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Research with party members offers an important clue about how to heal Brexit divisions.
By Professor Tim Bale
[ 4 min read ]
There seems little chance of getting people to agree on the big picture, but even partisans see eye-to-eye sometimes when you get down to the nitty gritty.
First published in February 2020.
Anyone wanting to understand post-Brexit Britain should make a beeline for a report published towards the end of last year by The Policy Institute at King's College London. It draws a crucial distinction between two modern phenomena.
On one hand there is affective polarisation – described in the report as "when individuals begin to segregate themselves socially and to distrust and dislike people from the opposing side, irrespective of whether they disagree on matters of policy". On the other is issue polarisation – "the difference in values and attitudes on one or more issues".
After sifting the survey evidence, the report's authors find that "people on both sides of the Brexit vote dislike the opposing side intensely even though they don't necessarily disagree with their positions on salient issues".
In other words, while there's plenty of evidence of affective polarisation, there's much less for issue polarisation. This provides at least a degree of comfort for those of us who hope the UK can somehow move on from the deeply divisive politics of the past four years.
That's not to say, of course, that moving on will be easy. And it will, in part, depend on how the nation's politicos respond in the coming years. As the Policy Institute's report notes: "voters to some extent take cues from party platforms and leaders, so polarisation among political leaders and activists can spread to the electorate."
And that's what makes the views of Britain's rank-and-file party members important. While they don't necessarily directly determine the tone and the direction their parties take, they do have an indirect and sometimes pretty immediate influence on them.
Witness, for example, how the slow growth of hard Euroscepticism within the Conservative party eventually went on to have such dramatic consequences for the nation.
Don't forget either that members also constitute the on-the-ground sales force for their parties. Because they interact on the doorstep with the public as well as with politicians, what they think, say and do about the UK's relationship with the European Union really can matter. That's especially the case as the nation decides what it wants its future relationship with Europe to look like.
Even partisans agree on some things
Over Christmas and the New Year, the Party Members Project, run out of Queen Mary University of London and Sussex University, asked the members of the Conservative, Labour, Liberal Democrat, Scottish Nationalist and Green parties (plus registered supporters of the Brexit Party) a couple of key questions about the UK/EU relationship.
The first touches on what, if you like, is the broad-brush future relationship between the UK and the EU. It shows a high degree of polarisation – and perhaps affective polarisation – between what are effectively two tribes.
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Irreconcilable viewpoints? / ESRC Party Members Project
On one side of the divide, Tory members and Brexit Party registered supporters are both overwhelmingly in favour of a more distant relationship. On the other, you have those who belong to Labour, the Lib Dems, the SNP and the Greens. They are even more overwhelmingly in favour of close alignment between the UK and the EU.
This would suggest that the country isn't about to heal its Brexit divisions any time soon. But before we descend into total despair, it's worth turning to the second question we asked. That's because it's a reminder that people – even highly partisan people – become less polarised when you ask them about specifics.
That's even true for immigration – often a subject that plays into the "culture wars" narrative. We asked whether European nationals should be treated differently from people from elsewhere in the world when it comes to post-Brexit immigration.
Finding unity wherever we can. / ESRC Party Members Project
While the two tribes are still pretty divided, there is far more overlap between parties on this second question than on the first one. Many members from the left-liberal parties are actually in agreement with Conservatives and Brexit Party supporters in wanting everyone to be treated the same. They might be said to come at the question from different viewpoints, but they still find some common ground, at least.
These findings at least give us a hint at how the UK might go about trying to heal divisions. Instead of focusing on Brexit identities and the big picture, it may be that people should move as soon as possible to talking about the myriad specifics that need sorting out. Now the UK has left the EU, the nation can best create a wider consensus on how to move forward by building on the fact that there's much less that separates people on individual issues than separates them emotionally.🔷
[This piece was originally published in The Conversation and re-published in PMP Magazine on 10 February 2020, with the authors' consent. | The authors write in a personal capacity.]
[Written by Tim Bale, Professor of Politics, Queen Mary University of London and Paul Webb, Professor of Politics, University of Sussex.]
(Cover: Pxhere.)
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The women's Hostel, partially Sponsored by University Grants Commission (UGC), New Delhi, started functioning in the Campus from the academic year 2009 - 2010. Any girl student of this college is eligible to join the hostel. The hostel is well furnished with triple seater rooms. A mess is run by the hostel authorities on dividing system. An establishment fee per semester is collected from each inmate.


It's not that the 2010 Edge was poor, flawed, or even unlikable . But beside the totally reworked model Ford just rolled out for 2011, it might as well be a Model T.
The company's popular crossover utility vehicle has been dressed up, slicked down and thoroughly doused in technology for its fifth year on the market. Twenty percent more torque from the same engine, with better fuel economy, too. A new front fascia that says "move over" in the rear view mirror more than "mom." An in-car computer that will not only let you place calls by speaking – it will read your incoming text messages to you aloud.
We spent hours flogging the 2011 in the back hills around Nashville, and while we spent the majority of it fiddling with MyFord Touch, we would be remiss to not mention that the first vehicle to get this automotive supercomputer is, well, a worthy set of wheels.
The 2011 Edge is the kind of vehicle that begs to be taken on a road trip. A total interior redesign has left everything from the seats to the steering wheel and dash feeling touchably plush and studded with technology. It's a welcome break from the hard plastics from the last generations, though performance enthusiasts might find the comfy wheel more Nerf than MOMO.
When it's not spitting out 305-horsepower at wide open throttle, the 3.7-liter V6 in the Sport edition (borrowed from the Mustang but apparently tamed along the way) purrs along with barely a whisper, and road noise seems to disappear somewhere in all the interior softness that separates you from the outside – an important factor given how heavily MyFord relies on a quiet cabin for voice commands.
Don't take that to mean Ford has literally gone soft on the Edge, though. While the suspension muffles highway potholes without complaint (even with the stiffer tuning and 22-inch wheels on the Sport edition) the Edge feels sure-footed and right at home after veering off into the curves, too. All-wheel drive made our rain-soaked trip through Tenesee twisties almost too safe feeling.
If you want noise, it does that too. An optional Sony 12-speaker stereo belts out bass low enough to rumble the door panels with the best of them, and you can tweak the sound to heart's content on the MyFord Touch screen. The same Sony upgrade also includes home-electronics-inspired capacitive touch buttons in the center stack. While they respond as readily as the real thing and look great, the lack of click still left us wondering if shifting everything to touch should really be the going trend.
The base price for the 2011 Ford Edge starts at $27,220, but loading it up with many of our favorite goodies can easily push it north of $40,000. For the road-weary traveler looking to be coddled in technology without totally losing the thrill of the open road, the Edge remains of the sharpest picks on the market for 2011.
Also check out our in-depth coverage of the MyFord Touch in-dash technology.


Father John Perich w/his Russian collectibles.
@KathyM23- That line was Gabriella T and she made beautiful, screen-printed sweaters. They were also sold on QVC UK while I was there. I got so many compliments on those sweaters. Wish I'd never gotten rid of them. You can still find some, but it's hit or miss.
That's a line I wish QVC would bring back.
I agree about George Simonton, too. He was an original, not cookie-cutter and you knew he designed his own line. Perhaps that's why both of these lines are gone.
Larry King pillow , one and done!
@MimiLouise That name is familiar. What did Linda Dano sell?
@iceberg Mario is kind of back. Martha Stewart is selling his products.
Don't forget Kathy Van Zeeland. I was a Kathy fan, but boy her handbags are horrible. I never had handbags that just completely fell apart in the closet. That did it for me, I will never buy a handbag that is not real leather.


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Professor Archibald McDonald says there must be partnership among all stakeholders in order to create a disability friendly society.
This is to ensure that Jamaica makes provisions for the disabled that are consistent with global developments.
Ensuring access to buildings, parking, and sanitary facilities by disabled persons, are crucial requirements in making any society more adaptable for disabled persons.
Pro-Vice Chancellor of the University of the West Indies (UWI), Professor Archibald McDonald says there must be partnership among the government, private sector, and academic stakeholders, in order to create a disability friendly society.
This he argues is to ensure that Jamaica makes provisions for the disabled that are consistent with global developments.
The Pro-Vice Chancellor was speaking at the recently held inaugural two-day biennial Regional Disability Studies Conference staged by the UWI's Centre for Disability Studies (CDS), at the Mona Visitors' Lodge and Conference Centre.
Professor McDonald, who is also Principal of the UWI's Mona Campus in St. Andrew, noted the "increasingly globalised nature" of the international community, which has facilitated the "crucial" transfer of knowledge and best practices on methods to protect and improve the quality of life for millions living with disabilities around the world.
"The introduction of assistive technology in classrooms, such as speech recognition software, or the use of sticky keys, has empowered many disabled students to embark on advanced education courses as they are provided with the essential tools that support their learning needs," the Pro-Vice Chancellor stated.
Additionally, he said ensuring access to buildings, parking, and sanitary facilities by disabled persons, are crucial requirements in making any society more adaptable for disabled persons.
"Our society (seems) oblivious to the international standards that have been developed to protect the quality of life for people with disabilities and, as such, their ability to prosper in society is severely hampered," he contended.
"It is, therefore, the responsibility of the government… private sector (and academic community) to begin engaging in crucial talks specially aimed at devising new policies and regulations to better provide for persons with disabilities. The introduction of public education initiatives is also important if we are keen on creating an inclusive society for all," he added.
Professor McDonald noted that Jamaica is at a "crucial turning point" that requires everyone to "show our willingness" to provide equal opportunities for all persons committed to the growth and development of Jamaica and the Caribbean.
More than 300 representatives and delegates from Jamaica and other Caribbean islands attended the two-day conference, held under the theme: 'Making Government and the Private Sector work for Persons with Disabilities'.
Participants focused and deliberated on issues related to the status of persons with disabilities across the Caribbean, with a view to developing a Charter of minimum service delivery in the public and private sectors, and assisting relevant stakeholders to fast track the disability agenda in the region.


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Listen to the new Neko Case: "Man (feat. M. Ward)"
With quick-punching snares we're introduced to the first new solo material from Neko Case in over three years. "Man" is a showcase of compositional bravado, compressing swirling guitar work by M. Ward, galloping rhythm, and absolute lyrical tenacity, all in only three and a half minutes.
While Case has shown exquisite at portraying abrasive lyrical honesty against delicate backdrops, this track really stands apart by showing off her temper in all facets of a track. This is a real treat from someone who has always been more than capable.
The single comes off of her lengthy-titled upcoming album, "The Worse Things Get, The Harder I Fight, The Harder I Fight, The More I Love You", out September 3rd via ANTI. Listen to "Man" here.

redpajama_set_name: RedPajamaCommonCrawl


Unexpected Homeschool: Back to Full Days, Finally!
Back to Full Days, Finally!
Whew, this has been a productive week! We didn't have much scheduled out of our house, however it was Amber's first week back to full days of school since November. I must say the week did test our ability to adapt lessons to Amber's ability.
As of this writing (before Friday lessons) Amber has earned 18 core hours, 11 non-core, plus 9 hours of free reading. Additionally, we still have all of Friday to earn a few more of those core hours. It's a good thing too as next week is a busy one with a lot of outside activities.
Amber started the week on Sunday with a fun trip to The Magic House, a children's museum here in St. Louis. She attended with several friends to celebrate another friend's birthday. They all left directly from church, which of course meant Amber was tachy and worn out before the fun was over, so we took her home a little early. This led to Monday being a rough start and a pretty slow day. Still, we used some of our alternate learning methods and successfully completed a full day of school.
(Left) The Magic House climbing tree. She only fits in the very top section these days. (Right) Starting her service hours for this module: baby hats for the hospital where she most often goes. Her first Cover Story lesson. The mild Steampunk theme doesn't hurt at all!
Amber started the day by listening to a dramatized audio book from in our history list instead of focusing on reading the same book. We then had oral discussions over the sections she heard. Then, for science Amber watched several videos on weather, the universe and our solar system after which again we had a discussion before Amber completed activities that went with the videos.
By late Monday afternoon Amber was feeling somewhat more together and was able to have her postponed crusades discussion with me. We have a few videos on the crusades yet to watch when time allows, but the majority of her work for this topic is now complete. Moving right along in history.
Amber did finally start her new creative writing course using Cover Story on Monday. It wasn't what she expected from the sample I showed her. (It was what I expected, lest you think the sample is not a good representation). Thankfully Amber is quite happy with the curriculum. Monday Amber watched the first video lesson and completed the first assignment in the student book. She was a little bummed that the journal was not explained in the first lesson, but when the second lesson came around she was afraid the journal was going to be boring. Again, it all worked out well and she loves the premise of the journal. I believe her exact words were, "This creative writing class is actually fun. I mean I am even enjoying it." High praise, indeed. We are going a little slower than the curriculum recommends simply because we don't have that much time in a week to do everything that every curriculum asks.
The rest of the week has been even more productive in all subjects except German. Amber did not catch up with my class yet since she only had one German lesson all week. That's okay too because it has been a week heavy in science which is something that we truly needed to work on since first semester was a near bust in science.
(Left) Being silly. Even now that she wears my size shoes she still fits in the "rocky" given to her on her first birthday.
(Right) Tired after a day of school but playing her well earned LEGO Batoman 3. And... this is the sum total of our "big" snowfall this year so far. It's been a pathetic year for us.
Amber is sailing right through the Astronomy curriculum from Real Science 4 Kids at such a speed that I had to plan out the Geology lessons on Wednesday for fear we might need them in a week or two. During a conversation on a different topic this week, Amber indicated that she very much enjoys chemistry and would like to study it again soon. Well, if she's going to ask I could at least look into it.
Our plans were to complete Astronomy and Geology this semester, then start Apologia's Physical Science if the school year was not finished yet. Amber will be moving to Apologia for 8th grade science and I already have the books. A more detailed review of the Apologia books revealed a lack of the type of chemistry Amber is interested in studying. At this point, I think we will be ordering the Real Science 4 Kids Chemistry books to start once Geology is complete. I *really* wanted a head start on Physical Science, but I'd rather hold Amber's interest than meet a mental schedule.
Amber reiterated this week how she missed her school lessons over the extended Christmas / birthday break. We will have to take a good look at scheduling next year because December activities make school almost impossible with Amber's dysautonomia. I had been planning to give Amber an even longer official Christmas break in 2015; but in reality it was a long break this season as she did very little school after Thanksgiving in 2014, even if I was striving for more.
For some fun this week Amber and I have started playing the LEGO Batman 3 video game. We knew almost nothing about these characters, except what almost everyone of my generation knows about Batman, Robin, and Wonder Woman. We are actually enjoying the game, even if the story line and characters confuse us (Martian Manhunter? That's not a character you'd assume to be a good guy).
Biscotti being cuddly.. see he really can be. Then Biscotti trying to look small. He is not. Also, Amber working on Astronomy. This was a common sight this week. Yay for science.
We also started watching Sons of Liberty and have made it about halfway through. We heard in advance from online sources and my mother that it was not terribly accurate, while still fairly entertaining. I have to agree. Amber was interested despite the historical inaccuracies, but I (not so secretly) think that might be almost entirely due to Ben Barnes (aka Samuel Adams). Once Amber found out he was in Sons of Liberty, as well as the upcoming Seventh Son, she couldn't wait to watch both. To be fair, Amber loves the book series the Seventh Son is based on and planned to see the movie before she knew the cast. We did have to re-watch Prince Caspian last weekend though. Teenagers.
This weekend I'm going to start sewing on Amber's costumes for the Narnia play. I have great hopes for completing a good deal of the sewing, however realistically I know I'll be lucky to finish even one piece. Wish me luck!
Sounds like you're required to count hours for school. I am thankful that we just have to count days here. I think it would be harder to do hours! Have you done a review for Real Science 4 Kids? I was looking at it for Sam for next year. Physics. It's a little pricey to get the whole package and I'm on the search for an experiment kit that goes with it as well. I don't like hunting down supplies!
I haven't reviewed it yet. I'll tell you that it is very simple compared to Apologia for this level. We are doing a lot of video supplementing and using other resources we have at home as extra reading. However the experiments are much better than what we had been using. Home Science tools has a combo experiment kit for the biology, chemistry, and physics. It lists which items go with which level. You could just get the physics items.
Looks like a really productive week. I am glad you were able to do some resting up before your very busy upcoming week.
I'm very glad to see that Amber had a good week! I love the Pic of her holding Biscotti! I hope you all have a great weekend and next week too!
It is good to see her having a productive week. Crash Course now has a series on Astronomy with Phil Plait. There are 4 episodes so far with more being released every Thursday.
I am having deja vu of having already shared this with you so if I did apologies.
We use cover story and my guys LOVE it. I have seen his influence even when they are talking to me, as they now choose much longer and descriptive words. I have to laugh though because they don't always get the right words at the right time!! It has been a huge success in our household though!
You are both doing a fabulous, fabulous job!


RICHLAND, Wash. - The Hanford Falcons baseball team hosted a tribute on Friday night for a student who passed away last year.
Dmetri Kennedy-Woody was with three other friends on Memorial Day when they jumped off a bridge into the Yakima River. Kennedy-Woody never resurfaced and his body was found almost a week later.
Kenned-Woody was just days away from graduating from Hanford High. He was a member of both the football and baseball teams.
On Friday, the baseball team and Kennedy-Woody's parents wanted to honor him. The baseball team dedicated their doubleheader against the Richland Bombers to Kennedy-Woody.
In between the two games, the tribute kicked off with Mark Allen from Allen Water Rescue giving the audience tips on water safety. After that, Kennedy-Woody's parents presented a preview of a plaque that will be placed on the side of the press box at the baseball field. The ceremony ended with a moment of silence for Kennedy-Woody.
Kennedy-Woody's mother said the plaque should be finished in a few weeks.


I love the intersections in my studio. The corner of a still life painting abuts the flower power fabric background of the still life table, and both adjoin the little drawing of a lotus that hangs on the side of the book cabinet just because.
There are all these natural abstractions lying about. Like the parts of the unfinished paintings that wait in the queue.


Is Merch By Amazon Preparing For A UK Launch?
In this week's Merch By Amazon update, there's really only one story worth talking about: Rumours of a UK launch.
Since it's inception, Merch By Amazon has been limited to Amazon.com – so you cannot find or purchase any Merch Shirts on Amazon.co.uk… or the other international Amazon sites. The principle problem would seem to be Amazon's ability to produce the T-Shirts within 'Prime Eligible' limits.
There has been no official word from Amazon, but it seems clear Amazon is at least testing the Merch platform in the UK, judging by this thread in the official forums.
A Seller asks if his Merch UK royalties will be mixed with his Merch USA royalties – which implies Amazon has been testing the UK platform with a limited number of sellers (presumably top-tier sellers based in the UK – though this is purely speculation on my part).
Other sellers have reported spotting Merch-style listings on Amazon.co.uk – which would corroborate the story that Amazon is already testing a Merch UK soft-launch.
Merch by Amazon may periodically test new markets or products. These beta programs are closed to the public and we cannot provide additional information.
…so no solid info yet.
But this would certainly imply Merch UK could be around the corner…and we could also be seeing new Merch products anytime now (who knows – but winter is around the corner).
When Merch UK does launch (which does seem certain – the only question being when?) – it remains to be seen if all existing Merch designs will follow over to Amazon.co.uk automatically. Perhaps we will get an 'enable for UK' button or some equivalent. Either way, the potential for increased earnings will be an exciting prospect for many Merch By Amazon creators (Especially those of us based in the UK!).


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La chiesa di San Saturnino di Usolvisi è una chiesa campestre situata nella Sardegna centro-settentrionale, in Goceano in territorio di Bultei e appartenente alla parrocchia di Benetutti.

Costruita nel XI secolo sul crollo di un nuraghe, di cui ancora si legge la conformazione quadrilobata, si trova nei pressi delle sponde del fiume Tirso nell'omonima piana.

L'edificio in trachite rossa presenta una navata unica chiusa da abside orientata a est, copertura con capriate lignee e illuminazione naturale garantita da cinque strette monofore (due per lato e una all'abside). Sul prospetto opposto all'abside, tra due imponenti paraste d'angolo, si trova l'ingresso principale architravato sormontato da arco di scarico a tutto sesto. Un secondo ingresso, nel prospetto secondario a sud, con le medesime fatture dell'ingresso principale, si apre sull'abside che ospita l'altare di recente fattura. Un campanile a vela, recentemente ricostruito, (originariamente con arco a tutto sesto) corona l'abside.

Internamente la chiesa si presenta spoglia, con muratura a vista priva di intonaci o decorazioni. Sono presenti un altare e un tabernacolo in trachite rossa realizzati in occasione degli ultimi interventi di recupero.

I primi documenti sulla chiesa risalgono al 1164, quando Atone, vescovo di Castro dona alla congregazione monastica dei Camaldolesi le chiese di San Saturnino di Usolvisi, di Santa Maria di Anela e di San Giorgio di Aneleto.

Voci correlate
Diocesi di Ozieri   -   https://www.diocesiozieri.org/ladiocesi

Diocesi di Castro

Bibliografia
Dionigi Scano, Storia dell'arte in Sardegna dal XI al XIV secolo, Cagliari-Sassari, Montorsi, 1907, p. 336;
Raffaello Delogu, L'architettura del medioevo in Sardegna, Roma, La Libreria dello Stato, 1953, p. 146;
Ginevra Zanetti, I Camaldolesi in Sardegna, Cagliari, Fossataro, 1974, pp. 125–129;
Aldo Sari, Una chiesa romanica del Goceano: il San Saturnino di Usolvisi, in Sesuja, I, 1985, pp. 121–127;
R. Coroneo, Architettura romanica dalla metà del Mille al primo '300, collana "Storia dell'arte in Sardegna", Nuoro, Ilisso, 1993, sch. 49;
A. Fenu, Bultei e il suo territorio, Nuoro, Solinas, 2005;
Pasquale Tola (a cura di),  Historiae patriae monumenta, vol X Codice Diplomatico di Sardegna, Augustae taurinorum e regio typographeo, Torino 1861 p.226

Saturnino, San
Chiese di Bultei
Chiese della provincia di Sassari

redpajama_set_name: RedPajamaWikipedia


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Why First is Far Less Important Than Best
fortnite live stream
Following Marshmello's 'live' performance in Fortnite which was seen by 10 million simultaneous gamers, there has been the inevitable chorus of 'but 2nd life did this more than a decade ago'. As I referenced in my blog post over the weekend "In game live experiences like this are nothing new…". The big deal with the Fortnite Marshmello gig was not whatwas done but how it was done.
It combined integrated merchandise (Marshmello dances and skins), a global shared experience that was also personal (only 50 gamers per game) and unique gameplay (gamers floated up into the sky). But perhaps smartest of all, this was not an event for Marshmello fans in the way that previous virtual concerts have been. This was a Fortnite event sound-tracked by Marshmello. Players were there because it was a Fortnite event. Marshmello though had instant credibility because he was part of the Fortnite experience (and of course being masked is a perfect brand fit). So instead of playing to an audience of existing fans Marshmello was handed, on a plate, millions of new fans in an instant, who they felt like they were part of something. (Wait for a major surge in streams of 'Happier'). These are the reasons the Fortnite Marshemello event was so important, not simply because it was a virtual gig. This is what innovation looks like when executed well.
Execution is everything in innovation. The history of technology is defined by first movers that created a category but failed to go the distance, with an early follower learning the lessons from the first mover and then executing with market winning implementation.
The hard reality is that first movers bleed out on the cutting edge of invention, early followers prosper on the wave of innovation.


Electrowetting displays were first reported in 1981, several approaches were examined. However, ADT's "Droplet- Driven-Displays" technology is the only bistable one which makes them very attractive for energy-saving systems. That means that the power supply can completely shut off after changing the content and it will keep its information for years. More features that make the ADT approach very unique are paper like white appearance (even in the powerless OFFstate) and the capability for backlighting (most of the other e-paper technologies like electrophoretics can not be backlighted). Further achievements are a white state reflectance of about 70% resulting in sunlight readability and a pixel size in the range from 0.3mm to 10mm. Summarizing, ADT's electrowetting technology is highly suitable for lowest power (means eco-friendly or "green") displays.


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mirangwonne@gmail.com
© 2013 by Mirang Wonne. All rights reserved.
by Heather Knight, Chronicle Staff Writer
Ask most any artist what part of nature most inspires him or her, and you're likely to hear about windswept beaches, brilliant golden sunsets, the vast redwood forest. Mirang Wonne has a different take on the great outdoors. She loves rocks. The Atherton artist creates portraits of rocks, giant copper mesh wall-hangings with rocks painted on them and groupings of copper rocks that sit on individual stands on the floor. But her most eye-catching work consists of giant wire-mesh boulders -- we're talking so big they're moved from gallery to gallery in U-Hauls.
"When I say nature, it's not a pretty, superficial meaning, with the flowers and the butterflies and the trees," she said. "It's rather a big view of nature -- the Earth and universe, the moon, the whole thing."
Elegant and well-spoken, Wonne, who declined to disclose her age, grew up in Korea and took many formal art classes. She won a scholarship to the University of the Sorbonne in Paris, where she earned her doctorate in aesthetics.
She followed her first husband to New York and worked as a designer in an upholstery factory. Her marriage dissolved after less than a year, and she became depressed. .
"That was a crucial moment for me as a person and an artist," she said. "That's when I got the idea for a rock -- so small, so miserable. . . . We are not as powerful as we think. The rock image has become like myself. It's small, lonesome, not really grouped together. That's how I felt, and ever since, it's been my motif."
For her first rock-related artwork, she painted a rock in pastels, which she now says "had no real life in it."
After she fell in love with her second husband, Won Choe, moved with him to the Bay Area and had two children, her vision of herself and rocks began to change. As she grew happier, her rocks did too. Now, she experiments with images of floating rocks and fiery rocks, grouped rocks and powerful rocks.
"I slowly became much happier and felt more confident," she said. "My work gets lighter and lighter."
It has also become more dangerous. Inside her Hunters Point studio, she keeps more than 20 kinds of toxic acid. She spontaneously splashes the acids on copper mesh so the material turns an unpredictable shade of green, blue, brown or red. She always keeps water and baking soda around just in case there's an accident.
"It's not too, too dangerous," she said.
Wonne's uncommon view of nature and her nontraditional artwork attracted the eye ofMatias Varela, executive director of the Arts Council of San Mateo County, which coordinated her current show at the Manor House Gallery in Belmont.
"She's very futuristic," Varela said. "She has a lot of vision and a lot of complicated mechanisms that are working. When I see the works, I think, 'Wow, who works in copper?' "
Her family, while supportive, doesn't have her artistic tastes, Wonne said. Her kids, Scott and Julia Choe, who attend Hillview Middle School, have decided they'll never become artists, because there's no payoff. And her husband, who works in a high-tech field, doesn't relate to her art.
"I don't really understand what he's doing, and I don't really think he understands what I'm doing," she said.
For Wonne, the rock motif reminds her of her home in Korea. She grew up in a mountainous region where she camped and hiked with her family and admired Buddha figures carved into mountainsides.
"Being Asian, nature is subconsciously a big part of your spirit," she said. "It's not just a geological element. . . . We didn't grow up with McDonald's or a mechanical anything. We grew up thinking nature is a part of us, not that we just live inside, and nature is out there."
Asian philosophy centers around nature, not for its beauty but for its virtue, she said. Ancient Asian scholars frequently painted bamboo because it never turns brown and orchids because of their subtle fragrance. Likewise, for Wonne, rocks represent solidity and concreteness.
"They're not just a natural phenomenon," she said. "They're something we can talk to and learn from."
Artist Has Soft Spot for Rocks
Mirang Wonne


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Strategies for Family Entertainment Centers to Increase Revenues
by Frank 'the Crank' Seninsky | Oct 27, 2015 | Family Entertainment Center | 0 comments
We've all heard the old adage, build it and they will come. If we're talking about Family Entertainment Centers (FEC's), that's simply not true. For a Family Entertainment Center to succeed, you have to build the 'right sized facility at the right price in the right location,' after conducting a proper feasibility study that backs up and integrates seamlessly with your business plan. And once your Family Entertainment Center is up and running, you have to pursue a strategic growth plan that includes both reinvestment and increasing repeat visitations while always working hard to attract new customers.
I see way too many facilities opening up or expanding these days without the owners/investors conducting a thorough feasibility study that looks at all of the crucial factors. These include measuring the available slice of the existing market, the earning and spending power of potential customers, the range of competition in the area and much, much more. Any time this first critical step is skipped, the chances of success are about the same as rolling the dice in a crap game. Without a detailed feasibility study you're simply fooling yourself. In my experience, most of the Family Entertainment Centers that fail do so because they didn't establish the proper revenue vs. expenses ratios that form the base of their operation.
Many industry suppliers, particularly those that offer popular attractions, are often providing advice that potential center owners/investors believe will serve as a substitute for conducting a full feasibility study. Even though the products these firms supply may be excellent, the revenue projections provided are not the same as a third party objective analysis. In fact, this type of advice is similar to the problems that led to the Financial Crisis of 2008 with rating agencies getting paid by Wall St. firms to rate those same firm's mortgage bonds. When you have an interest in selling a product, almost any facility becomes a viable one.
The profitability outlook of operating a good, sold family entertainment center remains strong, but as I said at the outset, you have to pick the right location and level of investment and you have to devise a solid plan for growth. What never ceases to amaze me is how often I encounter people who have been in the industry for even 20 or more years, many of whom want to grow their business, and yet these industry veterans continue to make rookie mistakes over and over again. These veterans need to seek out objective data and third party advice because they don't know what they don't know. Fortunately, we've seen about a third of our last year's attendees of Foundations Entertainment University (#1 ranked amusement industry educational program) coming from the ranks of industry veterans. We also have had a dozen veteran street amusement game vendors looking to better understand and reach greater game revenue potentials in the Family Entertainment Centers market.
Read more Top 60 Redemption & Merchandise Games October 2015
Through the years I've met owners/managers who have been running seemingly successful FECs for years and yet they do not pay much attention to their game data. They don't weekly track or manage their redemption games ticket or e-point payout percentages or merchandiser win percentages. Even the Family Entertainment Centers that do track that information aren't using it to improve their business. Any one of our AEM Team (Amusement Entertainment Management) can walk into a Family Entertainment Center and within just a few hours can recommend action steps that result in game revenue increases of 15%-25% or more. This involves teaching the technician and manager how to properly track their game information, make the necessary game programming and price/play adjustments, and improve the game layout.
FEC operators also don't pay much attention to the game mix. Even a rotation of one new game every three months would improve revenue because Family Entertainment Centers have to provide their customers a reason to come back. Just paying attention to a well thought out list of operating procedures could benefit so many Family Entertainment Centers.
When you drill down into who is patronizing locations, many Family Entertainment Centers are being supported by a very low number of individual customers in a particular market. That's why an accurate feasibility study is so crucial, so that you have a realistic grasp of your target audience and you can invest appropriately. You also have to analyze the average individual and family out-of-home entertainment spending on an annual basis. This is all the more crucial today when you consider how much money is going to mobile providers and the newest electronic devices. Those new family budget items have definitely cut into the money that used to get spent on more traditional entertainment like ours.
Read more Top 60 Redemption & Merchandising Games Combined & Test Games Spreadsheet Report - Dec 2015
As an example, a hypothetical FEC that grosses $1.2 million in revenues would have 100,000 customers walk through its doors, spending an average of $12 per visit. The simple formula for this is: Gross Revenue = Per Capita Spending X Attendance. But when you factor in repeat visits, you're really talking about only 35,000 unique visitors, many who come multiple times per year. So one of the most important growth strategies, beyond re-investing in your facility, is to increase the visitation rate of your core group with a few proven strategies.
For the past ten years my company has been focusing on trying to maximize our VIP loyalty programs by devising ways to encourage our small number of frequently visiting VIPs to recruit people like them who are also willing to visit frequently. We've done that in part through incentives; a 10% discount for life and additional bonus credits when they bring in and register other new customers, who, as is turns out, are most likely to be friends with people of similar consumption habits.
This is important because we have locations where 3% of the customer base are generating 20% of the total revenue! This is a great cushion to have and is the prime reason why our revenues did not slip at all during the past economic downturn. But what about the other 97% of the customer base? Obviously they are not interested in a VIP program but many can be encouraged to recruit their friends as new customers if the incentives were attractive. Every new location will generate a certain amount of traffic from people who will come once for the novelty factor or in response to a marketing effort. The goal is to convert enough of those people into repeat customers. It's really a numbers game because only a certain number of those initial visitors are going to come back after either a walk-in or a birthday party.
Read more What's possible with feasibility studies?
Family Entertainment Centers spend a lot of money trying to attract new customers but do not focus enough on increasing the frequency of visitation of their core customers. Once you attract a customer, then you have to give them real incentives to come back. That means achieving the following:
Providing a quality experience (in fact, this entire column presupposes a well managed Family Entertainment Center providing a quality entertainment experience).
Ensuring that the amount of money a person spends to have fun is fair, given the market demographics of your community.
Offer different incentives for each type of customer to register and to come back again (VIP plus bring a friend programs).
Finally, offer an incentive for that person to bring someone else with them when they return and get that new person to register.
Our hypothetical Family Entertainment Center can initially live off a 35,000 customer base, but we all know that operating costs continue to increase and the current customer base will naturally decrease. If you want to grow your profits you've got to turn that 35,000 base (100,000 annual visits) into a larger base and at the same time increase the frequency of visitation. Just a small increase in both categories can quickly add up an overall increase in total attendance. And that is without increasing average per capita spending!
There are so many factors that come into play in building and operating a profitable Family Entertainment Center. But if you start with the right location with the right amount of investment, you give yourself a fighting chance. Then, if you reinvest in your facility and you learn how to target the core customers and get them to visit more frequently, you can propel your growth instead of stagnating or losing ground after the initial novelty wears off. Unfortunately, many operators are just doing the basics or less. But it doesn't have to be that way. We can do so much with just a little bit of extra focused effort to build our businesses.
RePlay Magazine
Written By Frank 'the Crank' Seninsky
Amusement Entertainment Management


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\section{Introduction}\label{intro}
\justifying
Coronal mass ejections (CMEs) are large-scale eruptions of coronal plasma and magnetic fluxes ejected into the heliosphere. The speed of CMEs ranges from $\sim$100--3500~km~s$^{-1}$ \citep{2019SSRv..215...39L}, and  fast CMEs (e.g., speed $>$800~km~s$^{-1}$) are of great interest for their role in causing extreme space weather events \citep[e.g.,][]{kilpua2019,2018E&PP....2..112Z,2020ApJ...901...45Z}. Typically, CMEs are found to undergo three phases of dynamic evolution: (1) an initiation phase with a slow rise, (2) an impulsive phase with a fast acceleration, and (3) a propagation phase with a constant or slowly decreasing speed \citep{2001ApJ...559..452Z,2004ApJ...604..420Z,2008ApJ...673L..95T,2010ApJ...712.1410T}. During these three phases, the dominant force acting on CMEs is different \citep[e.g.,][]{2004A&A...423..717V,2015SoPh..290..903M}, i.e., the Lorentz force competing with the solar wind drag force (solar gravity can be neglected), as further explained below.

In the low corona where magnetic pressure is dominant over thermal pressure, the Lorentz force accounts for the CME initiation and initial acceleration \citep[e.g.,][]{2000JGR...10523153F}. The acceleration usually takes place within a few to tens of minutes impulsively with magnitudes varying from $\sim$200 to $\sim$7000~m~s$^{-2}$ \citep[e.g.,][]{2001ApJ...559..452Z,2004ApJ...604..420Z,2007SoPh..241...85V,2008ApJ...673L..95T}, and leads to fast CMEs associated with solar flares. Two temporal correlations, i.e., (1) between the solar flare soft X-ray flux and CME speed profile \citep[e.g.,][]{2001ApJ...559..452Z,2004ApJ...604..420Z,2004SoPh..225..355V}, and (2) between the flare hard X-ray flux and the acceleration profile of fast CMEs \citep{2008ApJ...673L..95T,2010ApJ...712.1410T,2018ApJ...868..107V,2020ApJ...897L..36G,2020ApJ...893..141Z}, have revealed a close flare-CME relationship. Flares and CMEs are coupled through the action of magnetic reconnection \citep[e.g.,][]{2020ApJ...897L..36G}. On the one hand, magnetic reconnection can result in a very large amount of energy release, which contributes to the plasma heating and the acceleration of solar energetic particles in flares. On the other hand, reconnection plays a significant role in the CME acceleration, which is achieved via reducing the tension force owing to the overlying magnetic loops and providing additional magnetic (especially poloidal) flux to the original CME structure \citep{2000JGR...105.2375L,2004ApJ...602..422L,2008AnGeo..26.3089V}.

At larger distances where coronal magnetic field decreases significantly and the solar wind has reached a faster speed, CMEs primarily experience an aerodynamic drag force due to interaction with the solar wind. This aerodynamic drag force accelerates slow CMEs but decelerates fast CMEs \citep[e.g.,][]{2000GeoRL..27..145G,2001SoPh..202..173V,2007SoPh..241...85V,2007A&A...472..937V,2004SoPh..221..135C,2012GeoRL..3919107S,2015ApJ...809..158S}. In this paper, the term slow (fast) refers to the condition where a CME travels slower (faster) than the solar wind which typically has a speed of $\sim$400--500~km~s$^{-1}$. Previous studies have shown that most fast CMEs reach their peak speed in the low to middle corona ($<$10~$R_\odot$) \citep[e.g.,][]{2001ApJ...559..452Z,2004ApJ...604..420Z,2007SoPh..241...85V,2010ApJ...712.1410T,2011ApJ...738..191B,2013ApJ...773..129S}. In this paper, we present an event for which the acceleration of a moderately fast CME clearly remains positive for around five hours in the high corona, and then study the mechanism acting on the continuous acceleration of the CME.

The CME speed in previous studies is usually derived by the height-time measurements in coronagraphic images where the height is located at the CME front (leading edge). However, since CMEs are known to have substantial expansion \citep[e.g.,][]{1993JGR....98.7621F,2010A&A...522A.100P,2017ApJ...848...75L,2020SoPh..295..107B}, the speed of the CME front along the propagation direction is the sum of the bulk speed indicative of the propagation of the CME center and the expansion speed relative to the center. \citet{2020SoPh..295..107B} analyzed a sample of 475 CMEs and found that the median expansion speed can reach $\sim$200--300~km~s$^{-1}$ in the corona, which is comparable to the magnitude of the bulk speed. Therefore, investigating the role of magnetic reconnection in CME dynamics by measuring the CME front variation would inevitably incorporate the effect of CME expansion. That is to say, magnetic reconnection leading to the CME true acceleration and expansion would together contribute to the speed variation at the CME front (leading edge). Furthermore, physical processes describing how magnetic reconnection contributes to CME expansion have not been investigated in depth, especially with quantitative measurements. One interpretation proposed by \citet{2004ApJ...602..422L} is that the reconnected magnetic flux accounts for the CME rapid expansion and the plasma flowing out of the current sheet fills the CME outer shell. Readers can also refer to Section \ref{sec5} for a discussion and a sketch about the broadening of the CME outer shell through the addition of plasma and magnetic flux associated with magnetic reconnection. In addition to the expansion along the radial direction, CMEs are found to undergo lateral expansion with similar magnitude to or larger than the radial expansion in the corona \citep[e.g.,][]{2005AnGeo..23.1033S,2009SoPh..260..401M,2010A&A...522A.100P,2010ApJ...724L.188P,2013ApJ...763...43C,2018ApJ...868..107V,2020SoPh..295..107B}.

In this paper, we study a CME event that occurred on 2013 February 27. The CME undergoes a long-duration acceleration in the high corona from $\sim$10 to $>$20~$R_\odot$, even though in this height range the CME speed is found to be substantially greater than the solar wind speed. Signatures of magnetic reconnection on the solar surface are found after the CME launch, which provides us a chance to study its contribution to the CME acceleration and expansion in the high corona. Section \ref{sec2} introduces the instruments and the CME event. Section \ref{sec3} studies the CME dynamics. Section \ref{sec4} analyzes the separate contribution of magnetic reconnection. Sections \ref{sec5} and \ref{sec6} provides discussion and conclusions.

\section{Observation}\label{sec2}
\subsection{Data and Instrument}\label{sec2.1}
We use the Large Angle and Spectrometric Coronagraph \citep[LASCO,][]{1995SoPh..162..357B} on board the Solar and Heliospheric Observatory \citep[SOHO,][]{domingo95} to study the CME dynamic evolution. LASCO C2 and C3 have a field of view (FOV) of 1.5--6~$R_\odot$ and 3.7--30~$R_\odot$, respectively. We also use the Sun-Earth Connection Coronal and Heliospheric Investigation \citep[SECCHI,][]{2008SSRv..136...67H} on board the ``Ahead'' and ``Behind'' satellites of the Solar TErrestial RElations Observatory \citep[STEREO,][]{2008SSRv..136....5K}, including COR1 and COR2 coronagraphs, and the Extreme Ultraviolet Imager (EUVI). During the eruption of the CME under study, STEREO-A and STEREO-B were located at 131$^\circ$ and -139$^\circ$ longitudinally in the Heliocentric Earth Ecliptic (HEE) coordinates. In situ solar wind parameters at 1~au are taken from the OMNI/Wind database.

\subsection{Event Overview}\label{sec2.2}
The event under study originates from the west solar limb (as seen from Earth) on 2013 February 27. Figures \ref{event}(a) and (b) show the running-difference images of the CME in LASCO C2 and C3 at two different times. The three-part structure, i.e., a bright expanding loop, followed by a relatively dark cavity and a bright core \citep{1986JGR....9110951I,2006ApJ...641..590G}, is clearly observed. The faint front ahead of the CME sharp bright front (leading edge) may refer to the shock structure \citep[e.g.,][]{2003ApJ...598.1392V}, indicated by the dashed green curve in Figure \ref{event}(b). Figures \ref{event}(c)--(h) show the observations by STEREO-A/EUVI in 195~$\mathring{\rm{A}}$ and 304~$\mathring{\rm{A}}$ wavelengths. This CME is related to a filament eruption from a quiet solar region that launches at around 04:00 UT as observed by STEREO-A/EUVI 304~$\mathring{\rm{A}}$. CME signatures in white-light appear first in LASCO C2 at 04:48 UT. Post-eruption arcades in EUVI 195~$\mathring{\rm{A}}$ and two bright ribbons in EUVI 304~$\mathring{\rm{A}}$ are observed after the CME rising. Since this CME can be observed by LASCO, STEREO-A, and STEREO-B simultaneously, we use the graduated cylindrical shell (GCS) model \citep{2006ApJ...652..763T,2009SoPh..256..111T} to obtain its 3-dimensional propagation parameters. We first focus on the propagation direction, which is S12W86 according to the GCS model. It indicates that this CME is an ideal limb event to LASCO observations, and thus we are able to directly analyze the CME dynamics in LASCO FOV with minimal projection effects.

\begin{figure}[!hbt]
	\centering
	\includegraphics[width=0.8\textwidth]{EventOverview.pdf}
	\caption{\small CME eruption on 2013 February 27. (a)--(b) Running-difference images of the CME in LASCO~C2 and C3 at two different times. The yellow line indicates the position angle used for the height measurement, the black and green diamonds indicate the CME core and front, and the two green asterisks locate the two lateral points. In panel (b), the dashed green curve indicates the shock front, and the inset shows the positions of STEREO-A and STEREO-B relative to the Sun (S) and Earth (E). Panels (a) and (b) show the heliocentric distance range of 1--6~$R_\odot$ and 1--17~$R_\odot$, respectively. (c)--(h) Observations of STEREO-A/EUVI 195~$\mathring{\rm{A}}$ and 304~$\mathring{\rm{A}}$. The solid line in panel (h) refers to the position of the superposed slit.}
	\label{event}
\end{figure}

\section{CME Dynamics}\label{sec3}
\subsection{Long-Duration CME Acceleration in the High Corona}\label{sec3.1}
We carefully measure the heights of the CME front and core along the position angle of 255$^\circ$ in LASCO C2 and C3 FOV (note that S12 as derived from GCS roughly corresponds to the projected position angle of 255$^\circ$). In Figures \ref{event}(a)--(b), the yellow line indicates the selected position angle, and the green and black diamonds mark the locations of the front and core, respectively. In the following analysis, we presume that the core locates near the CME axis in LASCO FOV, and we refer to the discussion for detailed interpretations. The height-time measurements of the front and core are shown in Figure \ref{timevar}(b). Since the CME becomes increasingly fainter during its outward propagation, here we set the uncertainties in measuring the height as increasing linearly from $\pm$0.023~$R_\odot$ (i.e., plus/minus two pixels) for the initial data point in C2 image to $\pm$0.25~$R_\odot$ (i.e., plus/minus four pixels) for the final one in C3 image.

The data points are then fitted linearly (solid line) and quadratically (dashed line). The errors below are the 1$\sigma$-uncertainty from the fits. The linear fit indicates that the CME front has an average speed significantly larger than that of the core, i.e., $602 \pm89$~km~s$^{-1}$ vs. $471 \pm20$~km~s$^{-1}$. This suggests that the CME expands radially with an average expansion speed of $131\pm 91$~km~s$^{-1}$. The quadratic fit shows that the front speed at 20~$R_\odot$ is $735 \pm26$~km~s$^{-1}$ and greater than the linearly fitted speed, and shows that the front has a positive acceleration of $a=14.0 \pm 1.0$~m~s$^{-2}$. These results are consistent with those measured by the Coordinated Data Analysis Workshop (CDAW) CME catalog, but the magnitudes are slightly smaller than those in the catalog because the catalog measures the relatively faint front of the shock structure. As for the core, the quadratic-fit speed is similar to the linear-fit speed, i.e., $507 \pm20$~km~s$^{-1}$ vs. $471 \pm20$~km~s$^{-1}$, associated with a smaller acceleration of $a=2.5 \pm 0.6$~m~s$^{-2}$.
\begin{figure}[!hbt]
	\centering
	\includegraphics[width=\textwidth]{Time_Var.pdf}
	\caption{\small (a) Base-difference image of the slit in STEREO-A/EUVI 304~$\mathring{\rm{A}}$. Separation of the two ribbons are indicated by the dashed red lines. Vertical dashed line marks the first appearance time of the two ribbons. (b) Height-time measurement of the CME front (black) and core (red), associated with the results by a linear fit (solid line) and a quadratic fit (dashed line). (c) Speed-time measurement. The dashed lines indicate the speed obtained from the quadratic fit in panel (b). (d) Height-speed measurement. The vertical black line indicates the front height at 6.5~$R_\odot$, and the red one indicates the core height at the same time. The solid lines are the linear-fit results.}
	\label{timevar}
\end{figure}

We then obtain the speed-time and speed-height variations in Figures \ref{timevar}(c) and (d), respectively. The speed at each time step is derived by a linear fit to three successive height-time measurements, and thus there are no speed data points for the first and final time steps. The dashed lines in Figure \ref{timevar}(c) show the speed derived by the quadratic fit to the height-time measurements, which indicate a linearly increased front speed and a constant core speed. It is also found that the front and the core experience two propagation phases, i.e., an impulsive acceleration (Phase-I) followed by a constant-speed propagation for the core and a smooth acceleration for the front (Phase-II). Based on the change of the CME front speed, the two phases are separated by the time at $\sim$06:50 UT and the height of $\sim$6.5~$R_\odot$, which are indicated by the vertical dashed black line in Figures \ref{timevar}(c) and \ref{timevar}(d). Vertical dashed red line in Figure \ref{timevar}(d) indicates the height of the core at 06:50 UT. The speed-time and speed-height data points in the two phases are then linearly fitted, and shown by the solid lines in Figure \ref{timevar}(d). In Phase I, $a=59.1 \pm 3.7$~m~s$^{-2}$ for the front, and $a=65.2 \pm11.4$~m~s$^{-2}$ for the core. The acceleration magnitudes are the same for both the core and the front. In Phase II, $a=10.1 \pm4.7$~m~s$^{-2}$ for the front, much higher than $a=1.0 \pm 0.7$~m~s$^{-2}$ for the core, indicating that in this height range, the CME front continues accelerating while its core can be approximated as propagating with a constant speed.

We focus on Phase-II, and emphasize here again that this long-duration acceleration is seen albeit the speed of the front at the start of Phase II is $\sim$600~km~s$^{-1}$ and larger than the expected solar wind speed at this height of 6.5~$R_\odot$ (see Section \ref{sec4} for the solar wind speed estimation). The acceleration of the CME front here lasts for nearly five hours as the CME propagates in the high corona. To the best of our knowledge, this is the first reported instance of a CME that continues to accelerate in the high corona, and even to $>$20~$R_\odot$, though it is already faster than the solar wind. Although the acceleration is not as large as compared to that in Phase-I, the long acceleration duration leads to: (1) the front speed increases by $\sim$170~km~s$^{-1}$ as the CME propagates in the high corona, and (2) the ``final'' speed reaches 700~km~s$^{-1}$ and above. Furthermore, the comparison between the acceleration of the front and core indicates that the apparent acceleration in observations of the CME front in Phase-II is primarily caused by a radial expansion with an acceleration of $a_{meas} = 9.1 \pm 4.8$~m~s$^{-2}$. If not for this expansion, the core would accelerate at the same rate due to the frozen-in conditions in the CME plasma.

Looking at the uncertainties in the CME speed, the finding about the continuous acceleration of the CME in the high corona may be questioned. To confirm that the main result holds, we perform the following calculations. Since the uncertainties come from the height measurement in coronagraphs, we obtain the acceleration by quadratically fitting the height-time measurements for the CME starting from larger distances, e.g., 15 and 20~$R_\odot$. These fitted acceleration is still around 10~m~s$^{-2}$. Furthermore, since the CME front becomes fainter as it propagates outward while the true leading edge might not be discernible, the height of the located front in coronagraphs may be lower than the true one. These two points would further support that the continuous acceleration of the CME front is true in the high corona. In addition, the CME front is too faint to be distinguished above 25~$R_\odot$ which may bring even larger uncertainties, and thus it is still unclear whether this CME has reached its final speed at this height.

\subsection{CME Lateral Expansion}
We turn our attention to the magnitude of the CME lateral expansion which should occur jointly with the radial expansion. The CME lateral width is calculated as the length of the line connecting the two asterisks as shown in Figures \ref{event}(a) and (b). The two asterisks at each time step mark the outermost locations of both CME side-edges. Figure \ref{width}(a) shows the variations of the lateral length associated with the asterisks at different times (varying with colors) in X-Y plane, where the origin indicates the center of the Sun. The solid black line indicates the position angle of $255^\circ$, which is found to be approximately perpendicular to those lateral lines. The two dashed curves correspond to the quadratic fit to the upper and lower sets of asterisks. A linear fit to half of the lateral length shows that the CME lateral expansion at one edge side has an average speed of $260 \ (\pm 17)$~km~s$^{-1}$, while a quadratic fit reveals that the acceleration of the expansion at one side is $14.7 \ (\pm 2.3)$~m~s$^{-2}$. These indicate that the CME has a stronger lateral expansion compared to the radial expansion, and such a positive acceleration confirms that the lateral expansion occurs jointly with the radial one.

\begin{figure}[!hbt]
	\centering
	\includegraphics[width=\textwidth]{Width_Change.pdf}
	\caption{\small (a) Variation of the CME lateral width at different times in X-Y plane. The black solid line indicates the position angle of 255$^\circ$, and the two curves show the quadratic fit to the X-Y data points. (b) Variation of the CME angular width (black) and the aspect ratio (red).}
	\label{width}
\end{figure}

Figure \ref{width}(b) shows the variation of the angular width ($\omega$) which is the total width between the two asterisks. It is found that $\omega$ increases by $\sim$10$^\circ$ in Phase-II, to reach $\sim$60$^\circ$ at $\sim$20~$R_\odot$. Again, the CME might continue to expand laterally beyond 20~$R_\odot$. The aspect ratio, i.e., the ratio of half of the lateral length to the radial length from the core to the front, is shown in Figure \ref{width}(b). The aspect ratio increases impulsively at first, and then keeps approximately constant at 1.5--1.6. A ratio greater than unity indicates that the cross-section of the CME is an ellipse with the major axis in the lateral direction and the minor axis in the radial direction. The aspect ratio $>1$ is consistent with the above results that the speed and acceleration in the lateral direction are larger than those in the radial direction.

\subsection{Magnetic Reconnection Associated with the CME Eruption}\label{sec-rec}
Signatures of magnetic reconnection on the solar surface are visible after the CME eruption. Two ribbons start brightening up at around 05:00 UT in STEREO-A/EUVI 304~$\mathring{\rm{A}}$ images, associated with a post-eruption arcade in 195~$\mathring{\rm{A}}$ images, as shown in Figures \ref{event}(e) and (h), respectively. The two ribbons separate as the eruption proceeds, shown by the stack plot of a virtual slit (Figure \ref{event}(h)) across the ribbons (with solar rotation corrected) in Figure \ref{timevar}(a). Ribbon separation acts as an indicator for the ongoing magnetic reconnection processes \citep[e.g.,][]{2002A&ARv..10..313P}. In Figure \ref{timevar}(a), vertical dashed line marks the first appearance time of the two ribbons. Dashed red lines locate the ribbon fronts which are visually identified, and the separation speed can be deduced by the associated slope. The separation of the ribbons is fast at first before 06:00--07:00 UT, which is consistent with the CME impulsive acceleration in Phase-I. The separation then slows down but lasts for around five hours to around 12:00 UT for which the signature is clearer as seen by the front of the ribbon R2, and its duration is comparable to the CME acceleration period in Phase-II. Since magnetic reconnection plays a significant role in the CME eruption processes, the separation motion of the two ribbons indicates that for the current event reconnection processes contribute to the CME dynamic evolution, impulsively from the low to middle corona, and continuously for several hours in the high corona. We come back to the consequence of this reconnection in the discussion.

\section{Contribution of Magnetic Reconnection to CME Dynamics}\label{sec4}
As presented in Section \ref{sec3.1}, the apparent acceleration in observations of the CME front is related to the CME expansion. However, as fast CMEs may experience deceleration due to the solar wind drag, a true CME acceleration is required to compensate for the effect of the drag and be present for the CME not to decelerate. Consequently, magnetic reconnection simultaneously contributes to both the true acceleration and the apparent acceleration (related to the expansion). The true acceleration for our event equals to the magnitude of the deceleration caused by the drag. We then use a drag-based model \citep[see e.g.,][]{1996JGR...101.4855C,2004SoPh..221..135C,2007A&A...472..937V,2012GeoRL..3919107S} to estimate the magnitude of the drag effect, which is expressed by
\begin{equation}\label{dragm}
	a_{drag}=\frac{F_{drag}}{m_{CME}}=-\frac{C_D A_{CME} n_p m_p }{2 m_{CME}}(V_{CME}-V_{SW})|V_{CME}-V_{SW}|
\end{equation}
and depends on the CME and solar wind characteristics. $C_D$ is the dimensionless drag coefficient and here we use a hybrid viscosity model for $C_D$ as presented by \citet{2012GeoRL..3919107S}. $A_{CME}$ is the CME cross-sectional area, and $A_{CME}\sim \pi R_{CME}^2$ where $R_{CME}$ approximately equals to half of the CME lateral length. $m_p$ and $m_{CME}$ are the proton and CME mass, respectively. In this paper, $m_{CME}$ is measured when the CME front is at the height of $\sim$10~$R_\odot$ in the C3 calibrated image by the solar software (SSW) program of CME$\_$MASS.pro, and the value is around $1.2\times 10^{15}$~g. One can also refer to \citet{2000ApJ...534..456V} for details about the mass measurement procedure. $V_{CME}$ is the CME speed, obtained by using the CME front speed as shown in Figure \ref{timevar}(d). $n_p$ is the solar wind proton number density, and $V_{SW}$ is the solar wind speed. In this paper, we use an 1-dimensional magnetohydrodynamic (MHD) numerical simulation \citep{1997JGR...10214661H} to estimate the solar wind parameters which are dependent on the heliocentric distance. The simulations are adjusted to ensure the simulated results at 1~au distance are as close as possible to the in situ observations obtained from OMNI/Wind database. Figures \ref{drag}(a)--(c) show the evolution of the simulated speed, proton number density, and temperature of the solar wind, while the in situ measurements are marked by the red asterisks. We note that panel (a) further confirms that the CME is faster than the solar wind in the corona, e.g., the solar wind speed is around 200--300~km~s$^{-1}$ in the height range of 6.5--25~$R_\odot$.
\begin{figure}[!hbt]
	\centering
	\includegraphics[width=0.9\textwidth]{drag_acc.pdf}
	\caption{\small (a)--(c) Variation of the simulated solar wind proton speed, number density and temperature with heliocentric distance, compared with the in-situ observational data at 1~au (red asterisks). Horizontal dotted line indicates the distance of 6.5~$R_\odot$. (d) $a_{drag}$ in the drag-based model by using the CME front speed based on discrete height-time measurements (filled circle) and quadratical fit to the height-time measurements (solid curve). (e) Ratio of $|a_{drag}|$ to $a_{meas}$. The two dashed curves indicate the lower and upper uncertainties. The vertical dashed lines in panels (d) and (e) indicate the height at 6.5~$R_\odot$.}
	\label{drag}
\end{figure}

The estimated $a_{drag}$ is shown in Figure \ref{drag}(d), in which the filled circles are the results obtained by using the CME front speed from the discrete height-time measurements, and the solid curve is obtained by using the front speed from the quadratic fit of the height-time measurements in Phase-II. The uncertainty of $a_{drag}$ in the figure comes from the uncertainty in measuring the CME speed. Uncertainty in the CME mass measurement is discussed later. $|a_{drag}|$ is found to decrease from $\sim$9 to $\sim$4 $\rm{m \ s^{-2}}$ during the CME propagation in the high corona. Figure \ref{drag}(e) shows the ratio of $|a_{drag}|$ (using the values of the solid curve in (d)) to $a_{meas}$ (9.1 $\rm{m \ s^{-2}}$) by the solid curve, with uncertainties shown by the two dashed curves. It is found that this ratio decreases from about 0.8 to 0.4, suggesting that in Phase-II the contribution of magnetic reconnection to the apparent acceleration related to the expansion is comparable to or even stronger than its contribution to the true acceleration that compensates the drag for the CME.

\section{Discussion}\label{sec5}
We first return to our assumption that the CME bright core corresponds to the CME center. It is traditionally suggested that the CME bright core in coronagraphic images corresponds to the prominence material. The dense prominence/filament material is suspended in the magnetic dips at the bottom of a flux rope \citep{2006ApJ...641..590G}, leading to a separation between the prominence/filament and the CME axis/center. However, this scenario might be primarily true during the CME initiation phase; when the CME propagates into the mid and outer corona, the bright core can be approximately co-located with the CME center. There are three arguments supporting this assumption. First, \citet{2017ApJ...834...86H} and \citet{2018ApJ...868..107V} presented observations showing that the inner core of the three-part coronagraph CME is not necessarily a prominence, while \citet{2018ApJ...868..107V} argued that the core is still a flux rope structure. Second, the large amount of newly added flux to the core (or initial flux rope) through magnetic reconnection during the eruption \citep[e.g.,][]{2000JGR...105.2375L,2004ApJ...602..422L} would keep the core in the center of the erupting structure. Third, the variation of the aspect ratio shown in Figure \ref{width} is relatively consistent with expectation \citep[e.g.,][]{2011ApJ...731..109S} that the CME starts with a circular cross-section. If the core is located at the back of the CME, the initial shape would already be very elliptical, which is contrary to past studies \citep[e.g.,][]{2001ApJ...562.1045K,2010A&A...522A.100P,2013ApJ...763...43C}. Note that if the core is not the center of the flux rope, this will affect the quantitative result but not the acceleration issue itself. The CME front is still seen as accelerating to large speeds but the acceleration related to expansion would only be half of what we consider here. The acceleration of the CME front would still need to be explained.

Figure \ref{sketch} shows a sketch of the CME eruption in this paper associated with a filament in the core region of the CME flux rope. This figure only shows the cross-section structures, and the shape of the cross section of the flux rope is designed to vary from circular to elliptical to be consistent with the aspect ratio variation as shown in Figure \ref{width}(b). In the left panel of the pre-eruption phase, the filament with heavy material (orange shadow) is suspended at the bottom of the initial flux rope. The flux rope then erupts associated with ongoing magnetic reconnection processes, as shown in the middle and right panels. Magnetic reconnection adds additional (poloidal) magnetic fluxes to the initial flux rope and forms the outer shells, which contributes to an additional expansion. Note that we do not show the normal expansion as the CME propagates outward, but emphasize the role of reconnection in the expansion, similar to Figure 11 in \citet{2004ApJ...602..422L}. Post-eruption arcade associated with reconnection is formed beneath the flux rope, as also seen in Figure \ref{event}(e) for the CME event. As the CME propagates upward, gravity decreases significantly, and the initial flux rope has been enveloped by a large amount of reconnected (poloidal) magnetic fluxes. The decreased gravity and the strong magnetic tension force from reconnected poloidal fluxes may keep the initial flux rope associated with the filament (which corresponds to the CME bright core in coronagraph images) near the center of the CME. In addition, this scenario does not consider the mass-unloading of the filament material, which was found to facilitate the CME radial expansion \citep{2018SoPh..293....7J}.
\begin{figure}[!hbt]
	\centering
	\includegraphics[width=\textwidth]{sketch.png}
	\caption{\small Sketch of a CME eruption associated with magnetic reconnection processes. Filament material is shown by the orange shadow, and magnetic reconnection site is marked by the red asteroid. The shape of the cross section of the flux rope is designed to vary from circular to elliptical to be consistent with the variation of the aspect ratio as found in Figure \ref{width}(b).}
	\label{sketch}
\end{figure}

We next turn our attention to the uncertainty in the CME mass measurement. Accurate measurements are important, because (1) the calculation of $a_{drag}$ is sensitive to CME mass as clearly seen in Equation \ref{dragm}, and (2) the pile-up of CME mass \citep[e.g.,][]{2005ApJ...627.1019L,2015ApJ...812...70F} may bring additional uncertainties as we set the mass as constant in the drag-based model. However, \citet{2013ApJ...768...31B} found that the mass pile-up is rare by analyzing the evolution of the deprojected CME mass, and \citet{2018SoPh..293...55H} also argued that there is no observed pile-up for CMEs in LASCO FOV by studying the variation of the electron density of the CME front. In addition, we test the influence of an $\pm15\%$ uncertainty of the measured mass on the comparison between CME expansion and acceleration. Still, we find similar contributions of reconnection to the expansion and acceleration.

\section{Conclusion}\label{sec6}
The CME on 2013 February 27, originating from a solar quiet region, is found to be associated with a continuous acceleration of its front for around five hours in the high corona and even up to 20~$R_\odot$, though its speed has already reached $\sim$700~km~s$^{-1}$, i.e., larger than the solar wind speed. This indicates that even fast CME events may not reach their ``final'' (or maximum) speed at 20~$R_\odot$. The long-duration acceleration has important consequences for some heliospheric models \citep[e.g.,][]{2003AdSpR..32..497O,2018JSWSC...8A..35P,2019A&A...626A.122S}, where the inner boundary is set at $\sim$20~$R_\odot$. We find that the long-duration apparent acceleration of the CME front is caused by the CME's own expansion, which further suggests the importance of considering expansion in studying CME dynamics and in those heliospheric models that usually assume a uniform speed distribution within the CME. For a discussion of including expansion in the initiation of CME at 20~$R_\odot$ in a heliospheric model, see \citet{2019A&A...626A.122S}. A long-duration magnetic reconnection occurs after the eruption, which contributes to the evolution of the CME dynamics. For this CME especially when it is in the high corona, magnetic reconnection results in (1) an apparent acceleration related to the expansion and (2) a true acceleration compensating the deceleration caused by the solar wind drag. Based on quantitative comparison between the CME expansion and true acceleration in the high corona, it indicates that the contribution of reconnection to the CME expansion is comparable to the contribution to the CME true acceleration in that height range. In addition, a study about the Alfv\'{e}n point locating up to 12--15~$R_\odot$ \citep{2014ApJ...787..124D}, and a recent paper showing that the Alfv\'{e}n point (or surface) even reaching as high as $\sim$19~$R_\odot$ using the observations from the Parker Solar Probe \citep{2021PhRvL.127y5101K}, support the possibility of magnetic reconnection continuously contributing to the CME dynamics from the low to high corona.

\textbf{Acknowledgement} We acknowledge the use of the data from SOHO, STEREO and OMNI/Wind. SOHO is a mission of international cooperation between ESA and NASA. Research for this work was made possible by NASA grants 80NSSC19K0831, 80NSSC20K0700, and 80NSSC20K0431.

\clearpage

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


Much of the discussion about B2C marketing revolves around e-commerce, but the strategies to increase user engagement are relevant to all industries.
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AMC Theatres vs. Alamo Drafthouse: Whose Marketing Receives Five Stars?


With 59 years of local banking under his belt, Billy Atkins is indisputably a patriarch of Clarksville's modern-era "community banking" movement.
He has retired as the legendary face of Clarksville-based Legends Bank.
But the community-focused business legacy that Atkins built goes on.
A $9 million bank from the outset, Legends now has assets of about a half-billion dollars.
Though passing off the bank's chairmanship to former Montgomery County (Mayor) Executive and bank board member Doug Weiland, Atkins will remain on the board to help ensure that the hometown feel of the financial institution — that Clarksville-centric feel that he first envisioned — will remain at the core of the bank's daily interactions with people.
Legends Bank's staff, board and associates surprised Atkins with a retirement party this week at The Belle Hollow.
Walking into the room to, at first, unknowingly greet many of his friends, family and associates, it was clear by Atkins' initial reaction that the party's organizers were able to achieve the element of surprise.
"Yes, I was surprised," Atkins said, "and as I look around this room, I've spent the past 20 years sitting in meetings with these people, and now I get to celebrate with them.
"I see so many friends and people who supported what we were successful in trying to do with a true community bank.
"I'll still be around, but I'm going to try to also do some farming and enjoy some time fishing," Atkins said.
Atkins' banking career began early while he was attending high school. He was hired at age 17 with the former Northern Bank of Tennessee.
"I remember the first day I went to work. I started as a teller at the New Providence branch along with Dotson Guinn," Atkins told The Leaf-Chronicle.
Atkins and Guinn would both ascend to highly successful professional careers, and they still take time a couple days each week to get together for breakfast, and reflect.
Atkins rose quickly in the bank from teller to branch manager, to lender, and found his niche in commercial lending.
He would spend 28 years with Northern Bank, advancing to senior vice president and becoming a member of the board of directors before the bank sold to First American National Bank in 1988.
During his time at First American, Atkins led the Clarksville market as senior vice president and senior credit officer until being named city president in 1993.
It was a time of frequent bank mergers in the financial industry, and Atkins was increasingly getting the itch to break out of the trend.
The term, "community banking," became his passion, if not his obsession.
Atkins resigned from First American in March 1998 and began laying the foundation for Legends Bank.
It happened just as he imagined it could. Legends was chartered and opened for business in November 1998 on the corner of College and North First Street in downtown Clarksville.
The bank now has eight offices in three middle Tennessee counties – Montgomery, Davidson and Williamson.
Over Legends' first 20 years, Atkins has served as organizer, president, chief executive officer, and director. In 2012, he was named chairman of the board and CEO.
To achieve a true community banking environment, Atkins knew he'd have to set the tone by becoming immersed in the life and development of Clarksville-Montgomery County.
It was a labor of love. For example, he has been a guiding force in the dramatic growth of Austin Peay State University, and in 2017, then-Gov. Bill Haslam appointed Atkins to serve on the university's inaugural Board of Trustees.
Atkins doesn't miss many APSU home football or basketball games and you might find him catching practices on the field or in the Dunn Center in his spare time.
Then, there was his work in local economic and industrial development that helped bring Clarksville to the threshold of a series of nine-digit corporate investments ranging from Hankook Tire, to Google and LG.
In 1994, Atkins served as president of the Clarksville Area Chamber of Commerce, and he has served three, six-year terms on the Industrial Development Board, having chaired the IDB four times within that period.
Among other community work, Atkins is also past president of St. Bethlehem Civitan Club, a life member of the Masonic Lodge, past chairman of Montgomery County Heart Association, past division chair and treasurer for the local United Way, and trustee of the Consumer Lending School for the Tennessee Bankers Association. He is a graduate of Leadership Clarksville's class of 1993..
Atkins and his wife, Sue, raised two daughters, Luann and Julie, and one granddaughter, Britney. He enjoys spending time with his family and two dogs, Boo Boo and Lucy.


I am looking for suggestions for a well supported graphics card, as in not Nvidia. I have an Nvidia card at the moment and it doesn't play well with Fedora resulting in a constantly broken system.
If you don't play gpu-intensive games on your Fedora machine then integrated Intel graphics works very well. By the way, open-source nouveau driver works quite well in this case too from my own experience. There were some quirks recently with 4.19 if i'm not mistaken, but it was the first time for the last several years.
Thanks @Night Romantic. I had tried the nouveau driver but then I was getting screen flicker. There is no integrated graphics card on my desktop. It's a refurbished HP Z400, NVS 310 Nvidia card.
Well, I personally have used either integrated Intel graphics or NVidia cards (end-user/gaming ones, not Quadro or NVS), so my experience is quite limited. Hope someone else can provide info you seek.
Basically it seems that in my corner of the world you can get NVidia, AMD or Matrox ones -- last one being quite expensive and I don't know anything about them. I see the same on newegg )) Then you're basically NVidia versus AMD.
From my experience, you can get reasonably good experience from not-expensive (but newer then what you have) NVidia's with nouveau.
I've heard quite a lot about AMD dropping there proprietary driver for Linux and supporting open-source one, which got much-much better during last few years. But I have no personal experience with AMD cards.
Last year I wanted to buy a new card for not-so-heavy gaming to replace my quite old NVidia one. I've looked for info, found some discussions, some complaints for both NVidia and AMD ones (on Linux I mean), found no definitive argument for AMD and decided to stick with the devil I know.
I use nouveau in Fedora for work/general usage and poprietary driver on other distro for some games.
As you've had some negative experience with NVidia card -- although I think its age is one of the culprits -- and if your available choices are AMD or NVidia, and if you're a bit adventurous -- you can research more AMD open source driver and decide if you want to try it yourself.
Since your NVS 310 Nvidia features very basic performance anyways, it shouldn't be too hard to find an AMD card that is much better for little bucks. How about the Radeon R7 240 for example? Or if you want to spend more, go for something like R7 260X or R7 370, ... all depends on your budget. You get what you pay for!
fedora workstation has 32bit non-PAE Version... ?


text:
Home Class EV
GM Plans For Eight 40 MPG Vehicles By 2017
Andre Smirnov
GM plans to produce at least eight vehicles capable of getting 40 mpg or better by 2017. This is all part of its plan to increase fuel economy and decrease emissions throughout its fleet.
Currently they've only got four vehicles that get over 40 mpg so although eight might not seem like much, that's double the current figure. The four cars that meet the mark are the 2013 Chevrolet Volt plug-in hybrid, the 2013 Chevrolet Cruze Eco, the 2013 Sonic hatchback with turbo and the 2013 Sonic sedan with turbo.
There are three models for 2014 that they can add to the list. These include the Chevrolet Cruze diesel, the Chevrolet Spark EV and the Cadillac ELR which will leave them just one shy of their goal for 2017.
United States corporate average fuel economy fleet standards will be 35.5 mpg by model year 2016 so there's pressure on all manufacturers to improve fuel efficiency sooner rather than later. The number will rise all the way up to 54.5 mpg by model year 2025 which will be a whole new hurdle for auto manufacturers to jump.
Chrysler only has two vehicles meeting the 40 mpg goal right now in the 2013 Dodge Dart Aero and the 2013 Fiat 500 electric vehicle while Ford leads the pack with 8 vehicles from the 2013 and 2014 model years making the list.
Ford's list of most fuel efficient cars includes the C-Max Hybrid, C-Max Energi plug-in hybrid, Fusion Hybrid, Fusion Energi plug-in hybrid, Lincoln MKZ Hybrid, Focus Electric, and certain Focus and Fiestas equipped with specific packages.
GM's plan also includes a goal of having 500,000 vehicles on the road by 2017 that would be at least partly powered by electricity. This would include plug-ins, pure electrics and hybrid vehicles. They've got a little way to go to hit that number as they had only 179,801 electrified vehicles on the road in 2012. This was up from 48,108 in 2011 so although the goal is a lofty one, it's one they believe they can achieve.
Nicole Wakelin fell in love with cars as a teenager when she got to go for a ride in a Ferrari. It was red and it was fast and that was all that mattered. Game over. She considers things a bit more carefully now, but still has a weakness for fast, beautiful cars. Nicole also writes for NerdApproved and GeekMom.
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Andre Smirnov is an Automotive Enthusiast, Producer, Reviewer, Videographer, Writer, Software Engineer, Husband, Father, and Friend.
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