Thinking of starting a business this 2019? The possibilities will be endless, each with a promise of profitability. However, one of the best ideas is to build an online store. In this digital age, online platforms are preferred for shopping compared to traditional stores because of the convenience that it offers. This means that the potential of an online store is huge!
Building a successful and competitive online store is not a piece of cake. With this, if you want things to be easier on your end, keep on reading the rest of this post and learn from some of the tips we will be sharing. Success is not an overnight feat, but with patience and determination, it won't take long before your online store will prosper.
This is perhaps the best thing that you should do if you want to build an online store this year. You do not need to be an expert in website design to get started. With an ecommerce platform, the creation of your online shop can be done in an instant.
One of the best examples of an ecommerce platform that holds a lot of promise is the 3dcart online store service. This makes setting up and managing an online store a breeze, even if you have zero knowledge of how things work. It is user-friendly and customizable, has no transaction fees, and comes with round-the-clock customer support for a speedy response if in case there is a problem. The latter makes sure that the customer experience will not be negatively affected.
There are some people who might think that working with a website developer is the best route to take to build an online store. Yes, this is true. However, the problem is that it can also be costly. If you want to have complete control of the store, use an ecommerce platform. As long as you make the right choice, it will make it effortless for you to manage the online presence of your store.
Like in the case of building any other business, you should also take the time to conduct thorough research. First, you should do a research on your competitors. Look for providers of the same product or service that you are offering within the area. Consider their strategies and how they are succeeding. You can use this as an inspiration when it comes to how you will proceed.
To add, you should also research your target market. This will provide you with insights on what can be done to captivate their attention. It will also be an effective way to determine the best approaches for promoting your business. Plus, this will be an opportunity to identify the best pricing strategy that will work.
As a part of your research, you should also be invested in looking for the right products and services to offer. It is not enough that you have the right idea. You also need to have the right market for your idea to be profitable. For this reason, a feasibility study is warranted to minimize the likelihood that your entry into the world of ecommerce will be a success story.
This may seem like a simple thing, but this is actually highly-influential of the success of your online store. The domain name can make or break your online business. This will be the name of your website and will be a critical element of the personality of your store's brand.
When choosing a domain name, one of the best practices is to keep it simple, making it easy to remember. Get rid of unusual names or those that are too long to remember. To add, it should also be unique, which will distinguish you from your competitors. You should also use keywords to rank well in search engine sites.
For most online shops, the name of the business is also the domain name of their shop.
Another must-have when building an online store is the right mode of payment. Most shops will offer wire transfers, credit card payments, and even PayPal. Some are radical enough to accept Bitcoin, but we won't suggest that you don't go that route yet as it can be complicated, especially if you lack knowledge about cryptocurrencies.
When setting up the payment methods, one of the most important is to make sure that it has high-level security features, especially in terms of protecting the information shared by the customers. It must also be easy to use since this will have an impact on the overall experience of the customer.
Visuals are important for the success of your ecommerce site. From the color to the font to the layout, it must be well-presented. Otherwise, the bounce rate will be inevitably high. With this, one of the most important is to post pictures of the products or services that you are selling, which will help to lure your customers.
The pictures should also be accompanied by descriptions. They will provide relevant information about what is being offered by your store, such as product size, ingredients, benefits, and the price, among others. This way, the online store will be as informative as possible.
There are many factors that will influence the success of the online store that you are building, but one of the most important is perhaps marketing. You need to come up with a robust marketing strategy, making it possible to stand out from the competition.
Fortunately, in this digital age, marketing does not need to cost an arm and a leg. Even small businesses can effectively market their products and services even when on a budget. Among others, digital platforms, such as social media, will be effective. The key here is to create engaging and relevant content that will capture the attention of your target market.
In line with your marketing strategy, you need to establish your brand. This will make it easy for your store to be recognized and hence, will have a huge impact on the profitability of your online store.
From the logo to the design of your website, there are certain elements that will be critical for your branding. It should immediately remind customers of your business. With this, it is also necessary to be consistent with your marketing materials for the brand to be easier to recognize.
If you are using an online platform for your business venture, you should be familiar with search engine optimization. In a nutshell, this refers to a practice of optimizing a website through different techniques with the intention of appearing on the top of search results. This is under the premise that the higher you are on the results page, the likelier it is that the users will click on your store.
There are many ways by which it is possible to optimize your online store, such as through the use of keywords that are often used by your target market when they are conducting an online search. Each product should come with an appropriate description with keywords in mind. The photos should also come with relevant tags to increase the likelihood that they will show up.
Even if there is no physical space to conduct business, this does not mean that you are spared from the requirements of business registration. The process will differ depending on where you are from. Regardless, you need to take care of the paperwork for the business to be legitimate. When done, you will have the licenses and permits needed to operate. This is also necessary to ensure that your tax obligations will be fulfilled.
It can be frustrating for customers to have problems when visiting the store, such as payments not pushing through. With this, to build a successful online store, you need to offer exceptional customer support that should be available round-the-clock. See to it that there are multiple ways to reach your representatives, such as through phone, chat, or email. Some stores even employ a chatbot to have someone immediately available to handle queries.
At the end of the day, the most important thing to remember is that you should not stop improving. The success of your online store should be a continuous endeavor. You should use different tools for analytics, making it easy to determine what else can be done to improve.
Through an analysis of the performance of the business, it will be easy to overtake the competition and deliver the highest level of satisfaction. From your marketing strategies to the products and services that are being offered, monitoring is crucial to identify potential areas for improvement. Technological tools and thorough research, among others, will be vital for monitoring your online store.
In sum, while a lot of people are building their online stores, success is a feat that is not enjoyed by everyone. To be one of those that triumphs in a competitive market, take note of the tips that have been mentioned above.
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I am in need of help to design/build a usb controller that will turn on/off 9 individual LEDs seperatly. The application that is to send commands to the controler is Visual Basic.
I am looking for low cost/ small in size/ good availability of parts needed.
I need schematics, source code ext. or am willing to pay for it to be fabricated.
There are any number of off the shelf solutions to what you desire to do.


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The Threat of Cyber Security
Jessica Lambert
Vehicle connectivity, while new and exciting, also comes with great threats as society makes its shift toward the future of autonomous cars. That being said, vehicle manufacturers will always do their best to deliver good, reliable products that customers can depend upon.
"What is the Threat to Cyber Security?"
In short, the most heinous threat we face with cybersecurity is the manipulation of the vehicle function or the retrieval of driver information through vulnerable areas in the system.
Access can be achieved through a vehicle's wireless communication system, such as mobile phones and tablets connected to the car via Bluetooth, USB, and WIFI. Vehicle hacking can even occur through a third party device plugged into the vehicle diagnostic port.
Because of these threats, the automotive industry will need to work quickly to create ways to defend and protect drivers and passengers alike.
The Biggest Challenge
Perhaps one of the biggest challenges that we face when it comes to cybersecurity in our vehicles is that the electrical components in our vehicles, (also known as electrical control units or ECUs), are all connected together in a massive internal network.
There are more than One Hundred Million lines of code in the cars of today. The more code, the greater the chance that a hacker will be able to infiltrate the system and create a lot of havoc in anything from the brakes, to the engine. Many countries are beginning to realize how big of a threat hacking really is when it comes to cybersecurity.
In 2015, two researchers looking into the threat of cyber security proved that they could take control of a Jeep Cherokee and send it off the road. In the same year, hackers uncovered a vulnerability in the BMW ConnectedDrive technology, (which is a system designed to bring ease of access and comfort), and exploited the weakness to prove they could take control of the vehicle. In 2016, there was yet another threat uncovered where hackers proved they could unlock Volkswagens remotely.
This is obviously not the kind of thing anyone wants to hear. But that's also why the automotive industry is doing its absolute best to fix holes and vulnerable areas in vehicle systems, especially as the demand for connected cars increases.
Cyber Security and the Automotive Industry
Cyber security, in a lot of ways, is changing the automotive industry from the inside out. Engineers are learning to combine human learning and artificial intelligence in the best way possible.
The Automotive industry realizes that they can't just put a firewall on a car and call it "safe". They realize that they have to take an offensive-defensive stance to the issue of cyber security. If they don't seek to understand the human brains behind the hacking, they can't learn how to defend against them.
It's a Two-Way Street
While the automotive industry and the brains behind autonomous vehicles will do their best to keep Cyber Security a priority, it takes cooperation from drivers, too.
This is especially true as the threat grows. The more vehicles that shift over and become autonomous, the more vehicles exist on the roadways that can be infiltrated. Thus the threat of danger will grow as the amount of autonomous vehicles grow. In the year 2014, a little over half of the vehicles sold were connected. This means that there are a good many cars on the road today that are vulnerable to attack.
In the coming years, we can expect this number to double or even triple. Because of this, the automotive industry will have to expand their knowledge and create ways to defend their new technology and keep it in the right hands. But again, this takes cooperation from the driver as well as the industry itself. If we're careful and take the proper precaution, we won't have to worry about vehicle hacking or manipulation.
The Government and Cyber Security
You may not be aware, but the government has actually played a major role in the threat to cyber security. The reason for this is because of the risk it poses to public safety. US Senators Blumenthal and Markey actually proposed legislation to establish mandatory federal standards for cyber security in automotive vehicles.
In fact, the US Transportation Secretary Anthony Foxx said: "Cyber Security is a safety issue and a top priority at the department. Our intention with today's guidance is to provide the best practices to help protect against breaches and other security features that put motor vehicle safety at risk."
However, this isn't the case for some of the other people in Washington. Senator Gary Peters has actually repeatedly argued that he believes that US lawmakers should take a step back and allow the private industry to take a stand in deciding for themselves what solutions and standards ought to be made to protect the general public from the looming threat to cyber security.
Fighting the Threat to Cyber Security
There are a lot of steps that the automotive industry plans on taking to minimize the threat that exists to Cyber Security.
One of these things is a defensive software solution stored on each ECU individually. They will be able to analyze threats and fight against them before they ever get into the internal world of the vehicle.
Since people are much more often reactive than proactive, there aren't very many ideas or software that will protect a vehicle from threats of Cyber Security. We hope that as society shifts toward the future of autonomous cars, the threat to cyber security will be be explored and dealt with accordingly.
While it's easy to enjoy the luxury that comes with connected cars, we should always stay aware of the threat that this poses and be aware of just how much we don't know about cyber security and focus on keeping our personal information where it belongs.
If you're scared of the threat, consider purchasing a used car that isn't connected, or exploring the issue for yourself. Either way, we can rest in the knowledge that as the automotive industry drives toward the future of connected vehicles, it will also advance technologically toward a better future for cyber security.
Whitepaper: How 5G will dramatically strengthen autonomous driving systems
Using AUTOSAR C++ coding guidelines to streamline ISO 26262 compliance
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Auto IQ News: Volvo's self-driving truck, Nuro delivers Domino's, and an electri...
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Location spotlight: Israel
List of carmaker R&D centers in Israel
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FCA and Renault merger: self-driving tech and emobility strategies could get boo...
Auto IQ News: Mercedes safety, Ford robots, Cruise autonomy and more

redpajama_set_name: RedPajamaCommonCrawl


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Why tuning into "The Last Drive-In" with Joe Bob Briggs on Shudder tomorrow matters
If someone were to ask me what was the best part about being a horror fan when I was a kid in the 90s, what was the thing I enjoyed most, that I could look forward to, it was always discovering new or unheard of gems that hadn't planted dynamite at the base of my brain and blown it to smithereens yet. And my favorite way to do that was to tune into the various horror hosts that populated late night TV on the weekends, in particular, Joe Bob Briggs on TNT with his show, Monstervision…
…Beginning in 1996, Monstervision and host Joe Bob Briggs gave me a reason to shut off the lights, grab some pizza and a shit ton of soda, and let dive into a world of monsters and ghouls, body counts and B-movie "terror". Some of my best memories of childhood are those late nights expanding the library of horror in my mind, engaged in Joe Bob's sometimes funny, sometimes interesting remarks and interviews with special guests as he interrupted whatever was playing that week during the commercial break with his particular flavor of commentary. That's why I'm delighted that, tomorrow, on July 13, 2018, Shudder is bringing back Monstervision with Joe Bob Briggs for a LIVE 24hr horror marathon entitled The Last Drive-In beginning at 9pm ET. It's a momentous occasion for fans, new and old, one that will feature 13 horror films and include special guests, giveaways, and perhaps most incredibly, fan discussion, allowing us all to react and interact together during what might as well be a national horror marathon sleepover. It is, without a doubt, one of the coolest horror events I have ever had the extreme pleasure to witness, but it's also one of dire importance.
See, this isn't just a horror marathon that we all get to tune into, enjoy, and then move on from and forget about. To me, this is an opportunity to re-establish something which has been missing from the horror genre for the past couple of decades…the horror host. For those of you that didn't grow up with Monstervision, Elvira, or even Svengoolie, who is still chugging along, God bless him, there was something special about those nights that is difficult to put into words. It's hard to describe the feeling of excitement and wonder as you waited to discover which blood-curdling horrors would be shown that night, and nine times out of ten, it was something you hadn't experienced before. These days, we don't get that. If you want to find something new, you have to go hop on streaming services and spend an exuberant amount of time scrolling through uninteresting catalogues of films like some mindless couch zombie with a blank look in your eyes and a little drool hanging off your lip. But imagine if you had a show that you could tune into where the host not only did the work for you in helping you unearth something fun to watch, but they were actually entertaining? (A foreign concept, I know).
The horror host means something to the horror genre. They have the ability to bring us back to that time in our childhood when the genre was still something forbidden and electrifying. Who doesn't miss lying to or hiding from their parents the fact that they were up all night watching buckets of blood be splashed across the screen in the name of our love for horror?
Already, The Last Drive-In has filled me with that same kind of nostalgic anticipation. At this point, we only know three of the films being shown during the marathon: Tourist Trap, Basket Case, and Sleepaway Camp (all of them gratuitous classics, by the way). Other than that, we know by the shirts being sold by Fright Rags that the marathon will contain 146 dead bodies, 37 undead bodies, and 131 gallons of blood. Who knows what else will show up during the marathon, or what sort of insights Joe Bob may give us on these films. Who knows which guests will appear to talk about their time during or after the making of these films. What I do know is I'm all in, and I'm ready for a day of reliving everything that makes being a horror fan so much fun.
We, as horror fans, have a chance to prove to the world that this sort of event means something. If Shudder doesn't receive the type of ratings they need for The Last Drive-In to be a success, then we can't expect anything like it will ever happen again. It isn't even that difficult to tune in, as Shudder offers a free 7-day trial, so grab the trial, tune in, and dump it after if that's your prerogative, there's no commitment. But I'm making this plea to all of us fans, not just for Joe Bob Briggs and Monstervision, but for that sense of discovery that is so hard for horror fans to recapture…save the horror host. Tune in tomorrow night and celebrate Friday the 13th the best way you can, by spending it with classic horror films, an enormous community that loves and supports each other and the genre, all the beer or soda or candy or whatever the hell you want, and the man who became a legend for his knowledge of the genre, Mr. Joe Bob Briggs.
For more details check out the trailer and the post below, and make sure to follow Shudder to join in on the live discussion!


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Philly may put traffic light back on Boulevard at site of fatal accident
Memorials mark the area of Roosevelt Boulevard near 2nd Street where Samara Banks and three children were killed as they attempted to cross the 12-lane roadway. (Emma Lee/for NewsWorks)
After last week's accident that killed a mother and three kids trying to cross Roosevelt Boulevard, the Philadelphia Streets Department is considering reinstalling a traffic signal at that spot.
If put back in, the signal would halt traffic in the middle of the block.
Samara Banks and three of her children were struck and killed by a car that allegedly was drag racing on the Roosevelt Boulevard near Second Street.
Acting Streets Commissioner David Perri says his department is going to study that location to see if a light needs to be put back in.
"Until the mid 1970s Second Street actually crossed the Boulevard, in the mid-1970s the intersection was eliminated but the signalized pedestrian crossing remained. The signalized pedestrian crossing however was eliminated in 1983 because of lack of use and because the equipment was vandalized," said Perri.
Perri says the study will take a few months.
"We'll look at things such as proximity to schools, destinations for pedestrians. We believe there is a higher use now of SEPTA in the area so it could very well warrant a signalization of a pedestrian crossing at Second Street."
Perri says the signal could be installed by next Spring.
Dozen's stood in protest outside Thursday's FDR Park redevelopment meeting in South Philly after being denied entry. A virtual meeting is scheduled for March 1.
South Philly group discusses renaming 'stop and frisk,' adding community-oriented policing
In one South Philly neighborhood, community leaders and law enforcement are discussing creating a procedure that supports officers stopping young people and sharing resources.
A massive electric vehicle test track sits amid hundreds of vehicles on display. It's a big upgrade from the dark corner where it was at last year's show.


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5 songs you must hear this week: 13 January 2020
Alan Cross Corus Radio
Out of the hundreds of song submissions that came in last week, here are the five I think are most ear-worthy. Thoughts? Let me know.
1. Tame Impala, Lost in Yesterday
The Slow Rush (Interscope)
Recommended If You Like: Nostalgic sounds, Bonnaroo headliners
Amidst news that Tame Impala (aka Fremantle, Australia's Kevin Parker) will be a headliner at Bonnaroo comes this another new loopy, disco-y single from an album will be out February 14. In case you missed the other three singles, they are Posthumous Forgiveness, It Might Be Time, and Borderline.
2. Taylor Hawkins and the Coattail Riders, Middle Child
Get the Money (Shanabelle/RCA Records)
RIYL: Foo Figthers, obviously…
The Foos other drummer is back with another single from the most honestly-named band in the history of rock. If you love the concept of early 80s MTV, you'll find much to love with the video. Boss Dave Grohl is also on this track.
3. Michael Stipe, Drive to the Ocean
Single (Audiam)
RIYL: REM, obviously…
After not being very active musically since REM called it a day, Michael Stipe has released two singles in the last four months. Back on October, he issued Your Capricious Soul. Now, just in time for his 60th birthday, he has this climate change song. Proceeds will go to Pathway to Paris, a nonprofit organization that's pushing for the Paris Accord. Stipe directed the video himself.
4. F-ed Up, In View
Single (Independent)
RIYL: Hip Covers
Back in October, F-ed Up released one of their trademark limited-edition 7-inch singles—in this case, just 200 copies were pressed up. The B-side to Fading Eyes was a bit of a surprise: a cover of the Hip song, In View. It's taken a while, but that recording has ended up online for everyone to hear. (BTW, Gord was a fan of F-ed Up and even guested as a singer on a 2014 track called The Art of Patrons).
Goody Grace feat. Blink-182, Scumbag
Single (Atlantic)
RIYL: Small town success stories
Goody Grace grew up in Selkirk, Manitoba, a small city just north of Winnipeg and about 20 kilometres from where I lived for the first 21 years of my life. How does a guy from this place on the Canadian prairies end up getting Blink-182 to perform on one of his song? Hard word. He's worked or collaborated with a number of people over the last five years from his new home in LA. He's got enough of a rep that (a) he got a major label deal with Atlantic and (b) people now return his calls.
© 2020 Corus Radio, a division of Corus Entertainment Inc.


For a while there, it looked like corporate IT resource planning was going to be easy. Organizations would move practically everything to the cloud, lean on their cloud service suppliers to maintain performance, cut back on operating expenses for local computing, and reduce—or at least stabilize—overall cost.
Unfortunately, that prediction didn't reckon with the Internet of Things (IoT), which, in terms of both size and importance, is exploding.
It varies. To a telecom, the edge could be a cell phone, or a cell tower. To a manufacturer, it could be a machine on a shop floor. To a hospital, it could be a pacemaker. What's important is that edge computing allows data to be analyzed in near real time, allowing actions to take place at a speed that would be impossible in a cloud-based environment.
Meanwhile, the need for massive data processing and analytics continues to grow, creating a kind of digital arms race between data creation and the ability to store and analyze it. In the life sciences, for instance, it's estimated that only 5% of the data ever created has been analyzed.
At Condusiv, we've seen users of our I/O reduction software solutions increase the capability of their storage and servers, including SQL servers, by 30% to 50% or more. In some cases, we've seen results as high as 10X initial performance—without the need to purchase a single box of new hardware.
While most users are familiar with the main Diskeeper®/V-locity®/SSDkeeper™ Dashboard view which focuses on the number of I/Os eliminated and Storage I/O Time Saved, the I/O Performance Dashboard tab takes a deeper look into the performance characteristics of I/O activity. The data shown here is similar in nature to other Windows performance monitoring utilities and provides a wealth of data on I/O traffic streams.
By default, the information displayed is from the time the product was installed. You can easily filter this down to a different time frame by clicking on the "Since Installation" picklist and choosing a different time frame such as Last 24 Hours, Last 7 Days, Last 30 Days, Last 60 Days, Last 90 Days, or Last 180 Days. The data displayed will automatically be updated to reflect the time frame selected.
The first section of the display above is labeled as "I/O Performance Metrics" and you will see values that represent Average, Minimum, and Maximum values for I/Os Per Second (IOPS), throughput measured in Megabytes per Second (MB/Sec) and application I/O Latency measured in milliseconds (msecs). Diskeeper, V-locity and SSDkeeper use the Windows high performance system counters to gather this data and it is measured down to the microsecond (1/1,000,000 second).
While most people are familiar with IOPS and throughput expressed in MB/Sec, I will give a short description just to make sure.
IOPS is the number of I/Os completed in 1 second of time. This is a measurement of both read and write I/O operations. MB/Sec is a measurement that reflects the amount of data being worked on and passed through the system. Taken together they represent speed and throughput efficiency. One thing I want to point out is that the Latency value shown in the above report is not measured at the storage device, but instead is a much more accurate reflection of I/O response time at an application level. This is where the rubber meets the road. Each I/O that passes through the Windows storage driver has a start and completion time stamp. The difference between these two values measures the real-world elapsed time for how long it takes an I/O to complete and be handed back to the application for further processing. Measurements at the storage device do not account for network, host, and hypervisor congestion. Therefore, our Latency value is a much more meaningful value than typical hardware counters for I/O response time or latency. In this display, we also provide meaningful data on the percentage of I/O traffic- which are reads and which are writes. This helps to better gauge which of our technologies (IntelliMemory® or IntelliWrite®) is likely to provide the greatest benefit.
The next section of the display measures the "Total Workload" in terms of the amount of data accessed for both reads and writes as well as any data satisfied from cache.
A system which has higher workloads as compared to other systems in your environment are the ones that likely have higher I/O traffic and tend to cause more of the I/O blender effect when connected to a shared SAN storage or virtualized environment and are prime candidates for the extra I/O capacity relief that Diskeeper, V-locity and SSDkeeper provide.
Now moving into the third section of the display labeled as "Memory Usage" we see some measurements that represent the Total Memory in the system and the total amount of I/O data that has been satisfied from the IntelliMemory cache. The purpose of our patented read caching technology is twofold. Satisfy from cache the frequently repetitive read data requests and be aware of the small read operations that tend to cause excessive "noise" in the I/O stream to storage and satisfy them from the cache. So, it's not uncommon to see the "Data Satisfied from Cache" compared to the "Total Workload" to be a bit lower than other types of caching algorithms. Storage arrays tend to do quite well when handed large sequential I/O traffic but choke when small random reads and writes are part of the mix. Eliminating I/O traffic from going to storage is what it's all about. The fewer I/Os to storage, the faster and more data your applications will be able to access.
In addition, we show the average, minimum, and maximum values for free memory used by the cache. For each of these values, the corresponding Total Free Memory in Cache for the system is shown (Total Free Memory is memory used by the cache plus memory reported by the system as free). The memory values will be displayed in a yellow color font if the size of the cache is being severely restricted due to the current memory demands of other applications and preventing our product from providing maximum I/O benefit. The memory values will be displayed in red if the Total Memory is less than 3GB.
Read I/O traffic, which is potentially cacheable, can receive an additional benefit by adding more DRAM for the cache and allowing the IntelliMemory caching technology to satisfy a greater amount of that read I/O traffic at the speed of DRAM (10-15 times faster than SSD), offloading it away from the slower back-end storage. This would have the effect of further reducing average storage I/O latency and saving even more storage I/O time.
Additional Note: For machines running SQL Server or Microsoft Exchange, you will likely need to cap the amount of memory that those applications can use (if you haven't done so already), to prevent them from 'stealing' any additional memory that you add to those machines.
It should be noted the IntelliMemory read cache is dynamic and self-learning. This means you do not need to pre-allocate a fixed amount of memory to the cache or run some pre-assessment tool or discovery utility to determine what should be loaded into cache. IntelliMemory will only use memory that is otherwise, free, available, or unused memory for its cache and will always leave plenty of memory untouched (1.5GB – 4GB depending on the total system memory) and available for Windows and other applications to use. As there is a demand for memory, IntelliMemory will release memory from it's cache and give this memory back to Windows so there will not be a memory shortage. There is further intelligence with the IntelliMemory caching technology to know in real time precisely what data should be in cache at any moment in time and the relative importance of the entries already in the cache. The goal is to ensure that the data maintained in the cache results in the maximum benefit possible to reduce Read I/O traffic.
So, there you have it. I hope this deeper dive explanation provides better clarity to the benefit and internal workings of Diskeeper, V-locity and SSDkeeper as it relates to I/O performance and memory management.


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Ruins of Mars სამაგიდო თამაში
Сэкономить -169.00 ₾
Atheris GamesКод:7730707
თანხა ფასდაკლებით169.00 ₾
The year is 2179, and Earth's future seems bleak. Years of pollution have tarnished the landscape, and the world's supplies of natural resources have dwindled to abysmal levels.The use of electric vehicles, solar technologies, and other energy-saving solutions have slowed the problem, but the long-term abuse on the planet by previous generations has been hard to reverse. Most Earthlings seem to have given up hope, yet a group of optimistic explorers are trekking to Mars, which some believe may turn around their fate.
In search of knowledge, these explorers hope that understanding the demise of alien populations can assist them with preventing or at least slowing the rapid deterioration of Earth. They'll need to replicate Martian technologies, translate their languages, and avoid gaining too much radiation along the way in order to end up with the most prestige and save Earth as they know it.
In Ruins of Mars, players compete to build out their arsenal of knowledge, attempting to understand the languages of ancient civilizations that colonized Mars and made it a hub of economic activity. The game is played around a board with five locations and eleven communal action tiles that are laid out at random underneath the board as evenly as possible.
Players: 1-4
Time: 60+


Alan Tyrer's discrimination links page.
An opportunity for disabled people and other vulnerable groups.
European Parliament gives a YES vote to Non-Discrimination in Europe.
A paper written by Hermann Christmann for the International Stuttering Awareness Day.
A paper written by Hermann Christmann for a World Congress of Fluency Disorders in Denmark 2000.
A survey made by ELSA on telephone discounts in different European countries.


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Search in titles only Search in Recreation Room only
DNA Results from Asturias
Previous 1 2 3 4 5 6 template Next
Originally posted by T E Peterman View Post
So you are S5520+?
If the 36 SNPs really happened at an average of 136 years, this would suggest that the S5520 mutation happened 4,896 years ago. Z156 would have happened 5,032 years ago. Z381 would have happened 5,168 years ago. U106 would have happened 5,304 years ago.
Let's say the mutation rate is really once every 125 years. This would make U106 4,875 years old, or 2875 BC, which is plausible. This would make P311 5,000 years old even.
Have you conferred yet with the administrator of the U106 project? What are his thoughts about the matter? If I have different SNPs to someone else in the same subclade, what do you want me to do? Pretend that they never happened.
Timothy Peterman
Those SNP rates are Dr Ian McDonald's, not mine. P311 does not have to be 5000 years old.
Last edited by 1798; 17 October 2014, 11:32 AM.
MMaddi
yDNA: R-CTS2509; mtDNA: T2e
As I posted previously here in regard to Dr. McDonald, who's quoted quite liberally by 1798 regarding aging estimates, Dr. McDonald recently posted in the R1b-U106 Yahoogroup that he agrees that there's no evidence that R1b was in Europe before the late Neolithic. He agrees with what most genetic genealogists who've studied the issue and population geneticists like Dr. Hammer believe, not what 1798 believes.
This is counter to the basic viewpoint that 1798 has about R1b in Europe. You would think that, if 1798 was interested in having a reasoned debate on this subject, he would not pick and choose what statements Dr. McDonald has made on the subject. I would understand if 1798 would report McDonald's statements on both subclade aging and the presence of R1b in Europe and tell us that McDonald is right on the former and wrong on the latter.
But ignoring Dr. McDonald's disagreement with 1798's basic premise of a Mesolithic presence in Europe is just plain intellectual dishonesty. This is why it's useless to argue with him, since he picks and chooses his "evidence," ignoring views and data which don't support his view. It suits his argument to cite Dr. McDonald on the subclade aging issue, so he quotes that. It undermines his argument to quote Dr. McDonald on the issue of when R1b was in Europe, so you'll never see him quote McDonald on that.
R-DF49
Originally posted by MMaddi View Post
Let me answer your objection, on behalf of 1798: "Heresy! It's as simple as that. Just multiply an average and I get what I want."
Indeed this is one of the problems, but there is also the matter of how the SNPs were counted. In order to do this properly you have to take care to eliminate ALL positions reported in the variance files that aren't downstream of the point you are looking at, S5520 in this case.
That's quite a job in itself and requires analysing a large no. of variance files from various L11 subclades.
Then you need to examine the bed files to make sure the other people were actually covered for each position you are looking at
When counting SNPs it's also advisable to watch out for mutations that are very close to each other, these could be single events.
Plus I wouldn't put it past 1798 to have included indels in his count, most of which are STRs.
Last edited by Subwoofer; 17 October 2014, 02:30 PM.
Originally posted by Subwoofer View Post
I have looked at the Big-Y files in the U106 at yahoo group forum. Four testers under Z156>S5520 have 27 of the same SNPs and the rest are singletons. The men who are already tested are within a GD of 10 at 111 markers of each other and I am a GD of 39 from this group at 111 markers. Perhaps Maddi thinks that I have been studying dna for eight years and that I have learned nothing.
lgmayka
Do you think that 70 is a lot out of millions of eastern European men?
No. That was precisely my point: It is absurd to a priori "decide" that a 4800-year-old SNP first arose in Western Europe without comprehensive, dense sampling of the rest of Europe, and perhaps beyond--sampling that we do not have yet for even the most basic clades like U106, much less some obscure newly discovered subclade.
And to "decide" a priori to discard any evidence contrary to one's pet hypothesis is utterly unscientific, and indeed intellectually dishonest (to oneself as well as others).
In short: "Deciding" the geographic origin of a 4800-year-old SNP is not nearly as easy as one might wish.
What downstream branches do they belong to and why do you think that it was one way traffic from east to west for 60,000 years?
A wide variety of branches, oddly enough. And you're off by one order of magnitude. U106 is no more than 6000 years old.
Last edited by lgmayka; 17 October 2014, 08:34 PM.
I'm guessing from this that my assumption that you are merely counting the differences in the variance files between yourself and fellow S5520 was correct.
No effort to correlate this with other U106 Big Ys let alone the rest of L11+ and not taking into consideration the information in the bed files ?
T E Peterman
It's possible that the P311 mutation may have occurred to an individual within the L11 population before the L11 migration up the Danube River began. That group may have been L11+, P311- & L11+, P311+. If P311 dates to prior to 3000 BC, we can be almost certain that this happened.
I should mention that for a long time, P311 & L11 were considered to have defined the same clade. Usually separate mutations like this didn't happen at the same time. Eventually, participants who were L11+, P311- must have turned up.
1798: Have you determined yet where the other S5520+ men live & where their patrilines are from. Are ALL of them from Ireland or Scotland? Or are some from other places?
Originally posted by lgmayka View Post
Is it wrong to assume that M222 had an origin in the Isles? Is it wrong to assume that Q1a3a had an origin in America?
The 60,000 year ref. was not about U106. It was about the time that AMH arrived in south west Asia.
At present Ireland and Scotland and that could change with tests from other regions.
You are so wrong.I know how to analyse the files.
I suggest that the U106 project try to get as many U106+ people as possible to test for the S5520 SNP.
If the S5520 mutation predates the population split between the P312 proto-Celts and U106 proto Germans... as I have said all along, there is a possibility that your branch of U106 could have crossed over & become part of the proto-Celts before reaching the Isles. This isn't the most likely explanation, but I haven't ruled it out. This would be consistent with the interpretation that R1b moved from Anatolia or the Pontic Steppe into Europe 4500 years ago.
236 U106 Big-Y kits have been analysed and only four are positive for S5520. There is no need to ask those who are U106 to test, only those who are Z156. Z156 has four branches at present that I know of and there are modals for some of them. My branch may have come to the Island with the copper workers. I don't know. I only know that it is old enough to be Bronze-Age and I already posted that two years ago.
Is it wrong to assume that M222 had an origin in the Isles?
Yes, it is, unless one has investigated and found good explanations for all the occurrences of M222 on the Continent and in Scandinavia. Once again, circular logic is not permitted.
Is it wrong to assume that Q1a3a had an origin in America?
Yes, it is. Q-M3 has been found in Siberia. It is not clear yet whether it first arose there, or whether it back-migrated from America.
To state that Rb in western Europe today originated in the Steppe or around the Black Sea is circular logic.


text:
using SpiceSharp.Components.SwitchBehaviors;

namespace SpiceSharp.Components
{
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    /// A model for a <see cref="CurrentSwitch"/>
    /// </summary>
    public class CurrentSwitchModel : Model
    {
        /// <summary>
        /// Creates a new instance of the <see cref="CurrentSwitchModel"/> class.
        /// </summary>
        /// <param name="name">The name of the model</param>
        public CurrentSwitchModel(string name) : base(name)
        {
            // Add parameters
            ParameterSets.Add(new CurrentModelParameters());
        }
    }
}

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\section{Introduction}
\label{sec:intro}
The damping of primordial magnetic fields (PMF) heats electrons and baryons through dissipative effects \citep{Jedamzik1998, Subramanian1998}. This causes two interesting signals in the cosmic microwave background (CMB). One is due to the effect on the CMB spectrum: the extra energy input from dissipating PMF through the electrons leads to up scattering of CMB photons, creating a $y$-distortion \citep[see][for recent overview on distortions]{Chluba2011therm, Chluba2014Moriond} after recombination, with $y$-parameter up to $y\simeq \pot{\rm few}{-7}$ \citep{Jedamzik2000, Sethi2005, Kunze2014, Kunze2015}. The second signal is seen as a change of the CMB anisotropies \citep{Sethi2005, Kunze2014, Kunze2015}: the damping of PMF heats electrons above the CMB temperature. This reduces the effective recombination rate of the plasma, leading to a delay of recombination and modifications of the Thomson visibility function.

The changes of the CMB anisotropy power spectra caused by PMF-induced heating adds to the effects of PMF on the Einstein-Boltzmann system of cosmological perturbations\footnote{In the standard treatment of magnetically induced cosmological perturbations, PMF contribute to energy density, pressure terms and and generate a Lorentz force on baryons.}. The latter effects have been subject of several investigations \citep[see][for review]{Giovannini:2005jw} and were used to derive upper limits on the PMF amplitude smoothed on $1\,{\rm Mpc}$ scale of $B_{1\,{\rm Mpc}} \lesssim \text{few}\times{\rm nG}$ with pre-{\sc Planck}\ \citep{Paoletti:2010rx,Shaw:2010ea,Paoletti:2012bb} and {\sc Planck}\ \citep{Planck2013params,Ade:2015cva} data.
In this paper, we discuss limits on the PMF amplitude using {\sc Planck}\ 2013 data \citep{Ade:2013ktc, Ade:2013kta}, {\it only} considering the effect of PMF-induced heating on the CMB anisotropies caused by changes in the ionization history.

Previously, an approach similar to {\tt recfast} \citep{Seager2000} was used to estimate the effects on
the CMB energy spectrum and CMB anisotropies \citep[e.g.,][]{Kunze2014}. While for the standard cosmology \citep{WMAP_params, Planck2013params}, {\tt recfast} reproduces the calculations of detailed recombination codes like {\tt CosmoRec} \citep{Chluba2010b} and {\tt HyRec} \citep{Yacine2010c} very well \citep{Shaw2011}, it was not developed for non-standard scenarios. We find that the effect of heating by PMF on the ionization history is overestimated because the photoionization coefficient inside {\tt recfast} is evaluated using the electron temperature, $T_{\rm e}$. Physically, the heating does not alter the CMB blackbody significantly. Thus, the photoionization coefficient should be evaluated using the CMB blackbody temperature, as discussed in \citet{Chluba2010} and also done in \citet{Sethi2005}. When comparing to {\tt CosmoRec}, we find that after this modification the agreement becomes very good. We also confirmed that collisional ionizations of both hydrogen and helium remain negligible until electron temperatures $T_{\rm e} \simeq 10^4\,{\rm K}$ at redshift $z\lesssim \text{few}\times 10^2$ are reached. This is only achieved for significant PMF heating by strong fields, in excess of current limits on the magnetic field amplitude of a few nG. Thus the main effect that changes the ionization history, is a reduction of the recombination rate due to the higher electron temperature rather than extra ionizations.

Our computations have two implications for the CMB. Firstly, the effect on the CMB power spectra from heating by PMF is reduced significantly. This implies that expected limits on the spectral index and amplitude of PMF derived from CMB anisotropy measurements become weaker.
Secondly, the departure of the electron temperature from the CMB temperature increases, because Compton cooling is reduced. Still, we find that the difference in the $y$-distortion signal from heating by PMF is not as large, since reduction of the free electron fraction and increase of the electron temperature more or less cancel each other (overall the same amount of energy is transferred to the CMB). The aspects discussed here may also be relevant to computations of the effect of PMF on the primordial chemistry \citep[e.g.,][]{Schleicher2008b, Schleicher2008} and 21cm signals \citep[e.g.,][]{Schleicher2009, Sethi2009}.
Modified versions of {\tt CosmoRec} and {\tt recfast++}, which include heating by PMF will be made available at \url{www.Chluba.de/CosmoRec}.

\vspace{-0mm}
\section{Computations of the ionization history}
\label{sec:results}
We consider a stochastic background of non-helical PMF characterized by
\begin{align}
\label{eq:SBofPMF}
\langle B_i(\mathbf{k})B_j^*(\mathbf{h}) \rangle = (2\pi)^3\,\delta^{(3)}(\mathbf{k}-\mathbf{h})\,
P_{ij}(k) \,P_{\rm B} (k)/2,
\end{align}
where $P_{ij}(k) = \delta_{ij} - \hat{k}_i \hat{k}_j$ and $P_{\rm B} (k) = A \, k^{n_{\rm B}}$ determines the PMF power spectrum, with amplitude, $A$, and spectral index, $n_{\rm B}$. As a measure for the
comoving integrated squared amplitude of the PMF, $B^2 = B^2_0/a^4$, we consider the treatment adopted by \citet{Kunze2014}:
\begin{align}
\label{eq:B2}
B_0^2=\left<B^2\right>
= \frac{A}{2 \pi^2} \int_0^\infty {\,\rm d} k \, k^{n_\mathrm{B}+2} \, \exp\left[{-\frac{2k^2}{k_{\rm D}^2}}\right]
= \frac{A\,k_{\rm D}^{(n_{\rm B}+3)/2}}{2^{\frac{n_{\rm B}+5}{2}} \Gamma\left(\frac{n_{\rm B}+3}{2}\right)},
\end{align}
where a Gaussian filter is used and the damping scale is given by \citet{Kunze2014}:
\begin{align}
k_{\rm D} \approx 286.91 \left({\rm nG}/B_0 \right) {\rm Mpc}^{-1}.
\label{kdKK}
\end{align}
We use the CGS conventions, i.e.  $\left<\rho_{\rm B}\right>=B_0^2/8\pi$ is the average comoving magnetic field energy density.

To include the effect of dissipation from PMF, we follow the procedure of \citet{Sethi2005} and \citet[][henceforth, KK14]{Kunze2014}. We implemented both the heating ($\Gamma\equiv {\,\rm d} E/{\,\rm d} t\equiv $ released energy per volume and second) by {\it ambipolar diffusion} and {\it decaying magnetic turbulence} (see Appendix~\ref{sec:heating_rates} for additional details). The PMF heating has to be added to the electron temperature equation with
\begin{align}
\label{eq:dT_dt}
\frac{{\,\rm d} T_{\rm e}}{{\,\rm d} t}=- 2 H T_{\rm e}
+ \frac{8 \sigTN_{\rm e} \,\rho_\gamma}{3m_{\rm e} c N_{\rm tot}} (T_{\gamma}-T_{\rm e})+\frac{\Gamma}{(3/2)k N_{\rm tot}}.
\end{align}
Here, $H(z)$ denotes Hubble rate, $N_{\rm tot} =N_{\rm H}(1+f_{\rm He}+X_{\rm e})$ the number density of all ordinary matter particles that share the thermal energy, beginning tightly coupled by Coulomb interactions; $N_{\rm H}$ is the number density of hydrogen nuclei, $f_{\rm He}\approx Y_{\rm p}/ 4(1-Y_{\rm p})\approx 0.079$ for helium mass fraction $Y_{\rm p}=0.24$; $X_{\rm e}=N_{\rm e}/N_{\rm H}$ denotes the free electron fraction and $\rho_\gamma=a_{\rm R} T_{\gamma}^4\approx 0.26 \, {\rm eV} (1+z)^4$ the CMB energy density.
The first term in Eq.~\eqref{eq:dT_dt} describes the adiabatic cooling of matter due to the Hubble expansion, while the second term is caused by Compton cooling and heating. The last term accounts for the PMF heating. Notice that the last two terms in Eq.~\eqref{eq:dT_dt} differ slightly from those presented in earlier works \citep[e.g.,][]{Sethi2005}. One reason is that the heat capacity contribution from helium was neglected so that for the Compton cooling term $N_{\rm tot} \approx N_{\rm H}(1+X_{\rm e})$. Secondly, for the PMF-induced heating term, the thermal energy was distributed only among the hydrogen atoms, $N_{\rm tot} \approx N_{\rm H}=N_{\rm e}/X_{\rm e}$, although even without helium, the free electrons contribute. However, we find that this only changes the free electron number by $\Delta N_{\rm e}/N_{\rm e} \simeq 10\%-20\%$ in the freeze-out tail.

We modified both {\tt recfast++} (which by default is meant to reproduce the original version of {\tt recfast}) and {\tt CosmoRec} to include the effects of heating by magnetic fields. For {\tt recfast++}, we can separately adjust the computation of the photoionization coefficients for hydrogen and helium. In the default setting, they are evaluated using the matter temperature, $T=T_{\rm e}$, as in {\tt recfast}. From the physical point of view, the photoionization coefficient, $\beta_{i\rm c}$, of an atomic level $i$ is a function of both photon and electron temperatures, $T_{\gamma}$ and $T_{\rm e}$, respectively. The dependence on the electron temperature enters through Doppler boosts. Even for high electron temperatures, this correction can be neglected, so that one has $\beta_{i\rm c}=\beta_{i\rm c}(T_{\gamma}, T_{\rm e})\approx \beta_{i\rm c}(T_{\gamma})\approx 4\pi \int \frac{B_\nu(T_{\gamma})}{h\nu} \sigma_{i\rm c}(\nu) {\,\rm d} \nu$, where $B_\nu(T_{\gamma})$ is the CMB blackbody intensity \citep[e.g.,][]{Seager2000}. Clearly, without significant distortions of the CMB radiation field, this expression directly confirms that the photoionization rate, $R_{i\rm c}=N_i \, \beta_{i\rm c}(T_{\gamma})$, where $N_i$ is the population of the level $i$ of the atom, depends only on the photon temperature. Thus, the effective (case-B) photoionization rate also only depends on the photon temperature, a modification that causes a big difference for the effect of heating by PMF, as we show below.

In contrast to this, the photo-recombination coefficient, $\alpha_{{\rm c} i}$, to atomic level $i$ mainly depends on the electron temperature, with a smaller correction due to stimulated recombinations in the ambient CMB blackbody radiation field. This implies, $\alpha_{{\rm c} i}=\alpha_{{\rm c} i}(T_{\rm e}, T_{\gamma})$, which for the {\tt recfast} treatment is set to $\alpha_{{\rm c} i}\approx \alpha_{{\rm c} i}(T_{\rm e}, T_{\gamma}=T_{\rm e})$. For the detailed recombination calculations, this approximation becomes inaccurate for highly excited levels \citep[e.g.,][]{Chluba2007}, changing the freeze-out tail of recombination at the percent level \citep{Chluba2007, Grin2009, Chluba2010}. In {\tt CosmoRec} and {\tt HyRec}, the full temperature dependence of the photo-recombination coefficient is taken into account using an effective multi-level atom method \citep{Yacine2010}. When including heating by PMF, the {\tt recfast} treatment thus slightly overestimates the photo-recombination rate to each level, since for $T_{\gamma}\ll T_{\rm e}$ stimulated recombinations are overestimated when assuming $T_{\gamma}=T_{\rm e}$. However, the difference is much less important than the error caused by evaluating the photoionization coefficient for $T=T_{\rm e}$.

\subsection{Collisional ionization}
The exponential dependence on the ionization potential suppresses the effect of collisional ionization from the ground state, so that in the standard computation they can be neglected \citep{Chluba2007}.
Since at low redshifts ($z\lesssim 800$) the electron temperature can be pushed quite significantly above the CMB photon temperature by heating processes (lower panels in Fig.~\ref{fig:examples} and \ref{fig:examples_II}), it is important to check if collisional ionizations by electron impact\footnote{Protons are heavier and thus slower, so that their effect is much smaller.} become efficient again. Using the fits of \citet{Bell1983}
\begin{align}
\label{eq:dN_dt_coll}
\frac{{\,\rm d} N_{\rm 1s, HI}}{{\,\rm d} t}
&\approx - \pot{5.85}{-9} T_4^{1/2} \expf{-T_{\rm H}/T} {\rm cm^3} \,{\rm s^{-1}}\,N_{\rm 1s, HI} \,N_{\rm e}
\nonumber
\\
\nonumber
\frac{{\,\rm d} N_{\rm 1s, HeI}}{{\,\rm d} t}
&\approx - \pot{2.02}{-9} T_4^{1/2} \expf{-T_{\rm He}/T}  {\rm cm^3}\, {\rm s^{-1}}\,N_{\rm 1s, HeI} \,N_{\rm e}
\end{align}
with $T_{\rm H}\approx \pot{1.58}{5}\, {\rm K}$, $T_{\rm He}\approx \pot{2.85}{5}\, {\rm K}$ and $T_4=T/10^4\,{\rm K}$, where $T\equiv T_{\rm e}$, we confirm that this effect can usually be neglected. We nevertheless add these rates to the calculation whenever heating by PMF is activated and for very large heating (pushing the electron temperature up to $T_{\rm e}\simeq 10^4\,{\rm K}$) they do become important in limiting the maximal electron temperature. We also included the cooling of electrons by the collisional ionization heating to ensure the correct thermal balance.

\begin{figure}
\centering
\includegraphics[width=0.97\columnwidth]{./eps/fig_1.pdf}
\\[1mm]
\includegraphics[width=0.97\columnwidth]{./eps/fig_2.pdf}
\caption{Effect of heating by decaying magnetic turbulence on the ionization history (upper panel) and electron temperature (lower panel) for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$.}
\label{fig:examples}
\end{figure}

\subsection{Decaying magnetic turbulence}
Using {\tt recfast++} with default setting, we are able to reproduce the central panel in Fig.~10 of KK14 for decaying magnetic turbulence.
One example, for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$ is shown in Fig.~\ref{fig:examples}. We compare the standard recombination history (no extra heating) with three cases obtained from {\tt recfast++} and the full computation of {\tt CosmoRec}. The effect of reionization at $z\lesssim 10$ was not included \citep[see][for some discussion]{Kunze2015}, as it does not affect our main discussion. The first agrees well with the result of KK14, with a large change in the freeze-out tail of the recombination history being found (dotted line). Modifying the evaluation of the hydrogen photoionization rate to $T=T_{\gamma}$ gives a smaller change (dash-dotted line). Also changing the evaluation of the helium photoionization rate finally gives the dashed line, with a $\simeq 5$ times smaller effect on the freeze-out tail. Using the standard {\tt recfast} approach, the photoionization rate is thus overestimated so that even helium is partially reionized. We find that after changing the evaluation of the photoionization rates to $T=T_{\gamma}$ the result obtained with {\tt recfast++} agrees to within $\simeq 10\%$ with the detailed treatment of {\tt CosmoRec} (solid/red line).
This case is also fairly close to the result for $m= 2(n_{\rm B}+3)/(n_{\rm B}+5)=0.1(\equiv n_{\rm B}\simeq -2.9)$ shown in Fig.~4 of \citet{Sethi2005}. The remaining difference to {\tt CosmoRec} is caused by stimulated recombination effects that are not captured correctly with a {\tt recfast} treatment.

Our computations show that the smaller effect on the free electron fraction allows the electron temperature to rise higher above the photon temperature than with the default {\tt recfast} treatment  (see Fig.~\ref{fig:examples}). This is because for  a lower free electron fraction, Compton-cooling becomes less efficient.
We find that in terms of the Compton-$y$ parameter, these two effects practically cancel each other, leaving a difference at the level of $\lesssim 5\%$. For instance, computing the $y$-parameter, $y=\int \frac{k (T_{\rm e}-T_{\gamma})}{m_{\rm e} c^2} \sigma_{\rm T} N_{\rm e} c {\,\rm d} t$, for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$ using the default {\tt recfast++} result we obtain $y\simeq \pot{1.0}{-7} (B_0/3\,{\rm nG})^2$, while when evaluating the photoionization rates correctly we have $y\simeq \pot{9.7}{-8}$, corresponding to a $\simeq 4\%$ effect. For larger spectral index, the difference becomes even smaller. For $B_0=3\,{\rm nG}$ and $n_{\rm B}=0$, we find $y\simeq \pot{5.4}{-7}(B_0/3\,{\rm nG})^2$ with a difference $\lesssim 1\%$ in the two treatments. The reason is that for larger spectral index, most of the effect arises from higher redshifts ($z\simeq 10^3$), which are less sensitive to the evaluation of the photoionization rates since Compton-cooling is still extremely efficient, forcing $T_{\rm e}\simeq T_{\gamma}$.

In the treatment of the heating by decaying magnetic turbulence, we switch the effect on rather abruptly ($\Delta z/z\simeq 5\%$) around $z_i\simeq 1088$ following previous approaches \citep{Sethi2005, Schleicher2008, Kunze2014}.  Although the effect of heating by decaying magnetic turbulence is not as visible at early times (see Fig.~\ref{fig:examples}), this approximation adds uncertainty to the predictions of the CMB anisotropies since small effects close to the maximum of the Thomson visibility function can have a larger effect than similar changes in the freeze-out tail \citep[e.g.,][]{Jose2008, Farhang2011}. For detailed CMB constraints, this approximation should be improved, including more detailed consideration of the time-dependence of the heating rate at $z>z_i\simeq 1088$. For example, when changing from very abrupt to more smooth transition between no heating and heating at $z\simeq z_i$, we find that the numerical result for the $TT$ power spectrum at large scales ($\ell\lesssim200$) is affected noticeably.
However, in the present paper we shall follow the previous approach, addressing order-of-magnitude questions only.

\begin{figure}
\centering
\includegraphics[width=0.97\columnwidth]{./eps/fig_1_II.pdf}
\\[1mm]
\includegraphics[width=0.97\columnwidth]{./eps/fig_2_II.pdf}
\caption{Effect of ambipolar diffusion on the ionization history (upper panel) and electron temperature (lower panel) for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$. For comparison, we also show the case obtained with settings similar to  \citet{Sethi2005}.}
\label{fig:examples_II}
\end{figure}

\subsection{Ambipolar diffusion}
For heating by ambipolar diffusion, we also find a reduction of the effects when modifying the evaluation of the photoionization rates. This is illustrated in Fig.~\ref{fig:examples_II}, again for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$. The effect of reionization was not modeled. Evaluating the photoionization rates correctly reduces the effect on the freeze-out tail by more than one order of magnitude.
Also, the low-redshift electron temperature is underestimated by roughly one order of magnitude, with a plateau rising to $T_{\rm e} \simeq 10^4\,{\rm K}$.
Comparing with Figures~1 and 2 of \citet{Sethi2005}, we find good agreement with our computation when setting $\left<L^2\right>\approx \rho_{\rm B}^2/ l^2_{\rm d}$, which is equivalent to setting $f_L=1$ (see lines labeled `SS2005' in our Fig.~\ref{fig:examples_II}) for the average Lorentz force caused by the PMF.

With the expressions given in Appendix~\ref{sec:heating_rates}, we are also able to reproduce Fig.~10 of KK14 for the ambipolar diffusion case; however, we had to multiply our heating rate by a factor of $1/(8\pi)^2$, albeit being based on the same expressions. We confirmed the order of magnitude of the heating rates for $n_{\rm B}=-2.9$ using an alternative evaluation based on the analytic expressions of \citet{Finelli2008} and \citet{Paoletti2009}, finding that the importance of the process was indeed underestimated. This changes the $y$-parameter contribution caused by ambipolar diffusion. Including only heating due to ambipolar diffusion for $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$ we find $y\simeq \pot{3.1}{-11}(B_0/3\,{\rm nG})^2$ for the heating rate of KK14, while here we find $y\simeq \pot{6.6}{-9}(B_0/3\,{\rm nG})^2$. Relative to the contribution from decaying magnetic turbulence this is a small correction, well below the precision of the approximations made in the computation. However, for larger spectral index, the effect becomes more important. For $B_0=3\,{\rm nG}$ and $n_{\rm B}=0$ we find $y\simeq \pot{7.5}{-10}(B_0/3\,{\rm nG})^2$ using the evaluation of KK14 but $y\simeq \pot{1.1}{-7}(B_0/3\,{\rm nG})^2$ with our treatment, making this contribution comparable to the one from heating by decaying magnetic turbulence.

For ambipolar diffusion, the numerical treatment mainly depends on the evaluation of the average of the Lorentz force squared and the distribution used to characterize the stochastic background of PMF as small scales. \citet{Sethi2005} and  \citet{Schleicher2008}, adopted an order of magnitude estimate, i.e., $\left<L^2\right>\approx \rho_B^2/ l^2_{\rm d}$, while in KK14, expressions from \citet{Kunze2011} were used. This introduces a strong dependence of the heating by ambipolar diffusion on $n_{\rm B}$, reducing the effect significantly as the spectral index approaches $n_{\rm B}\simeq -3$.
Using a sharp cut-off instead to approximate the effect of damping at small-scales allows obtaining exact analytic expressions for the energy-momentum tensor correlators \citep{Finelli2008,Paoletti2009}. However, here we adopt the approximations of \citet{Kunze2011} to illustrate the effects.

\begin{figure}
\centering
\includegraphics[width=0.97\columnwidth]{./eps/fig_3_I.pdf}
\\[1mm]
\includegraphics[width=0.97\columnwidth]{./eps/fig_3_II.pdf}
\caption{Effect of PMF heating on the $TT$ and $EE$ power spectra for two choices of the PMF power spectrum parameters. The standard {\sc Planck}\ 2013 cosmology with $\tau=0.09$ was used. See Sect.~\ref{sec:CMB_effects} for discussion.}
\label{fig:examples_III}
\end{figure}

\vspace{-2mm}
\section{Effects on the CMB anisotropies}
\label{sec:CMB_effects}
The changes to the ionization history introduced by heating from magnetic field inevitably affects the CMB temperature and polarization anisotropies \citep{Sethi2005, Kunze2014, Kunze2015}. We can estimate the importance of this effect using {\tt camb} \citep{CAMB} with our modified recombination codes. We use the {\sc Planck}\ 2013 cosmology \citep{Planck2013params} with reionization optical depth $\tau=0.09$.
Changes of the free electron fraction around decoupling $z\simeq 1100$ usually weigh more than modifications at late times in the freeze-out tail \citep[e.g.][]{Jose2008, Farhang2011}. Thus, although not as visible in Fig.~\ref{fig:examples} and \ref{fig:examples_II}, especially at small scales, a large part of the effect on the CMB power spectra arises from modifications at $z\simeq 1100$, causing additional diffusion damping and shifts in the positions of the acoustic peaks.

For ambipolar diffusion, the effect on the ionization history around $z\simeq 1100$ is much smaller than for decaying magnetic turbulence. The former mainly affects the freeze-out tail and thus the optical depth to the last scattering surface, $\tau$. This leads to extra $\simeq \expf{-2\tau}$ damping of the CMB anisotropies at small scales, an effect that is partially degenerate with the curvature power spectrum amplitude, $A_\zeta$, and its spectral index $n_{\rm S}$. Extra polarization at large scales is generated by re-scattering events, an effect to which CMB polarization data is sensitive \citep[see also][]{Kunze2015}.
These effects are very similar to changes to the CMB power spectra caused by dark matter annihilation \citep{Chen2004, Padmanabhan2005, Zhang2006}, so that some degeneracy with this process is expected, especially when including the effect of clumping at late times \citep{Huetsi2009}, which can boost the free electron fraction in the freeze-out tail in a similar manner.
For decaying magnetic turbulence, the Thomson visibility function is affected close to its maximum, so that changes in the positions of the acoustic peaks are found, which can be tightly constrained using CMB data.

In Fig.~\ref{fig:examples_III}, we show the separate contributions from decaying magnetic turbulence and ambipolar diffusion to the changes in the $TT$ and $EE$ power spectra. For $B_0=3\,{\rm nG}$ and $n_{\rm B}=-2.9$, the effect of ambipolar diffusion is small and the dominant effect is caused by decaying magnetic turbulence, which introduces clear shifts in the positions of the acoustic peaks.
Setting $n_{\rm B}=3.0$, we see that ambipolar diffusion does add a significant correction, $\Delta \tau\simeq -6\%\,(B_0/3\,{\rm nG})^2$, to the Thomson optical depth. At very low $\ell$, it also introduces features into the power spectra, which help breaking the degeneracies mentioned above.
The shifts in the peak positions due to decaying magnetic turbulence also increase strongly for this case.
Notice that the heating rates for both decaying magnetic turbulence and ambipolar diffusion scale as $\Gamma\propto B^2_0$, so that the changes in the CMB power spectra strongly decrease with $B_0$. The aforementioned effects can be constrained with current data, and one expects decaying magnetic turbulence to drive the limits, at least for quasi-scale invariant PMF power spectra.

\vspace{-2mm}
\subsection{Constraints from {\sc Planck}\ 2013 data}
In this section, we discuss constraints on the PMF power spectrum using {\sc Planck}\ 2013 data \citep{Planck2013params}.
We explicitly include {\em only} the effect of PMF-induced heating on the CMB power spectra.
Taking into account {\em only} the PMF contributions to the Einstein-Boltzmann system for cosmological perturbations, the {\sc Planck}\ 2013 95\% c.l. upper limit on the magnetic field strength, smoothed over $1\,{\rm Mpc}$ length, is\footnote{In \cite{Planck2013params} the constraint on the amplitude of PMF is quoted in terms of $B_{1\,{\rm Mpc}}$, i.e., the amplitude smoothed over $1\,{\rm Mpc}$ length, which is often considered in the literature \citep{Paoletti:2010rx,Shaw:2010ea}. Note that the relation $B_0^2 = (k_{\rm D} \lambda /\sqrt{2})^{n_B+3} B_{\lambda}^2$. We have therefore $B_0 \simeq 1.3 \, B_{1\,{\rm Mpc}}$ for $k_{\rm D}$ given by Eq. (\ref{kdKK}), $\lambda = 1$ Mpc and $n_{\rm B} = -2.9$.} $B_{1\,{\rm Mpc}} \lesssim 4.1\,{\rm nG}$, obtained by varying $n_{\rm B}$ in the interval $[-2.9,3]$.

\begin{figure}
\centering
\includegraphics[width=0.97\columnwidth]{./eps/KK.pdf}
\caption{Posterior distribution for the PMF strength, $B_0$, with $n_{\rm B}=-2.9$ and different combinations of heating by decaying magnetic turbulence (MHD) and ambipolar diffusion.}
\label{fig:B0}
\end{figure}
In Fig.~\ref{fig:B0}, we show the posterior distribution for $B_0$ at fixed $n_{\rm B}=-2.9$. We compare three cases, including the heating caused by decaying magnetic turbulence, ambipolar diffusion and the combination of both. The 95\% upper limits on the magnetic field strength are $B^{\rm MHD}_0 \lesssim 1.1\,{\rm nG}$, $B^{\rm ambi}_0 \lesssim 1.5\,{\rm nG}$ and $B_0 \lesssim 1.1\,{\rm nG}$, respectively. As anticipated earlier, decaying magnetic turbulence strongly drives the constraint and shape of the posterior distribution of $B_0$, with ambipolar diffusion leading to a correction only. It is also clear that the limits $B^{\rm MHD}_0$, $B^{\rm ambi}_0$ and $B_0$ are so comparable mainly because the posteriors have strong non-Gaussian tails.

Evaluating the photoionization rates using $T=T_{\rm e}$, we expect an upper limit of $B_0 \lesssim 0.5\,{\rm nG}$ (95\% c.l.) when including both ambipolar diffusion and decaying magnetic turbulence. This is about $\simeq \sqrt{5}\simeq 2.2$ times tighter than the limit quoted above, simply because the effect on the ionization history is overestimated. This illustrates how important the modification to the {\tt recfast} treatment discussed here is.

\section{Conclusions}
We investigated the effect of heating due to {\it ambipolar diffusion} and {\it decaying magnetic turbulence} on the thermal and ionization history of our Universe. We find that changes in the ionization history, computed with an approach similar to {\tt recfast}, are significantly overestimated when compared with {\tt CosmoRec}.
However, after evaluating the photoionization rates at the photon temperature, $T=T_{\gamma}$, the results agree to within $\simeq 10\%$ with the more detailed treatment.
The remaining difference to {\tt CosmoRec} is mainly because of stimulated recombination effects.

For the Compton $y$-parameter computed in different treatments of the problem, we find only small differences at the level of $\lesssim 5\%$ for decaying magnetic turbulence. This is because the reduction of the effect on the free electron fraction is roughly compensated by the increase in the electron temperature.
However, our computations do show that the $y$-parameter contribution caused by ambipolar diffusion was underestimated. For nearly scale-invariant PMF power spectrum, ambipolar diffusion still causes only a small correction relative to the $y$-parameter contribution from decaying magnetic turbulence; however, for $n_{\rm B}\simeq 0$ the two contributions become comparable in order of magnitude.

Using {\sc Planck}\ 2013 data and only including the PMF heating effect, we find an upper limit on the magnetic field strength of
$B_0 \lesssim 1.1\,{\rm nG}$ (95\% c.l.) for a PMF power spectrum with spectral index $n_{\rm B}=-2.9$.
As shown in \citet{Ade:2015cva}, the heating effect considered here leads to a tighter constraint than the one derived by considering {\em only} the direct effects of PMF on the cosmological perturbations. The improvement is approximatively a factor of $3$ for {\sc Planck}\ 2015 data \citep{Ade:2015cva} and $n_{\rm B}=-2.9$. However, we expect uncertainties in the modeling of the heating by decaying magnetic turbulence to affect the results for quasi-scale invariant PMF power spectra,
while for blue PMF power spectra, details in the modeling of ambipolar diffusion becomes important. Given that the effects of PMF heating studied here are so competitive with those of PMF on the fluid perturbations, this problem deserves more careful consideration, in particular with respect to future improved measurements of polarization on large angular scales by {\sc Planck}, which could lead to a better estimate of $\tau$.

An additional uncertainty is caused by the way the reionization epoch is added at $z\lesssim 10$. Currently, we simply use the {\tt camb} default prescription that ensures a smooth transition at the start of reionization. However, for strong PMF, the pre-reionization at $z\gtrsim 10$ can be significant (see Fig.~\ref{fig:examples} and \ref{fig:examples_II}), so that priors on the total optical depth need to be considered more carefully. This is expected to be important only for very blue PMF power spectra or when the PMF amplitude becomes very large.

For quasi-scale invariant PMF power spectra, our analysis suggests that PMF heating can contribute no more than $y\lesssim \pot{1.1}{-8}$ (95\% c.l.) to the average Compton $y$ distortion. Although measurements with a PIXIE-like experiment \citep{Kogut2011PIXIE} could reach this sensitivity, a much larger distortion ($y\simeq 10^{-7}-10^{-6}$) is created just from the reionization and structure formation process \citep{Hu1994pert, Cen1999, Refregier2000}. Thus, it will be very difficult to use future spectral distortions measurements to constrain the presence of PMF in the early Universe in a model-independent way.

Finally, we confirmed that evaluating the photoionization rates at $T=T_{\gamma}$ in {\tt recfast++} does not affect the ionization history by more than $\Delta N_{\rm e}/N_{\rm e}\simeq 0.3\%$ at $z\simeq 780$ for the standard cosmology and thus has no significant effect on the analysis of current and upcoming CMB data. To improve the consistency of the {\tt recfast} treatment one could thus change this convention and then recalibrate the fudge-functions without additional changes.

Our results are important for the derivation of constraints on the PMF power spectrum obtained from measurements of the cosmic microwave background anisotropies with {\sc Planck}\ full-mission data \citep[see][]{Ade:2015cva}. They may also be relevant to computations of the effect of PMF on the primordial chemistry \citep[e.g.,][]{Schleicher2008b, Schleicher2008} and 21cm signals \citep[e.g.,][]{Schleicher2009, Sethi2009}. In all cases, it will be important to improve the description of the PMF heating rate, since current approximations introduce noticeable uncertainty. This will be left for future work.

\small
\vspace{-3mm}
\section*{Acknowledgments}
We wish to thank Yacine Ali-Ha{\"i}moud, E. Komatsu, K. Kunze, G. Sigl and K. Subramanian for comments and suggestions.
JC is supported by the Royal Society as a Royal Society University Research Fellow at the University of Cambridge, U.K.
JARM acknowledges financial support from the Spanish Ministry
of Economy and Competitiveness under the 2011 Severo
Ochoa Program MINECO SEV-2011-0187, and the Consolider-Ingenio
project CSD2010-00064 (EPI: Exploring the Physics of Inflation).

{
\vspace{-3mm}
\small
\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


Possession of a prohibited drug the law in New South Wales under the provisions of s 10 of the Drug Misuse and Trafficking Act 1985 (NSW), it is an offence for a person to have a prohibited drug in his or her possession. However, when talking about possession, the question of what constitutes possession is a multilayered question because there are a number of different associated elements that includes knowledge, intent, custody and control.
the person knew that this was the case.
Defining what is custody and control can be broken down in the following manner. In relation to custody of a prohibited drug, a person may be seen to be in custody of an illegal drug if it is within their immediate physical possession – most obviously, having a drug in their pockets for example. Reference to the control element can mean that the person has the right to keep, use, or share the prohibited drug.
How is custody and control proven?
In order to demonstrate a person has custody and control, it must be proven that the person had control over the prohibited drug, either in their vehicle or place of residence for example. However, it should be pointed out that just because a prohibited drug was found within a person's property, it does not necessarily mean they have ownership of all articles and items within the property.
The question of custody and control is extremely nuanced. So, if a person is aware that one of their housemates has control of a prohibited drug on the property for example, they may still not be guilty of possession, as was the case in R v Fillipetti (1984) 13 A Crim R 334. The appellant, Edward Fillippetti resided with six other people, all of whom had access to and made free use of the lounge room where police found a large quantity of cannabis. The appellant was charged with (deemed) supply on the basis of possession of a quantity of cannabis in excess of the prescribed quantity and was convicted, and subsequently appealed.
The appeal was allowed and it was held by Street CJ and Maxwell JJ that access to, and use of the place where the cannabis was found by others meant that the Crown had not produced enough evidence to negate possession on the part of any other occupants. Furthermore, the Court of Criminal Appeal, New South Wales, also held there was insufficient evidence to enable the jury to come to the conclusion that the cannabis was in the appellant's exclusive physical control.
Although with that being said, a person may be guilty of an offence of possession of a prohibited drug, even if the custody or control was momentary – such as having a marijuana water pipe handed to them.
Drug charges are a serious offence that may result in imprisonment. If you have been charged with a drug offence, it is imperative you contact George Sten & Co Criminal Lawyers for our specialised legal advice. With over 50 years experience in this area of law, our criminal lawyers will be able to assist you in building your case and gaining the best possible result.


text:
NS20, NS 20, NS-20, NS.20, or variation, may refer to:

Places
 Novena MRT station (station code: NS20), Novena, Singapore; a mass transit station
 Guysborough-Eastern Shore-Tracadie (constituency N.S. 20), Nova Scotia, Canada; a provincial electoral district

Technology
 NS-20 inertial navigation system, for the D37D flight computer of the LGM-118 Peacekeeper
 Travan NS20, data backup tape standard
 Element NS20, a brand of e-cigarette

Other uses
 Lakshya (2021 film), codenamed "NS20"
 New Penguin Shakespeare volume 20
 Blue Origin NS-20, a Blue Origin suborbital spaceflight by the New Shepard space capsule on 31 March 2022

See also

 NS (disambiguation)
 20 (disambiguation)

redpajama_set_name: RedPajamaWikipedia


The AS 300 is a 3 seater hot tub which includes a lounger and 2 deep seats and having 31 Hydrotherapy Jets, a 2 Speed Pump, Ozonator, Deluxe LED Lighting makes this a very highly desirable Spa. The AS300 is ideal for the smaller garden or will sit nicely in a conservatory as the size makes this hot tub very flexible when it comes to delivery.
Aquadream Spas are produced with Superior Construction beyond what the eye can see, every Aquadream Spa is constructed using the finest components and expert craftsmanship throughout. From the use of Lucite's™ world recognized and luxurious acrylic surface, market leading Balboa Control Systems and the utilization of a custom molded plastic bottom to protect the home owners deck or patio and will ensure you spa base does not suffer from water ingress with pressure treated wood substructure, maintenance friendly synthetic cabinets and a heavy duty thermal cover are all components that will insure you a lifetime of hot tub enjoyment. With a selection of spa sizes to choose from a 3 seater hot tub through to the largest spa which offers seating for 7 adults you should be able to find a spa that suits your requirements.


text:
Michael Carrick Was One Of Sir Alex Ferguson's Most Important Manchester United Signings
Samuel Luckhurst
Football writer, The Manchester Evening News
Judging Sir Alex Ferguson's most important signings highlights how much the footballing landscape has changed in a quarter of a century. Peter Schmeichel, Eric Cantona and Roy Keane barely cost over £5 million in the early 90s, £1.6m was paid to Molde for Ole Gunnar Solskjaer in '96 and Cristiano Ronaldo was bought for £12.24m seven years later.
One name often overlooked is Michael Carrick's, who joined for £18.6m from Tottenham in 2006. United's first bid was a fair £10m, and while their first experience of negotiating with Daniel Levy would not be their last, it was enough to dissuade Ferguson from attempting to sign Luka Modrić in 2011.
United had been promised "two world-class players" in the summer of 2006 by duplicitous then-chief executive David Gill. Carrick and goalkeeper Tomasz Kuszczak were the only arrivals, whereas reigning champions Chelsea brought in Michael Ballack and Andriy Shevchenko. One football magazine predicted United would finish fourth ahead of the 2006-07 campaign.
The problem was the midfield. It had been 20 years earlier, as Ferguson writes in his book, ostensibly without a hint of self-awareness: "Martin Edwards gave me a list of my players. I suddenly realised, we had no midfielders, it was a nightmare."
Roy Keane's dressed-up sacking in November 2005 and Paul Scholes' eye injury the following month left United with John O'Shea and Ryan Giggs as the midfield partnership for the second half of the season. AC Milan rejected a move for Johann Vogel in January as Ferguson instead reinforced the defence, bringing in Patrice Evra and Nemanja Vidić.
By the time Carrick had followed them to Old Trafford, Scholes was fit again, and the duo would prove to be indispensable as United won their first Premier League title in four years. Certain starters, their deep-lying roles allowed Ryan Giggs, Cristiano Ronaldo, Wayne Rooney and Louis Saha to wreak havoc and United were top for all but two weeks of 2006-07.
Carrick's United career
Ahead of the next season, Ferguson supplemented the midfield with Owen Hargreaves and Anderson, who formed their own auspicious partnership at Arsenal and Liverpool as the strength in depth afforded United greater variety, and culminated in a Champions League win. Carrick started all but one of the seven knockout ties.
That 2007-08 campaign was Hargreaves' zenith at United, though, and Anderson has never truly thrived alongside anyone else since. Ferguson's astonishing decision not to sign a central midfielder in the last six years of his United era exacerbated the midfield malaise.
So it is testament to Carrick's resilience he has re-emerged despite a sub-standard supporting cast and the extensive dip in form he experienced between 2008 and 2010, when Ferguson all but labelled him the scapegoat after United's Champions League elimination by Bayern Munich.
Involved in five title wins and one of five players who started the three Champions League finals United were involved in, Carrick belatedly received recognition in May via the Players' Player of the Year award, an accolade he was more worthy of the previous term. A place in the Premier League Team of the Year and a terrace chant have also revoked his status as an unsung hero.
uk sportuk footballpremier leagueMichael CarrickDavid Moyes


Desperate to make my bedroom look like every aesthetically-pleasing IG blogger's room ever, I recently ran to my nearby florist to buy the perfect decoration- a succulent terrarium. I excitedly grabbed the most instagrammable terrarium, only to find out that it was *gulp*… $135. Way out of my budget. Determined to get the perfect terrarium (and the perfect insta), I asked The Sill exactly how to make my own succulent terrarium at home. Below, find a detailed guide from our friend at the Sill, Plant Scientist Christopher Satch.
What is a terrarium? What even are succulents?
Terrariums are cool, but making them is even cooler! Succulents are quite popular nowadays, and are the perfect candidates for those insta-worthy terrariums. Just a few things you have to know about succulents before we begin.
Succulents are living things! To be successful with them, you need to understand that they are not a piece of furniture that you can just forget about. If you pay attention to them, and care for them the way that they want, they will reward you with growth, and for some even flowers!
The term "succulent" contains plants that are unrelated, but have all adapted to living in desert conditions. That means that cacti are also succulents, and can be planted with them. Succulents are desert plants, and to make them the happiest, you have to recreate desert conditions. It's very sunny in the desert, so to make your plants happy, you have to blast them with as much sunlight as possible!
It doesn't rain often in the desert, so you won't be watering too often. Succulents show that they want water by wrinkling. If you're ever unsure of when to water, only water if the soil is bone dry. Give enough water to get all the soil uniformly moist, then let dry. If you water, and the water rushes off the sides, then you have not watered. Remember to always plant like-plants with like-plants. Never plant succulents and moss together- moss likes it wet and shady; succulents are the opposite.
Estimate the number of succulents/cacti you'll need by taking into account the size of the bowl. Typically an 8" diameter bowl can fit 4x of 1" succulents. a 6" diameter bowl can fit 3x of 1" succulents.
Choose a glass container with an opening, like a fish bowl. You can also choose a flat bowl with no cover to plant the succulents in.
Since these planters won't have drainage, line the bottom of each with an inch of lava rocks to provide a place for water to pool.
Cover the lava rocks with a layer of soil to just cover them and pack tight!
You should remove about half the old soil, but no big deal if you remove more or less.
Place them where you want, giving them space to grow.
Using a cup or your hands, stabilize them and fill in the soil around them.
WATER! Use enough water to saturate the soil but not so much that the plants are sitting in water.
Place in a sunny windowsill and you're good to go!
Gather materials - lava rocks, soil, planter, and succulents!
Add lava rocks to planter and pack a layer of soil on top. Loosen roots of succulents and arrange in planter.
Pack in more soil to stabilize plants and water until soil is wet, but plants aren't swimming in water.
Place in sunlight and watch it grow!


If you are transferring to our practice, please call our office to register your child into our system and establish them as our patient. You will need to contact your child's prior pediatrician to have them forward your child's medical records. Due to HIPPA regulations, this usually has to done in writing.
With many insurances it is MANDATORY to call your insurance carrier and select one of our doctors to be your child's new Primary Care Physician (PCP). This should be done prior to your first visit with us. If not, payment can be denied and you would be responsible for all charges incurred.
The physicians are listed as a "group" by your insurance company enabling you to schedule visits with any of the physicians in our practice.


SpellBound – Spellchecker for Firefox and the Mozilla Suite: All those comments this morning about my spelling made me self-conscious. This works beautifully.
SpellBound is a port of the spellchecker code and user interface from the Mozilla Suite's Composer that enables spell checking in web forms such as html textarea / input elements (html input password elements are not checked by SpellBound) and rich text form elements.
I was just wishing I had the time to hook something like this up after I misspelled a word in a form submission to my senator this morning.
I should just sleep later and read Gadgetopia more … then everything would be good in the world.
It's so true. Gadgetopia is really the key to a better life.
I've been using that extension for about a month now, and its been great. Not quite as good as Safari's built -in, on the fly, spell checking, because I forget sometimes to right-click and use spellbound…but very nice none the less for my windows machines.
"Safari's built -in, on the fly, spell checking"?! Dang! How long have I been using Safari & didn't know that was there? Thanks, Mike!


TECHNOLOGY IS NOT A BUZZWORD FOR US – IT IS OUR LIFELONG PROMISE.
ELIN Motoren is your life-cycle partner for rotating electrical machines and solutions, working for the best companies around the world.
With over 120 years of experience, a unique quality and comprehensive solution expertise, we generate added value over the entire life-cycle of your plant. Active flexibility is a part of our performance philosophy and enables us to develop perfectly tailored solutions – powerful, reliable, and cost optimized. The result is optimum industrial performance coupled with sustainable growth. All of which combines to make us the preferred partner in development and total solutions for exacting technical requirements.


UPromise recently (as far as I know) introduced a new program called eCoupon that allows participants to save money when shopping at local grocery stops and, at the same time, get college savings.
If you don't have a UPromise account, get one.
Register your grocery shopping cards at UPromise, which will link them to your UPromise accounts.
Every month, UPromise provides different coupons for items you usually shop, such as tissues, bottled water, snacks, detergents, etc.
Select the items you want to buy and add them to your active coupon list.
Go shopping and enjoy the savings.
Yes, that's it. Unlike other online coupon programs, you don't have to print or clip anything with UPromise' eCoupons. Because your grocery shopping cards are already linked to your UPromise account, the only thing you need to bring when you shop is your grocery cards. When you check out the items, the savings from eCoupons will be applied and rewards from the purchases (not the coupon values) will be added to your UPromise accounts as college savings.
Quite easy, right? Do you want to use it?


text:
HomeNewsWorld Series Of Poker
CodigoPoker Reports WSOP Main Event Heads-Up Delayed until January
December 28 2020 Will Shillibier
On the day Upeshka De Silva was disqualified from the WSOP Final Table for a positive COVID-19 test, there have been further ramifications for the Main Event with the news that the heads-up match will be postponed until Jan. 3.
Argentina's Damian Salas was set to play the winner of tonight's final table on Dec. 30, but according to CodigoPoker Salas has been denied entry to the United States.
This is due to him having been in Europe less than 15 days ago, participating in the final table held at King's Casino, Rozvadov in the Czech Republic. Salas defeated Brazil's Brunno Botteon heads-up just 13 days ago.
Negative Tests, but No Travel
According to CodigoPoker, Salas has tested negative for COVID-19 and had obtained a "certificate of exemption" from the WSOP in order to participate in the event.
However, two possible routes to the United States - via Dallas and Miami - were shut off by authorities, due to Salas attending the Final Table in Rozvadov earlier this month.
"I was going to travel to Las Vegas on Saturday via Dallas," Salas told the site. "But 15 minutes before leaving for the airport I received a notification that in Dallas they did not recognize my certificate and that they would not let me in."
Salas was then instructed to change his tickets, along with those of his wife, brother and two friends, and to travel to Las Vegas via Miami However, Miami also refused to recognize the certificate leaving Salas stranded.
The father of three, is said to be "very dissatisfied" at the inconvenience, this has caused him. He will now travel this Wednesday - the original date of the heads-up match - and arrive in the United States the following day. The heads-up match will take place on Jan. 2.
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