Auction Trends
Cartographic Miscellany
Cartographic Myths
Map Basics
Mapmaking
OWA News
Hidden Treasures & Collector's Corner
Hidden Treasures by Jon Dotson
One of the most frequent questions that we receive from people not familiar with our line of business is "do you sell treasure maps?" While we have yet to encounter a true treasure map where "X" marks the spot, we do occasionally uncover mysterious gems while cataloging. Tucked away in the pages of antique books, atlases, and folding maps are artifacts left behind by previous owners. These extras can provide additional context to an item's intended purpose or simply offer the lucky finder a fun bonus. Over the last year we have been collecting these "treasures" and wanted to share a small sampling with you.
Pressed for Time - Pressed Plants/Flowers
One of the more common items that we find in antique books is pressed plants and flowers. Collecting plants was a popular pastime in the mid to late 19th century, where flowers were a key design element. During this Victorian era, both men and women pressed leaves and flowers in books for a variety of reasons including household decorations, personal journals, and botanical scrapbooks. While a serious collector would likely use a field press to preserve specimens, an amateur hobbyist would typically press them between pages in a book. A few examples we have discovered include:
A set of maple leaves in Johnson's New Illustrated Family Atlas, circa 1861
Flowers in a Brookes' General Gazetteer published in 1796 and in Colton's General Atlas published in 1868.
Say Cheese - Anonymous Photograph
The photograph below was adhered to the front pastedown of William Chamber's Atlas of Modern and Ancient Geography. For Use in Schools, published in 1853. It captures a school group including teachers, a few students, and a clergyman in Victorian era attire, presumably somewhere in Britain given that Edinburgh is the publication city. The photograph is a bit of a mystery to us as there are no additional notations in the endpapers about it or a previous owner's signature. The only manuscript found in the atlas is on a blank page opposing the map of England & Wales listing various place names in what appears to be a student's hand. This is the first photograph that Eliane or I have encountered being pasted into an antique book.
A Picture Is Worth a Thousand Words - Splatter Art & Poem
This "splatter" art was discovered in a copy of David Burr's A New Universal Atlas, published circa 1835. The word "Hope" is revealed at center and is surrounded by ferns, with a small dove perched above the letter "p."
The verso contains a poem that is rather difficult to decipher, but the first few lines reveal the author is clearly new to verse and forces some rhymes:
"I wish to give you a little lecture and I hope it will do you good-er
but as I am a new hand at that kind of business-er
I hope you will be chorible-er [charitable?]
as much as it is possible for humone netter [human nature?].
Now gole-keeper don't you be winking at that girl-er
or I shall be entirely discouraged-er
and give up-er."
The illustration/poem was composed on ruled paper with a thin blue line, and I initially assumed that this was a 20th century addition. To my surprise, however, ruled paper started appearing on the marked in the early 19th century, so its insertion date is "unclear-er."
Another beautiful example of splatter art was recently discovered on the verso of a map of the eastern United States that was originally issued in Charles Smith's General Atlas. A variety of ferns were laid on the verso and paint was applied to the sheet, leaving a detailed outline. Somehow the map on recto was unaffected by this lovely illustration.
The Better Half - Half a Song Sheet
This torn sheet likely became a bookmark in an example of D.W. Beadle's The American Lawyer, and Business-Man's Form Book for 1852. The obscure song is entitled "International Ode. Our Fathers' Land" and is based upon the tune to "God Save the Queen" (as well as "America"). It was written by the famous physician and writer, Oliver Holmes Sr.
The first verse, which would have been present on the full sheet, reads:
God bless our Fathers' Land!
Keep her in heart and hand
One with our own!
From all her foes defend,
Be her brave People's Friend,
On all her realms descend,
Protect her Throne!
Before the Border Patrol - News Clipping, Indian Encounter
This fascinating article was first issued in the San Francisco Call on August 2, 1881 and was picked up here by another unidentified newspaper. The account describes an encounter between an American party, consisting of a gold prospector and a surveying crew for the Mexican Central Railway (incorporated in Massachusetts in 1880), and a band of Apache Indians approximately 30 miles south of El Paso. The Apaches attacked the Americans, killing the entire 13-person surveying crew and stealing their supplies. The lone prospector, Ambroise Somprax of Natchitoches (LA), was spared as they believed he had hostage value. Somprax eventually escaped to California where he recounted his story to a reporter. The article ends with Somprax stating that he was headed to Washington "to see what can be done to teach them a lesson."
This clipping was found with the two southern sheets of a large western map entitled Map of the Territory of the United States, West of the Mississippi River that was published two years prior to the article (1879) by the U.S. Army. The map would certainly be useful in avoiding this hostile area of Chihuahua!
These little extras are not only entertaining in themselves, but help an object come to life. Personalization is timeless and can make a 200-year old artifact seem like it was handled just yesterday. So keep your eye out for hidden treasure, and please let us know if you find anything of interest. We will continue to collect samples over the coming months and hope to have a new entry in this series next year.
Collector's Corner by Eliane Dotson
The "Collector's Corner" is a new, recurring segment that will highlight one collector's journey through map collecting in their own words.
Dennis G.
"Well I always liked maps. I was a Boy Scout and I used maps for hiking and things like that, but the real thing was when I was in Hawaii on vacation and I saw a map of Washington, DC, and it was well framed (over-framed actually) with a nice Hawaiian Koa wood. It was an 1845 map of Washington, so I said, 'I need that for the office so it looks like we've been here for a while' [we had just opened up an office in Spring Valley, which was inside the District of Columbia]. So that was the first one. And then a few years later I had a little more money and was on vacation in Hawaii and bought a Hondius 1650 map of Virginia, really gaudily framed in Koa wood. That was more expensive and I wanted to know what I had purchased (this was pre-Internet) so I actually got them to send me copies of books. And then there was a third map, but I forget what that is, but that means you have "old map pox" and you have to have all the maps that were ever done of Washington, D.C. In the beginning my collecting interest focused on Washington, DC. That was broadened out to DC, Virginia and Maryland, because DC didn't exist until 1792 so if you want old maps you've got to get Maryland and Virginia. Now I'm actually trying to cut it back to just Washington DC, so it's a very complete collection at this point. My favorite map is map #1 of Washington DC that was printed in 1792 in 'The Universal Asylum and Columbia Magazine' and it was the first printed plan of the city."
If you would like to share your story, please reply to this email explaining (in 200-500 words) how you first became interested in collecting maps, how you decided on your collecting interest, and what is your favorite map and why. Hopefully we will feature your collecting journey soon!