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France and the IMF
IMF Press center
Opening Statement by Christine Lagarde to the Economic and Monetary Affairs Committee of the European Parliament
AS PREPARED FOR DELIVERY
Mr Chairman,
Honourable members of the Economic and Monetary Affairs Committee,
I am honoured to appear before your Committee for this hearing. The relationship between the European Parliament and the ECB is a cornerstone of our Monetary Union. Central bankers are independent, but not directly elected, and that can only be justified in democracies if they are held accountable by elected representatives. I therefore consider the Opinion of the European Parliament as a key step in my appointment process.
I would like to start by briefly highlighting some aspects of my professional experience which I consider particularly relevant to the tasks of the ECB President.
I have been the Managing Director of the International Monetary Fund since July 2011, and have therefore had the privilege to head an institution that is the core of the global financial stability safety net and whose governors are central banks. In that capacity, and also as Finance Minister of France, I have contributed to enhancing crisis resolution tools and financial regulation on both the European and international levels. I have also been directly involved in strengthening the Economic and Monetary Union.
What has driven me in each of these roles is a determination to serve the public interest and to deliver on the justified expectations of the people. Mindful of the profound impact the decisions of public institutions can have on many people's lives, I have always sought to focus on the fundamental issues of our time. At the IMF this also meant addressing rising inequality, tackling climate change, and promoting fairer and more inclusive growth.
But good leadership is not just about setting out priorities; it is about listening to all voices, expert advice and fostering diversity of thought. Thus at the IMF I worked closely with our economists to produce evidence-based and data-led decisions, and listened carefully to staff to develop a common and modern vision of the IMF's work. Making the IMF more inclusive, enhancing its diversity and opening it to civil society were central to this strategy.
These are the same values I would promote if confirmed as ECB President. In my remarks today, I would like to lay out more specifically the principles which would guide my approach to the role. There are three in particular.
The first is commitment to the ECB's mandate as laid down by the Treaty. The second is agility in responding to new challenges. Third, inclusiveness will remain a core tenet of my leadership and DNA.
1. Commitment and agility
How do I see these principles applying to monetary policy?
We know from decades of theory and practice that a clear mandate for monetary policy, and the central bank's commitment to pursue it, are vital for stability and welfare. Since its inception, the ECB has demonstrated a steadfast commitment to its goal.
In its early years, it achieved the remarkable feat of steering a diverse monetary union into a regime of low and stable inflation. It then faced an abrupt reversal in the economic environment after 2008, where inflation risks disappeared and were replaced by deflationary ones. Again, commitment was crucial – this time to ensure that price stability was not jeopardised by a long period of what I have termed "lowflation".
But in doing so, the ECB had to adjust to the new challenges it faced. It had to reappraise prior convictions in the light of evidence and experience, and to be innovative in its policy toolkit within the boundaries set by the law. It was exactly this agility that allowed the central bank to continue delivering in rapidly changing circumstances. Without this, the crisis would have been much worse.
In fact, the ECB estimates that the economy is almost 2% larger today thanks to the unconventional measures taken since mid-2014. Employment in the euro area has increased by over 11 million since its trough in mid-2013, as those measures boosted confidence in the economic recovery and encouraged job creation.
So, if confirmed as President, I will draw on the same sound principles: combining firm commitment to the mandate with the agility to adapt as the world around us changes .
The challenges that warrant the ECB's current policy stance have not disappeared . The euro area economy faces some near-term risks, mainly related to external factors, and inflation remains persistently below the ECB's objective. I therefore agree with the view of the Governing Council that a highly accommodative policy stance is warranted for a prolonged period of time in order to bring inflation back to "below but close to 2%".
But there are also some important questions on the horizon that monetary policy will need to address. First, though the impact of unconventional policies continues to be positive, we need to be mindful about their potential side effects and we have to take the concerns of people seriously. While remaining committed to our price-stability mandate, this requires continuous monitoring.
Second, the global environment of low inflation and low interest rates poses strategic questions for all central banks. They need to enhance their understanding of inflation dynamics; take stock of the new instruments activated to contain the crisis, including balance sheet and other unconventional policies; and reflect on whether their monetary policy frameworks are sufficiently robust to future challenges. My goal will be to ensure that the ECB, for its part, engages in such reflections with an open mind and dedication.
Third, central banks are increasingly facing new types of challenges, not least related to climate change, the disruptive impact of technological change, and the potential fragmentation of the current multilateral order. Here I see it as crucial that monetary policy is forward-looking and considers the broader context in which price stability is achieved.
Ultimately, the effectiveness of our monetary policy hinges on the resilience of the financial system. The ECB's role in financial stability has expanded significantly in response to the challenges that emerged during the crisis. It has been asked to embrace new responsibilities for macro-prudential policy and to host the new European banking supervisor.
European Banking Supervision has done an effective job in strengthening capital buffers and reducing risks on banks' balance sheets. Common Equity Tier 1 ratios have risen from 11% at the end of 2014 when European supervision began, to 14% in 2018. [1] The stock of non-performing loans of significant banks has almost halved.
A series of challenges nonetheless remain. Both banking union and capital markets union need to be completed to foster deeper private risk-sharing in the euro area and expand access to finance. Bank profitability is low. And the landscape of the financial sector is being changed by the growing role of non-banks in intermediation and technological transformation. The share of non-bank financing flows to euro area firms has risen from around 30% before the crisis to more than 50% today. Fintech firms now receive around a quarter of the financial service industry's venture and startup funding. [2]
In this environment, central banks and supervisors need to ensure the safety of the financial sector, but also to be open to the opportunities provided by change. In the case of new technologies – including digital currencies – that means being alert to risks in terms of financial stability, privacy or criminal activities, and ensuring appropriate regulation is in place to steer technology towards the public good. But it also means recognising the wider social benefits from innovation and allowing them space to develop.
2. Inclusiveness
For central banks to safely navigate these currents and crosswinds,inclusiveness is essential. To me it means two things.
The first is cooperation. Within the Eurosystem, there is a wealth of expertise we can draw on to prepare for the future and strengthen our capacity to tackle common challenges. An excellent example is the Network for Greening the Financial System launched by central banks and supervisors in 2017. [3] This will help identify and measure the financial system's exposures to climate‑related risks and foster a greener financial system.
Central banks can also play a key role in sustaining global cooperation, thereby helping to underpin the multilateral order in their fields of competence.
But central banks do not act in a vacuum. The effectiveness of monetary policy can be enhanced by appropriate national and European policies, and by the trust of the public. So I see a possibility for deeper cooperation in other policy areas, too.
Completing the Single Market remains one of the most powerful tools we have to spread new technologies and raise productivity, while also safeguarding consumers and protecting labour standards by limiting "social dumping". This holds true for the real economy – and especially in the area of services – but also the financial sector which I already touched upon. The role of the Parliament here is instrumental as the co-legislator.
Another area is fiscal policies, which need to be available to stabilise our economies through downturns and avoid overburdening monetary policy.
In my experience as Finance Minister, I have witnessed the difficulties in coordinating fiscal policies, which are inherently focused on national issues and not the euro area perspective. That is why I am convinced that we need both effective and simplified rules and a meaningful euro area fiscal instrument as a complement . In other words, we need to further institutionalise cooperation rather than trust it will emerge in crisis times.
In the short term, concluding the reform of the European Stability Mechanism, operationalising the backstop to the Single Resolution Fund and establishing a scalable Budgetary Instrument for Competitiveness and Convergence would be useful steps forward.
In combination with other reforms to the financial and payments systems, these measures would also help strengthen the international role of the euro. That would afford the euro area more of the benefits of issuing an international reserve currency, and a greater degree of strategic independence in an increasingly uncertain world.
The second dimension of inclusiveness is diversity.
As Paul Valéry rightly said in the aftermath of the war: "mettons en commun ce que nous avons de meilleur et enrichissons nous de nos différences". Simone Veil made a similar observation as President of the European Parliament. In other words, she understood that diversity was a strength. I am of the same view.
Diversity means drawing on all talents from all backgrounds, and committing absolutely to all people being treated equally – be that on the basis of gender, race or nationality. But it also means speaking and listening to as wide a range of voices as possible, and making that dialogue a central part of policymaking.
The ECB needs to be understood by the markets that transmit its policy, but it also needs to be understood by the people whom it ultimately serves. People need to know that it is their central bank, and it is making policy with their interests at heart. One of the priorities of my Presidency, if confirmed, will be to reinforce that bridge with the public.
There is much we can learn from those who see the different aspects of monetary policy in their daily lives, be they trade unions, consumer groups, NGOs or other civil society partners. Beyond the regular accountability hearings in front of this assembly, listening to their voices can only make the ECB's policymaking stronger.
Trust in the euro currently stands at 76%, the highest level ever, thanks not least to the courageous actions of the current ECB leadership. [4] Yet trust in EU institutions, including the ECB, is not at the same level. In further strengthening our bond with the public, we can build on that confidence in the euro and extend trust in the wider European project. To deliver on commitment, agility and inclusiveness, innovation and cooperation will be required in addition to accountability and communication.
I look forward to a fruitful exchange during today's hearing, not only to answer your questions, but also to hear your views.
[1] ECB (2019), Supervisory banking statistics.
[2] IMF (2019), "Fintech: The Experience So Far", Policy Paper No. 19/024.
[3] https://www.banque-france.fr/en/financial-stability/international-role/network-greening-financial-system
[4] Spring 2019 Standard Eurobarometer.
IMF Communications Department
PRESS OFFICER:
Phone: +1 202 623-7100Email: MEDIA@IMF.org
@IMFSpokesperson


I had my kids naturally too-by choice. and I had them fast too. Good thing the train didnt go thru.
and I like salt on my water melon. It was how my dad ate it-sometimes fresh cracked pepper is good too.
Fun reading your facts Nancy! LOL...natural eh? Glad it was quick!!
Thanks for the tag...I'll try and get this up soon my friend!
I sometimes salt my watermelon too! And cantelope and sometimes even apples! YUM!
You're so sweet!! Thanks for the tag! I'm going to have to think about this one....I'm pretty boring!!
Are you saying not everyone salts watermelon? That's just weird! I do! :D . . . . And suddenly, we're the majority!


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Edmonds School District » About Us » Driving Directions » High Schools (9-12)
From Everett: I-5, exit #179 (220th Street SW), turn right (W).Continue west on 220th, cross Hwy 99. Turn right (N) onto 76th Ave. W (light). Continue north on 76th. Turn left on 212th Street SW. School will be on the left.
From Seattle: I-5, exit #179 (220th Street SW), turn left (W). Continue west on 220th, cross Hwy 99. Turn right (N) onto 76th Ave. W (light). Continue north on 76th. Turn left on 212th Street SW. School will be on the left.
18218 North Road
From Everett: I-5, exit #183 (164th Street SW), turn left (E). Turn right (S) onto North Road. Continue south on North Road. Turn right (W) at school entrance.
From Seattle: I-5, exit #181B (Alderwood Mall Parkway) toward Hwy 524/196th St. Stay straight on Alderwood Mall Pkwy. Turn right (E) onto 196th Street SW/Hwy 524. Follow Hwy 524 for 1.9 miles. Turn left (N) onto North Road. Turn left (W) at school entrance.
From Everett: I-5, exit #183 (164th Street SW). Turn right (W), 164th becomes 44th Ave. W. Turn right (W) onto 168th Street SW, cross Hwy 99. Continue west on 168th, pass Beverly Elementary. School is on the left.
From Seattle: I-5, exit #181A (44th Ave. W). Turn left (N) onto 44th Ave. W. Turn left (W) onto 168th Street SW, cross Hwy 99. Continue west on 168th, pass Beverly Elementary. School is on the left.
From Everett: I-5, exit #181 (Lynnwood), follow to the right (W) onto 196th Street SW. Turn left (S) onto 44th Ave. W. Continue south on 44th. School entrance is on the left at traffic light.
From Seattle: I-5, exit #181A (44th Ave. W), turn right (S). Continue south on 44th. School entrance is on the left at traffic light.
23200 100th Ave. W
From Everett: I-5, exit #177 (NE 205th Street), turn right (W). Continue west on NE 205th (follow signs for Ferry/Hwy 104 (West)). Follow the "Y" to the right (becomes Edmonds Way). Continue on Edmonds Way, turn left at 100th Ave. W. Turn right at next signal.
From Seattle: I-5, exit #177 (Edmonds/Kingston Ferry), turn right (W). Continue west on NE 205th Street (follow signs for Ferry/Hwy 104 (West)). Follow the "Y" to the right (becomes Edmonds Way). Continue on Edmonds Way, turn left at 100th Ave. W. Turn right at next signal.

redpajama_set_name: RedPajamaCommonCrawl


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NewsSportsGolfBack spasm forces Tiger Woods to withdraw from Dubai Desert Classic
Back spasm forces Tiger Woods to withdraw from Dubai Desert Classic
Appearing for the eighth time in Dubai, where he has won twice before, Tiger Woods looked out of sorts in his opening round before deciding to pull out ahead of the second round due to a back spasm.
Tiger Woods (Reuters Photo)
Woods withdrew ahead of his second round because of a back spasm
Steinberg said the problem was not the same nerve pain that caused Woods' lengthy absence from the sport
Woods is scheduled to play the PGA Tour Genesis Open in California next
By Reuters: Former world number one Tiger Woods has pulled out of the Dubai Desert Classic ahead of his second round because of a back spasm, the European Tour said on Friday.
The American 14-times major champion, now ranked 666th after his long injury layoff due to a series of back issues, shot a miserable five-over 77 on Thursday, a round in which he failed to record a single birdie in perfect conditions. (Also read: Miserable start for Tiger Woods at Dubai Desert Classic)
Woods' agent Mark Steinberg said the player started to feel pain on Thursday night and regretted having to pull out.
"He went into a spasm in his lower back very late last night after dinner," Steinberg told reporters. "We tried to work it out last night (but) really didn't get worked out.
"We had treatment starting very early this morning for the past three, three and half hours, but can't get the back spasm to calm down. He feels terrible."
Steinberg said the problem was not the same nerve pain that caused Woods' lengthy absence from the sport.
Appearing for the eighth time in Dubai, where he has won twice before, the 41-year-old Woods looked out of sorts in his opening round as he continued his comeback at the European Tour event.
His chances of avoiding another early exit looked slim on Thursday, however, with the American appearing to be in some discomfort as he struggled to find a rhythm.
After his round, Woods said he had not felt any pain on the course but failed to even make it to the practice range on Friday, withdrawing from the event a distant 12 shots behind overnight leader Sergio Garcia.
Woods had also looked rusty when he played his first full-field PGA Tour event in 17 months a week ago after being sidelined by back pain and spine surgery, comfortably missing the cut at the Farmers Insurance Open at Torrey Pines.
The latest setback could put Woods' participation in his next scheduled event in doubt with the American due to tee off at the PGA Tour Genesis Open at the Riviera Country Club in Pacific Palisades, California on February 16.
Woods is then scheduled to play in the Honda Classic in Florida a week later.


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The All-New 2019 Subaru Crosstrek Hybrid.
Smartly powered for modern adventure.
$34,995[1]
Starting at MSRP
90MPGe[2]
Welcome to the best of both worlds. The all-new Subaru Crosstrek Hybrid gives you options without the compromises. It's the Subaru SUV you can plug in when you're running errands around town, or gas up for your long weekend road trip. And it's our best performing, most equipped, most fuel-efficient Crosstrek ever.
90 MPGe[2] – The most fuel efficient all-wheel drive plug-in hybrid in America.
The Crosstrek Hybrid uses Subaru StarDrive Technology to combine the efficiency of a plug-in electric vehicle for city commuting with the long-range capability of a SUBARU BOXER® gasoline engine for road trips without limits. The gas engine charges the electric battery, even if you can't plug in, so there's no worry about running out of electric power. The Crosstrek Hybrid provides up to 90 MPGe and up to 480 miles of total vehicle range[3], all with the confidence of Symmetrical All-Wheel Drive.
Every Day Driving
All Electric Power
Charging On The Go
All of the power. All of the efficiency. All of the confidence.
Subaru StarDrive Technology is smartly designed to give you ultimate freedom. Simply drive how you want and this advanced system automatically optimizes power, torque and fuel-efficiency to deliver not only improved acceleration, but up to 90 MPGe[2]. Take on any adventure and leave worries behind.
Everyday Driving
The system will run on a combination of electric and gas power. To maximize efficiency, the Crosstrek Hybrid automatically draws power from the hybrid battery first. The battery also recharges by harnessing kinetic energy, such as when you're coasting downhill or whenever you take your foot off the throttle. The system can also draw more power from the gas engine when you need it. It constantly works to maximize power and efficiency, so you don't have to worry about either.
All-Electric Power
The Crosstrek Hybrid will automatically drive in all-electric mode as much as possible, saving you in fuel costs by achieving up to 90 MPGe, while still delivering generous off-the-line power. And when the weather turns, only Subaru gives you the confidence of standard Symmetrical All-Wheel Drive.
When you want to maintain the battery's charge level, Battery Save Mode directs the gas engine to provide most of the power while keeping the battery level constant as much as possible. This is useful when you're taking a longer trip and plan to do more electric driving later.
The Crosstrek Hybrid battery automatically recharges while you're on the road, so you never have to worry about running out. When the battery gets low, the gas engine will automatically start up and charge it. You can also charge the battery by driving in Battery Charge Mode, which directs the gas engine to charge the battery at all times, even when the vehicle is stopped—gaining up to 33% of battery capacity in 30 minutes of driving.
Plug-in Charging
You can charge the Crosstrek Hybrid at home, using the included charger, or anywhere with a standard outlet.  When plugged in to a 120V household outlet (Level 1), the Crosstrek Hybrid can take approximately five hours to fully charge a fully depleted battery. When using a 240V outlet (Level 2), a full charge only takes approximately two hours. Most commercial charging stations use the 240V charging capability, enabling faster charge times for your Crosstrek Hybrid.
Charge Finder Charging Station Locator
With the all-new Charge Finder app, you're able to search for and identify nearby public charging stations right from inside the Crosstrek Hybrid via the in-vehicle touchscreen. This STARLINK application utilizes a nation-wide network of charging stations to provide detailed information for each station, including location, charger availability, charging rates, charger compatibility and hours of operation.
A Value That Lasts
The Crosstrek Hybrid is a value that gets better with every mile. Not just because it's a hybrid; but because it's a Subaru — 97% of Subaru vehicles sold in the last 10 years are still on the road today[4] and Subaru is Kelley Blue Book's Most Trusted Brand for four years running[5].
Better Commuting with Restricted Lane Access
The Subaru Crosstrek Hybrid is eligible for High-Occupancy Vehicle (HOV) lane access in select states[14], so your commute can be even more efficient and enjoyable.
Hybrid Incentives
As low as $28,995 after federal tax credit[15].
The Crosstrek Hybrid qualifies you for a federal tax credit of up to $4,500 after purchase. There are a variety of other tax credits, incentives, and discounts offered by state and local governments — even from energy utilities and employers. With all that plus an estimated annual gas savings of $350[16], the Crosstrek Hybrid adds up to a smart investment for years to come.
Make sure to check with a tax or financial advisor to confirm your eligibility for benefits and learn more about available rebates in your state.
VISIT AFDC.ENERGY.GOV/LAWS
Versatile Capability
Subaru Symmetrical All-Wheel Drive
The Crosstrek Hybrid has all the capability you've come to expect from a Subaru SUV, including standard Symmetrical All-Wheel Drive. The balanced design of Symmetrical All-Wheel Drive creates uniform stability and delivers an optimal distribution of power for maximum traction. It makes for improved handling, efficiency, and a quicker response to road conditions. And with 8.7 inches of ground clearance, the Crosstrek Hybrid can handle all kinds of weather and off-pavement adventure as well.
Best Performing and Most Efficient Crosstrek Ever
Our engineers designed the most efficient Crosstrek ever to be the best performing Crosstrek yet. With Subaru StarDrive Technology, the advanced hybrid drivetrain can instantly generate torque for effortless acceleration — which is more responsive and means you're always ready and nimble in traffic. And with 1,000 pounds of towing capacity, you can bring along everything you need for your latest adventure.
Integrated Roof Rails
Standard low-profile roof rails and an extensive line of Thule® racking accessories provide cargo-carrying flexibility to help bring more gear wherever life takes you.
Connected and Comfortable
Stylish, Spacious Interior
The smartly designed 2019 Crosstrek Hybrid provides a surprisingly spacious interior — with up to 100.7 cubic feet of passenger volume — in a compact SUV that remains agile and conveniently sized. Once inside, you'll find a stylish, modern interior with high-contrast navy and gray leather seats with blue stitching, standard heated front seats and an available heated steering wheel.
Flexible Cargo Area and 60/40-Split Fold-Down Rear Seats
There's always room for more fun in the Crosstrek Hybrid. A wide rear gate opening makes bigger gear easier to load. And with 60/40-split fold-down rear seats, you can fit three in the back with both rear seat-backs up, or fold a seat down for extra cargo space.
SUBARU STARLINK™ Multimedia
STARLINK Multimedia with Apple CarPlay™, Android™ Auto, and Pandora® integration[6] comes standard on the 2019 Crosstrek Hybrid. Wireless pairing and hands-free smartphone operation allow for safe and easy connection to your favorite apps and content. Access news, navigation, music, podcasts, and more through available STARLINK apps, such as iHeartRadio®, Yelp and Magellan, and SiriusXM® All Access Radio[7]. Plus, a built-in and voice-activated navigation system powered by TomTom is available, as well as an 8-inch touchscreen.
With available Wi-Fi connectivity built right into the 2019 Crosstrek Hybrid, passengers can stream and share their favorite content online[8].
Standard EyeSight® Driver Assist Technology
EyeSight has been found to reduce rear-end crashes with injuries by up to 85%[9]
EyeSight monitors traffic movement, optimizes cruise control, and warns you when you're swaying outside your lane[10]. The Pre-Collision Braking feature can even apply full braking force in emergency situations. And with Lane Keep Assist, it can even help you steer back into your lane. Another way Subaru designs vehicles with your safety in mind.
Learn more about Eyesight
SUBARU STARLINK™ Safety and Security
The latest STARLINK Safety and Security features include Advanced Automatic Collision Notification to alert first responders when an airbag deploys, and SOS Emergency Assistance to lend a hand when you encounter trouble on the road. Crosstrek Hybrid includes the STARLINK Safety and Security Plus package for 10 years. There's also the new STARLINK Concierge service for personal assistance with tasks like navigation, restaurant reservations, and scheduling service appointments.
All-Around Awareness
The 2019 Crosstrek Hybrid comes with a suite of safety technologies to help protect you and your passengers. The standard Blind-Spot Detection[12] system warns you with a visual indicator in each side mirror if it senses a vehicle in your blind spots. Standard Rear Cross-Traffic Alert[12] helps warn you of traffic approaching from the side as you are backing up, and a standard Rear-Vision Camera enhances visibility when reversing. And with standard Reverse Automatic Braking, your vehicle can even stop itself to help avoid objects behind you[13].
LED Steering Responsive Headlights and High Beam Assist
Get a clearer look around every bend with standard LED Steering Responsive Headlights, which actively track in the direction of a turn to enhance visibility.
High Beam Assist works in conjunction with EyeSight to automatically switch the headlights between the high and low settings when an oncoming vehicle is detected, enhancing safety for both you and other drivers on the road.
What is a plug-in hybrid vehicle?
A plug-in hybrid vehicle uses both an electric motor and gas-powered engine to optimize fuel efficiency and reduce vehicle emissions. The battery is large enough to allow electric-only operation, allowing the vehicle to be powered completely by its electric engine over limited range, and can be charged at home or a charging station, as well as by its gas-powered engine.
How can I charge the Crosstrek Hybrid and how do I find the closest charging station?
Owners can charge their vehicle at home or anywhere there's a 120V outlet using the included Level 1 charging cable — or at any charging station with a 240V/Level 2 charger. And with the new Charge Finder app, drivers are able to locate thousands of charging station throughout the country on their head unit.
Do I need to plug in the Hybrid before I drive it?
The Crosstrek Hybrid will run even if it's not charged, as it can be driven with gasoline by operating on the gas-powered SUBARU BOXER® engine. However, in order to maximize fuel efficiency, it's recommended to charge the vehicle.
Do I need gas in the tank?
Yes. The Crosstrek Hybrid always requires gas as the vehicle will use the gas engine for power when certain conditions are met.
What is the expected driving range?
The Crosstrek Hybrid has a total range of up to 480 miles using both the electric- and gas-powered engines together and is capable of recharging the electric battery while driving. It can travel using only the electric motor for up to 17 miles. The Crosstrek Hybrid fuel tank holds 13.2 gallons.
How long does the Crosstrek Hybrid take to charge and how can I monitor charging status?
The time it takes to fully charge the Crosstrek Hybrid varies based on the charging option. Level 1 charging occurs when using the included 120V charging cable and can take approximately five hours to fully charge. Level 2 charging happens when using a 240V charger and can fill the battery in around two hours. Charging status can be monitored remotely through the MySubaru app.
Is a charging cable included with the vehicle and where can I purchase additional chargers?
A Level 1 charging cable comes standard with the Crosstrek Hybrid. You can purchase additional Level 1 charging cables at your local authorized Subaru Crosstrek Hybrid retailer. Level 2 chargers for use at home can be purchased from a third-party provider. Level 2 charging stations should be installed by a professional licensed electrician.
What type of charger do I need to charge the Crosstrek Hybrid?
The Crosstrek Hybrid can be charged using a Level 1 (120V) or Level 2 (240V) charger. The vehicle cannot be charged using a DC charger or Tesla Supercharger.
How long is the battery designed to last?
The battery is designed to last the life of the vehicle.
Can the Crosstrek Hybrid drive off-road?
Yes. The Crosstrek Hybrid is fully capable of driving in off-road conditions with its standard Symmetrical All-Wheel Drive. Consult your Owner's Manual for more details.


There are two types of rays: UVA and UVB. UVA rays cause aging by destroying your skin's collagen and elastin while UVB rays cause burning. Your tender skin is exposed to both UVA and UVB rays year-round. While it's easy to know that your skin has been burned by the sun, the effects of UVA rays are more insidious: you won't see the damage for years!
What Kind of Sunscreen Should You Wear in the Winter?
You might suspect that there are "special" sunscreen products designed for winter use but, in fact, you don't need a "winter" sunscreen. You can continue to use a broad-spectrum product that protects against both kinds of rays. It should have a minimum of 40 SPF. Higher SPF products are more expensive but provide very little additional protection. Be sure you use enough: a dollop about the size of a quarter for each area of exposed skin is about right. Be sure to extend the sunscreen to your neck, as well as the back of your hands.
Wearing sunscreen daily will protect your skin from premature aging caused by UVA rays! Come in and see our options so you can maintain protection during the winter months!


Discernment brings deep knowingness to living a life of purpose and inner connection. Join hosts Laurie Seymour, Aparna Sain, Marianne McGuire, Sabrina Fritts and Gitanjali Hemp as they explore the potent value of learning discernment.
Develop the critical ability to discern the truth of another's words, to know when inner guidance comes from the truest part of yourself, to feel the difference between judgment and discernment and to choose well.


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HomeBOOKSSHORT STORIESTHE SECOND SHOT
THE SECOND SHOT
Short story in Betrayed anthology
All proceeds benefit organizations helping domestic violence victims.
21 Crime Thrillers by bestselling, award-winning, and critically acclaimed authors! What happens when the person you trust the most betrays you? That's the question posed in BETRAYED, a powerful collection of stories about love, violence, and survival. The characters in these pages may suffer and bleed, but they fight back. They are survivors—not victims.
In Terri Lynn Coop's Legal Aid, an overworked lawyer takes on a complex divorce case that just may get her fired … or killed. An invalid who believes his neighbor is tormenting his young wife takes matters into his own hands in Wendy Tyson's Soap. When a private investigator is hired to find someone who appears to have disappeared from the face of the earth, he questions whether some people should be found in How Not to Find Someone in Houston by Liam Sweeney. And in Elizabeth Heiter's The Second Shot a teenage girl is convicted of murdering her abusive father…but is she really guilty?
As a bonus, New York Times bestseller Allison Brennan contributed the novella Mirror, Mirror about what happens when a police detective suspects her sister is hiding a dark secret … a secret that just may get them both killed.
These stories and more fill the pages of the first anthology published by Authors on the Air. Victims become victors and – hopefully – justice is served.
BUZZ FOR BETRAYED:
"Some anthologies are too important not to be published. BETRAYED is one of them. It's about the enemy among us. In the house next to you. At the desk next to you. Maybe much closer. It's about darkness. It's about outrage. It's about hope."
– David Morrell, New York Times bestselling author of The Protector
"Moving. compelling, well-written, buy this book!"
– NTY best selling author, Lori Wilde
"I read this gritty and well-crafted collection in one sitting because I couldn't turn away. These stories, as much about courage and strength as about betrayal, explore the darkest corners of the human heart, leaving room for the transformative power of love and hope. Highly recommended."
– New York Times bestselling author Rebecca Cantrell
"Crime and punishment. Dirty deeds and comeuppance. BETRAYED is a fun and quick read from a variety of accomplished voices that's sure to delight readers looking to take a walk on life's dark side. I heartily recommend it."
– Russell Blake, NYT and WSJ best-selling author of the JET series
"An impressive collection of stories about crime survivors who've been up against the wall, survived, and triumphed over people and forces who wanted to crush them. What really moved me, aside from the great writing, was the absence of self-pity and victimhood. Each story is clear-eyed, nuanced, and captivating. Do yourself a favor and make time to read BETRAYED."
– Award-winning author Libby Fischer Hellmann
"BETRAYED reveals the truth of crime violence through well-crafted fiction. Tough, tender, and moving… BETRAYED will make you think, make you feel, and make you remember. An important read."
– Matt Coyle, author of the Anthony Award-winning Rick Cahill crime series
"Spanning from heartbreaking to heartwarming, BETRAYED shines a bright light on the beauty and strength of the human spirit. Prepare yourself for deep emotions and stories that will stay with you long after you leave the pages."
– K.J. Howe, author of THE FREEDOM BROKER


text:
Q: Will `not` media query save resources when importing css? Current I have the following set in the css:
<style>
        @import url("default.css") screen;
        @import url("light.css") screen and (prefers-color-scheme: light);
</style>

I want the default.css be loaded when
i) user is in dark mode;
ii) user did not specify any colour theme preferences; or
iii) user is visiting with a browser that does not support prefers-colour-scheme query.
should I then change the first import rule to @import url("default.css") screen not (prefers-color-scheme: light); to save resources, and will this actually save resources?
Appreciate for your answer.

A: Whether or not it will save resources is browser dependent.
From what I have observed, the media query is evaluated at runtime after actually importing the file. You can easily check in the network tabs of the debugging tools if the file is being downloaded or not. This has the most impacts client-side.
opinionated:
For the content of the files, you should make your default.css agnostic of the colouring scheme (more about common stuff) and have a light.css with only changes that apply, and then have another dark.css for the "non-light" theme.
The less you override rules, the better (for your own sake).
Although, unless you have millions of rules, the impact of overriding a rule or adding more rules is close to negligible and is/should be optimized by the browser.

redpajama_set_name: RedPajamaStackExchange


We all know that every game has its own jargon which facilitates easy communication amongst the players while the game is being played.
Breaking the bubble: The bubble refers to the least number of balls which are required to complete the bingo pattern. Whenever a player reaches bingo using the least number of balls to complete the bingo pattern, it is termed as 'breaking the bubble'.
Wild numbers: These numbers enable the players to start with multiple called numbers.
Ready/Waiting: Whenever a person is just one number away from completing the bingo pattern and win the game, he/ she are said to be ready, waiting, cased or set.
Jumping the gun: When a player shouts 'bingo' before having a valid bingo or out of eagerness of the next number to be called out, the situation is called jumping the gun.
False alarm: It is very similar to jumping the gun. Whenever a player calls bingo and has not completed the bingo pattern, it is termed as false alarm/bongo/social error. It often happens when the players mishear the called out number.
Standard: The numbers ending with the second digit of the first number called out is a standard number.
Forward/backward: This refers to the numbers which are either beginning or ending with the wild numbers.
Crying number: Once the game of bingo is wrapped up and is officially closed, the numbers which would have been drawn next are termed as crying numbers.
Wrap up: This term refers to the last game of a session.
We are located in Killeen, Copperas Cove, Georgetown and Bryan in Central Texas. To know about the Charity Bingo events happening at our Bingo halls, call us at our All Day Bingo Hotline number (254) 634-2143 which provides you with all required details about the time, directions, and types of bingo played at our Texas Charity Bingo Halls.


The BSOD issue appears to have started after users installed a recent cumulative update for Windows 10 version 1803.
Updated December 7, 2018: Microsoft has now pulled cumulative update KB4467682 completely following reports of blue and black screen errors from users. In its updated release notes, Microsoft states: "As a precaution, we have removed this optional update from Windows Update and Window Catalog to protect customers." A fix for the issue is still expected to launch with December's Patch Tuesday updates next week. The original story follows.
If you've been experiencing the dreaded Blue Screen of Death (BSOD) on your Surface Book 2 recently, you're not alone. Microsoft has confirmed that a recent cumulative update for Windows 10 version 1803 (April 2018 Update) is causing havoc for Surface Book 2 users, causing the company to put a block in place.
After installing this optional update some users may get a blue or black screen with error code, "System thread exception not handled."
As a temporary solution, Microsoft recommends using its blue screen troubleshooter. Some users have reported success with uninstalling KB4467682, but getting a BSOD in the middle of the process could wind up bricking your Windows installation. For now, Microsoft has put an upgrade block in place for Surface Book 2 users, so you shouldn't be prompted to install the KB4467682 going forward.
As for when the issue will be fixed, Microsoft is promising a resolution will be available in the December 2018 security update release. That should mean a fix will arrive on December 11 as part of Microsoft's monthly Patch Tuesday updates.


text:
News Sports HS Sports Life & Events Obituaries E-Edition Legals
Sheridan plays lights out, hands Fairfield Union first loss of the season
Lancaster Eagle-Gazette
RUSHVILLE — Fairfield Union withstood Sheridan's first punch Tuesday night in a non-conference showdown, but the Falcons couldn't withstand the Generals' body blows, especially in the second half.
Sheridan raced out to a 10-0 lead to start the game, but the Falcons, who entered the game with a 10-0 mark, came storming back and finished the first quarter on a 12-4 run and tied the score early in the second quarter.
However, Fairfield Union had no answer for the Generals and standout senior post player Faith Stinson, who scored 16 of her game-high 25 points in the second half.
Sheridan kept scoring in the final two periods and made it difficult for the Falcons to get any good looks as the Generals cruised to a convincing 61-35 victory in front of a large crowd.
"We knew they would come out and punch us in the mouth and we just had to withstand it and we did," Fairfield Union coach Ryan Montgomery said. "We are all about wearing teams down, that's what we've done each game coming into this one, but that's not the type of team you can wear down. They are just as deep as we are. In the second half, there were some things we wanted to get done and we just didn't execute well. We struggled with getting back in transition and it just kind of snowballed from there."
Stinson's 25 points was a season-high and she also finished with 12 rebounds, but the key for the Generals' offense was the fact that she made four 3-pointers, which opened up driving lanes for senior guard Bailey Beckstedt, who finished with 17 points.
"We knew this was going to be a big game and we were excited for it," Stinson said. "We knew we had to take control of the game from the start and control the pace of it. We like getting up and down the floor fast, so we wanted to make sure we kept the pace the way we wanted it.
"We have struggled, offensively, in the past couple of games, so my main goal was to be more aggressive and try to be that leader for our team."
Trailing 14-12 at the end of the first quarter, the Falcons (10-1) tied it on a layup from Hannah Rauch, who led the Falcons with 12 points, four rebounds and two assists, but the Generals (7-2) finished the half on a 10-2 run to take a 24-16 halftime lead.
Sheridan opened a 32-23 lead midway through the third quarter then proceeded to outscore the Falcons 12-2 in the final three minutes to take control of the game as the Generals led 44-25 heading into the fourth quarter.
"I thought we really played hard in the second half and we have been on our girls all year about being more aggressive and being a physical team," Sheridan coach J.D. Walters said. "We have a lot of skilled players and sometimes they get beat to loose balls and aren't as aggressive as they need to be, but tonight, I thought we won all the hustle plays in the second half.
"We were diving on the floor and had some second-chance points, and that's the way we need to play to be a good basketball team. We defended well and we rebounded well, and it allowed us to get out in transition and when we get out in transition, it's tough to stop us."
Sheridan's defense was outstanding as they limited the Falcons to just 11 of 48 shooting from the field. Offensively, the Generals connected on 20 of 43 shots and made eight 3-pointers.
Tom Wilson is a sports reporter for the Lancaster Eagle Gazette. Contact him at 740-689-5150 or via email at twilson@gannett.com for comments or story tips. Follow him on Twitter @twil2323.
© 2022 www.lancastereaglegazette.com. All rights reserved.


One of the more exciting aspects of advances in technology is what it can do in the medical field. A recent advancement is no less exciting. A new mobile app can detect anemia by just using the camera to examine the user's fingernails, all without the normally required blood test.
I'll add before I go even further how grateful I would have been for such an app a few years ago. I was diagnosed with anemia, and the doctors kept an eye on that with frequent blood tests. I was deemed okay until my blood tests and bone marrow biopsies eventually showed a worse problem: leukemia, a blood cancer. I have terrible veins, so the frequent blood tests were really difficult for me.
This medical advancement, however, means that until my condition worsened, instead of the frequent blood tests, I could have gotten by with checking my own levels with my smartphone, by using the camera to check out the color of my fingernails.
Anemia is a blood disorder that is present in 29 percent of pregnant women, 38 percent of non-pregnant women, and 43 percent of children. Its hallmark is a low hemoglobin count. This causes fatigue, heart problems, and pregnancy complications in two-billion people worldwide.
While blood samples are required of the patient, a trained phlebotomist and laboratory technicians, a clinical hematology analyzer that requires a power source, and biochemical reagents are all normally required to make that diagnosis.
Researchers from Georgia Tech and Emory University in Atlanta, Georgia, can detect anemia without the trained professionals and equipment. They relied on studies that showed anemia could be detected by analyzing a patient's pale appearance of their fingernails (pallor), palm, or tongue.
This algorithm was created by Wilburn Lam and a team at Emory. It focused on the concentration of hemoglobin detected in fingernails, using photos taken with a smartphone camera to determine the results.
The app uses the photo's metadata, adjusts for the background lighting conditions, and detects the paleness in a person's fingernail bed. In all earlier non-invasive methods to detect anemia, this technique wasn't discovered.
A study was conducted using the app on 337 people with various blood conditions, including 72 healthy people used as a control group. This app was able to better detect anemia than doctors with a traditional physical exam.
That said, this method was not as good as a blood test but was as good or better than existing FDA-approved diagnostic tools, making it good for screening but not clinical diagnosis. Yet they believe additional research could lead to it replacing blood-based testing methods.
Certainly, I could have used this app while I was being monitored, before being diagnosed with something other than chronic anemia. It could be a godsend to the two-billion people across the globe that have this disease.
What do you think of using a mobile app for detecting or monitoring diseases such as anemia? Would you be able to trust the results? Drop your opinions and thoughts into the comments below.
Image Credit: Wilbur A. Lam et al.
For some of us, this is nothing new. I have a number of friends who are naturopaths who have been doing this for YEARS. Same with iridology – they can look at your eyes as an aid in diagnosis of problems.


text:
Anderson Hays Cooper Vanderbilt (Nueva York, 3 de junio de 1967) es un periodista, escritor y presentador estadounidense, ganador del premio Emmy, otorgado por su destacado reportaje Haiti in Ruins. Es presentador de noticias del programa Anderson Cooper 360°, en CNN, así como presentador del talk show sindicado, Anderson Live.

Biografía
Cooper nació el 3 de junio de 1967 en la ciudad de Nueva York. Era el hijo menor del escritor Wyatt Emory Cooper y de la artista, diseñadora, escritora y heredera Gloria Vanderbilt, nieta de Cornelius Vanderbilt II procedente de la distinguida familia Vanderbilt de Nueva York. Su ascendencia es principalmente inglesa, escocesa, irlandesa, galesa, neerlandesa y chilena.

Desde temprana edad estuvo expuesto a los medios de comunicación y cuando era bebé fue fotografiado por Diane Arbus para la revista de moda Harper's Bazaar. El 17 de septiembre de 1970, a la edad de tres años fue invitado junto con su madre al programa televisivo The Tonight Show. Durante 1977 a 1980, modeló en la agencia Ford Models para las casas de moda Ralph Lauren, Calvin Klein y Macy's.

Su padre sufrió una serie de infartos, y falleció el 5 de enero de 1978 a la edad de 50 años, mientras se le practicaba una cirugía de corazón abierto. Esta situación afectó al joven Cooper enormemente y en retrospectiva declaró: «Creo que soy muy parecido a mi padre en muchas formas, incluyendo que somos muy parecidos físicamente y que tenemos un sentido del humor muy similar y sentimos pasión por relatar historias». Asimismo, consideró que el libro de su padre titulado Families «[...] es un tipo de guía sobre [...] como hubiese querido que viva la vida y las decisiones que hubiese querido que haga, y me siento muy conectado a él».

Después de graduarse del colegio Dalton School a la edad de 17, viajó a África austral en un camión del ejército inglés de trece toneladas de peso, y durante la travesía contrajo malaria, por lo que fue hospitalizado en Kenia. Más tarde, Cooper escribió sobre su experiencia, «África es un lugar para olvidar y ser olvidado».

Carter Vanderbilt Cooper, su hermano mayor, se suicidó el 22 de julio de 1988, a la edad de 23 años, arrojándose desde la terraza del decimocuarto piso del apartamento de la familia Vanderbilt en Nueva York. Posteriormente, Gloria Vanderbilt escribió sobre la muerte de su hijo en el libro A Mother's Story, donde expresó que «[...] el suicidio fue ocasionado por un episodio de psicosis inducido por una alergia hacia un medicamento contra el asma conocido como salbutamol». El suicidio de Carter aparentemente fue la causa de que Anderson decidiese convertirse en periodista.

En un programa de Oprah Winfrey, mientras promovía su libro, Dispatches from the Edge: A Memoir of War, Disasters, and Survival, indicó que sufrió de dislexia en su niñez, y volvió a confirmarlo en el programa The Tonight Show dirigido por el también disléxico Jay Leno, el 1 de agosto de 2007.

Educación
Después de graduarse del colegio Dalton School a la edad de 17, viajó a África austral en un camión del ejército inglés de 13 toneladas de peso, y durante la travesía contrajo malaria, y fue hospitalizado en Kenia. Al relatar su experiencia, Cooper escribió: «África es un lugar para olvidar y ser olvidado».

Asistió a la Universidad Yale, donde residió en el Trumbull College, y se unió a la  Manuscript Society. Se graduó en Ciencias políticas en 1989.

Trayectoria
Durante su estancia en la universidad, Cooper pasó dos veranos como pasante en los cuarteles generales de la Agencia Central de Inteligencia, ubicados en Langley, Virginia, en un programa para estudiantes interesados en trabajos de inteligencia. A pesar de que no tiene educación formal sobre periodismo, optó por seguir esa carrera en lugar de permanecer en la CIA, al término de sus estudios.

Después de su primer trabajo como corresponsal en la década de los noventa, se tomó un descanso y vivió en Vietnam durante un año, tiempo durante el cual estudió el idioma vietnamita en la Vietnam National University, Hanói.

ABC
En 1995, Cooper se convirtió en corresponsal de ABC News, y el 21 de septiembre de 1999 asumió la posición de co-presentador del programa World News Now. En 2000, aceptó el trabajo como anfitrión del reality show The Mole. En 2007 fue presentador temporal del programa Live! with Kelly, donde ocupó el lugar de Regis Philbin quien se ausentó debido a una operación del corazón.

CBS
En 2007 Cooper fue corresponsal para el programa 60 Minutes de CBS News, al mismo tiempo que se desempeñaba como corresponsal en CNN.

Vida privada
Cooper tiene dos medio hermanos mayores, fruto del matrimonio de diez años de su madre con el director de orquesta Leopold Stokowski, llamados Leopold Stokowski (nacido en 1950) y Christopher Stokowski (nacido en 1952).

Nunca se ha casado y ha evitado activamente hablar sobre sus relaciones sentimentales, manifestando un deseo de proteger su neutralidad como periodista.

Su reticencia pública contrasta deliberadamente con la vida de su madre, quien ha sido el centro de atención de los tabloides periodísticos y ha publicado sus memorias detallando explícitamente sus aventuras amorosas con celebridades. A pesar de que Cooper ha mantenido en privado sus asuntos personales, ha expresado su deseo de formar una familia y tener hijos.

La sexualidad de Cooper había sido cuestionada varias veces por los medios de comunicación, de hecho, en mayo de 2007, la revista Out usó una foto de él y otra de la actriz Jodie Foster para ilustrar un reportaje titulado «El armario de vidrio», donde se intentaba explicar por qué algunas celebridades preferían no admitir públicamente su homosexualidad. El 2 de julio de 2012, previa autorización de Cooper, el sitio web de The Daily Beast publicó un correo electrónico que envió a su amigo, el periodista y escritor Andrew Sullivan, donde asumía su homosexualidad con orgullo.

Desde el 2009 mantiene una relación amorosa con Benjamin Maisani y ha mencionado que tiene intenciones de casarse con él en Nueva York, cuando las uniones entre parejas del mismo sexo sean legales en ese estado. Actualmente vive en la ciudad de Nueva York, en una estación de bomberos que adquirió en enero de 2010, tras pagar alrededor de 4,3 millones de dólares, y que modificó para que sea una vivienda.

El 30 de abril de 2020, Cooper anunció el nacimiento de su hijo Wyatt Morgan Cooper, al que tuvo mediante vientre de alquiler. Anunció el nacimiento de su segundo hijo, Sebastian, en febrero de 2022.

Véase también

Ana Navarro Flores
Andrés Oppenheimer
Carlos Alberto Montaner
Carlos Montero
Fareed Zakaria
Geovanny Vicente Romero
Glenda Umaña
Patricia Janiot
Pedro Bordaberry
Sylvia Garcia
CNN en Español

Referencias

Bibliografía

Enlaces externos
 AndersonCooper.com, Sitio oficial. (Inglés)
 Perfil de Anderson Cooper en CNN. (Inglés)
 AC360.Blogs.CNN.com, Blog de Anderson Cooper en CNN. (Inglés)

Hombres
Nacidos en 1967
Alumnado de la Universidad Yale
Blogueros de Estados Unidos
CNN
Corresponsales de guerra de Estados Unidos
Escritores gais
Ganadores del Premio Emmy
Modelos masculinos de Estados Unidos
Personas de Nueva York (estado)
Periodistas de Estados Unidos
Periodistas gais
Personas LGBT de Nueva York
Modelos infantiles de Estados Unidos
Homosexuales de Estados Unidos
Familia Vanderbilt

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction} \label{sec:intro}
Solar filaments are filled with cool dense plasma, manifesting as cool clouds suspended in the surrounding hot tenuous corona. They appear as elongated absorption features
on the solar disk in $H_{\alpha}$ and some extreme ultraviolet (EUV) lines \citep{anz05}. Outside the solar disk, they appear as emitting plasma structures
called ``prominences". Filaments are usually formed above the polarity inversion lines (PILs),
which separate positive and negative magnetic flux regions in the photosphere \citep{mar98}. It has become a consensus that magnetic field supports
the cold and dense plasma of filaments against gravity in the corona. Despite over a century of increasingly detailed observations and studies,
the mechanism accounting for the filament formation is still controversial. Unravelling the mechanism of filament formation
requires a thorough understanding of the formation of the magnetic structure and the cool dense plasma of filaments.

As stressed by \citet{chen20a} that a filament should be a coronal structure. Many direct measurements of prominence magnetic fields
have shed some light on the magnetic structure of prominences \citep{ler89,oro14,schm14}.
However, it is difficult to determine prominence magnetic fields due to the ambiguity of Stokes inversion or the coronal magnetic fields surrounding the prominences.
The detailed magnetic structure of filaments is still far from being fully understood. Nevertheless,
previous theoretical and observational studies on filaments have deepened our understanding of the magnetic structure of filaments.
Sheared arcades \citep{ks57,dev00} and flux ropes \citep{kr74,van89} are believed to be suitable for supporting filaments.
A flux rope naturally contains magnetic dips above the PILs, and the cool dense plasma of the filaments is preferentially supported in the dips.
A sheared arcade can contain or not contain magnetic dips. Considering a filament is a dynamic entity, \citet{kar01}
suggested that filaments can even be supported by sheared arcades without magnetic dips. Both sheared arcades and flux ropes
can be formed by the surface mechanisms or the subsurface mechanisms \citep[see the review by][]{mac10}.
In the surface mechanisms \citep{van89,mar01}, magnetic reconnection occurs between a series of magnetic arcades
straddling the PILs to form the sheared arcades or flux ropes, under the joint of photospheric shear flows parallel to the PILs and converging flows perpendicular to the PILs.
In the subsurface mechanisms, a preexisting flux rope in the convection zone partly emerges through the solar surface into the corona by buoyancy \citep{rus94,fan01}.
Hitherto, a great deal of observations have tended to support the surface mechanisms \citep{chae01,yan16,yang15,yang16,yang19a,chen20b},
and only a handful of observations have been in favor of the subsurface mechanisms \citep{oka08,lit10,xu12,yan17}.

It is generally accepted that the filament plasma originates from the solar chromosphere \citep{song17,chen20a},
but the mechanism by which the chromospheric plasma is transported into the corona to form filaments is still under debate.
Historically, there are three promising models for chromospheric plasma being transported into the corona to form filaments \citep{mac10,chen20a}.
The first is the injection model, which demonstrated that chromospheric plasma can be injected into a filament channel through magnetic reconnection \citep{wang99,liu05,wang18,shen19,yang19b,wei20}.
The second is the levitation model, which suggested that chromospheric plasma can be directly lifted to the corona by emerging flux or magnetic flux cancellation \citep{rus94,zhao17}.
The third is the evaporation-condensation model, which proposed that chromospheric plasma can be heated to several million kelvin and evaporated into the corona,
and then thermal instability \citep{par53,fie65} or thermal non-equilibrium \citep{ant91,ant00} causes catastrophic cooling and coronal condensation.
The essence of this model is that artificial localized heating concentrated exclusively at the chromospheric footpoints of magnetic loops
are needed to heat the chromosphere and then drive chromospheric evaporation. More recently,
\citet{huang21} tried to unify the injection model and the evaporation-condensation model in a single framework.
They found that when the localized heating is situated in the upper chromosphere,
the local plasma is heated to evaporate into the corona; when the localized heating is situated in the lower chromosphere,
the enhanced gas pressure pushes the cold upper chromospheric material to be injected into the corona.
On the basis of the evaporation-condensation model, an increasing number of numerical simulations have successfully simulated the formation of filaments with steady or
non-steady localized heating symmetrically or asymmetrically distributed at the two chromospheric ends of filaments \citep{kar08,xia11,luna12,kep14,xia16,zhou20}.
Moreover, many dynamic phenomena of filaments, such as filament oscillations \citep[see the review by][]{chen20a}, the moving blobs \citep{luna12,xia16},
the plasma circulation of long-lived filaments \citep{xia16}, the cold $H_{\alpha}$ counterstreaming flows \citep{xia11,zhou20},
and the hot EUV counterstreaming flows between filament threads \citep{zhou20}, have also been simulated.

The evaporative-condensation model has been extensively and thoroughly analyzed in numerical simulations,
but complete and definitive observations that support and validate this model have not yet been reported.
So far, only two undisputed observations of coronal condensation forming prominences have been reported. \citet{liu12} presented a clear observation that coronal condensation occurs
at the magnetic dips of a transequatorial loop system and results in the formation of a cloud prominence after a confined eruption. Soon after, \citet{ber12} observed
the dynamic formation of a quiescent polar crown prominence in a coronal cavity and implied that the prominence is formed via in situ condensation of hot plasma from the coronal cavity.
In both cases, it is not clear whether the hot plasmas originate from chromospheric evaporation. The direct injection \citep{wangj07} and even magneto-thermal convection
involving emerging magnetic bubbles and plumes \citep{ber11} are all potential sources of the hot plasmas. In addition, recent numerical simulation \citep{kan17}
and observations \citep{li18,li21} also proposed that apart from artificial localized heating in the chromosphere,
magnetic reconnection in the corona can also trigger thermal instability and result in coronal condensation.
In this paper, we report the first definitive observation that magnetic reconnection and associated chromospheric evaporation followed by coronal condensation lead to the formation of a filament.
This observation may enhance our understanding on the filament formation.

\section{Observations}
The event was well-observed by the Atmospheric Imaging Assembly \citep[AIA;][]{lem12} and the Helioseismic and Magnetic Imager \citep[HMI;][]{sch12}
on board the \emph{Solar Dynamics Observatory} \citep[\emph{SDO};][]{pes12}. AIA takes the full-disk images of the Sun in seven EUV
and two ultraviolet (UV) wavelengths with a pixel size of 0$\arcsec$.6 at a high cadence of up to 12s.
Here, the Level 1.5 images centered at 304 \AA \ (\ion{He}{2}, 0.05 MK), 171 \AA\ (Fe {\sc ix}, 0.6 MK ), 193 \AA\ (Fe {\sc xii}, 1.3 MK and Fe {\sc xxiv}, 20 MK),
211 \AA \ (\ion{Fe}{14}, 2 MK), 335 \AA \ (\ion{Fe}{16}, 2.5 MK), 94 \AA\ (\ion{Fe}{18}, 7 MK), 131 \AA \ (Fe {\sc viii}, 0.6 MK and Fe {\sc xxi}, 10 MK),
and 1600 \AA \ (\ion{C}{4} + cont., 0.01 MK) were adopted to study the event.
HMI provides full-disk continuum intensity images and the vector magnetic field data with a pixel size of 0.$\arcsec$5.
The time cadence of the HMI are 45 s (for the continuum intensity images) and 720 s (for vector magnetic field data).
In addition, we used $H_{\alpha}$ images from the Global Oscillation Network Group (GONG) and the New Vacuum Solar Telescope \citep[NVST;][]{liu14},
soft X-ray (SXR) flux of flare at 1-8 \AA\ from the \emph {Geostationary Operational Environmental Satellites (GOES)},
and SXR image from the X-ray Telescope \citep[XRT;][]{gol07} on board the \emph{Hinode}  \citep{kos07} satellite. Images taken from the AIA, HMI, and GONG
were aligned by differentially rotating to the reference time of 22:30 UT on 2014 February 2.

To detect the chromospheric evaporation, the spectroscopic data from the EUV Imaging Spectrometer \citep[EIS;][]{cul07} onboard \emph{Hinode} satellite was also analyzed.
We mainly used the EIS data during the period of 21:31:12 UT and 21:39:58 UT that corresponds to the impulsive phase of the flare.
EIS observed this flare with 15 spectral windows, using a 2$\arcsec$ wide slit and 3$\arcsec$ step size with an exposure time of 5 s.
The spectra were taken at 80 positions, and it took an averaged duration of 8 minutes to scan an area of 240$\arcsec$$\times$304$\arcsec$.
Here, we concentrated on three strong emission lines, \ion{He}{2} 256.32 \AA, \ion{Fe}{15} 284.16 \AA, and \ion{Fe}{16}  262.98 \AA,
which provide temperature coverage from the chromosphere (log T$\approx$4.7) to the corona (log T$\approx$6.4).
The EIS level-0 data was performed with the standard Solar Software(SSW) eis\_prep.pro routine to correct the dark current, detector bias, hot pixels,
cosmic rays, and radiometric calibration. Meanwhile, the orbital variation and wavelength calibration were also corrected by using house keeping data \citep{kam10}.
Then, we used the standard SSW eis\_auto\_fit.pro routine with a single Gaussian model to derive spectral intensities, line widths and Doppler velocities.
To derive the reference wavelengths of the three strong emission lines,
the average line centers of \ion{He}{2}, \ion{Fe}{15}, and \ion{Fe}{16} lines for the quieter region of the EIS FOV were measured, respectively.
The Doppler velocities estimated by Doppler shift in these emission lines have a few km s$^{-1}$ uncertainty.

\section{Results}
\subsection{Overview of AR 11967 and Photospheric Magnetic Field Evolution }
On 2014 February 2, NOAA AR 11967 was located at about S$13\degr$E$04\degr$.
Figures 1({\it a})-({\it b}) illustrate the general appearance of the AR. On this day, four M-class flares occurred in this AR,
three of which had unique X-shape ribbons and occurred in a facular region of the AR (for a detailed analysis of these flares, see \citet{liu16}),
one had a typical two ribbons and took place in the central and northwestern section of the AR (enclosed by the blue box in Figure 1({\it a})).
Here, we focus on the M1.3 two ribbon flare, which started at about 21:24 UT, peaked at 22:04 UT, and ended at 22:14 UT in \emph{GOES} 1-8 \AA\ flux.
Apart from its two ribbons, the most striking feature of this flare is that the flare had a conjugate compact footpoint brightenings (Figure 1({\it c})).
The conjugate compact footpoint brightenings were more pronounced in the $H_{\alpha}$ observations (see the inserted images in Figure 2).
They were distributed on the sunspots with opposite polarities and corresponded to the footpoints of the subsequent formed filament (Figures 1({\it c}) and ({\it d})).

The central and northwestern section of the AR, where the flare of interest occurred, developed rapidly and formed a contiguous penumbral structure (Figure 1({\it a}))
due to magnetic flux emergence. The emerging magnetic flux was characterized by one negative sunspot, labeled as ``N",
and two major positive sunspots, labeled as ``P" and ``P1" (Figure 1({\it a})). There was constant flux emergence between P and N.
A significant flux of positive polarity emerged toward and merged with P, a significant flux of negative polarity emerged to the east of P
and then migrated eastward into N, forming an elongated channel of negative magnetic fluxes (Figure 1({\it b})).
For the sake of description, we call the elongated channel as the negative magnetic channel.
In this region, the photospheric magnetic field was highly sheared with respect to the PILs (Figure 1({\it b})).
It is notable from the NVST high-resolution $H_{\alpha}$ image (Figure 1({\it d})) that the emerged sunspots with opposite polarities were connected by highly sheared arch filament systems (AFS).
Figures 1({\it e})-({\it g}) show the evolution of the photospheric magnetic field before, during, and after the flare, covering part of the episodes of the flux emergence.
It is clear that there was significant flux cancellation ongoing along the main PILs of this region.
Unsigned negative flux integrated in a red rectangle (Figure 1({\it g})) is shown in Figure 1({\it h}).
This region was selected to avoid the negative magnetic flux that continuously migrated along the negative magnetic channel into N.
One can see that the unsigned negative flux persistently decreased from the beginning to the end of the observation.
Applying the inductive DAVE4VM \citep{sch08} method to the 12-minute cadence HMI vector magnetic field data, we calculated the photospheric velocity field,
which integrated over two hours between 20:00 UT and 22:00 UT and superimposed on a HMI vertical image (Figure 1({\it f})).
Remarkably, persistent northwestward photospheric flows characterize the positive sunspots P and P1,
while southeastward photospheric flows dominate the negative sunspot N and the negative magnetic channel, displaying overall strong shearing motion over the core region of the flare.
These observations are suggestive that the flux cancellation ongoing along the PILs may be driven by the strong shearing motion and is tightly related to the
triggering of the flare and the subsequent formation of the filament.

\subsection{The Flare Associated with the Formation of a Sigmoid}
The light curves of AIA 131 \AA\ and \emph{GOES} 1-8 \AA\ SXR flux display multiple impulsive peaks in the course of the flare (Figure 1({\it h})).
This is similar to our previous observations \citep{yang19a} that each impulsive peak may correspond to a magnetic reconnection process.
Figures 2({\it a})-({\it d}) show the evolution of the flare associated with the formation of a sigmoid structure.
It is clear that a set of brighter and shorter hot loops, which apparently connect P1 to the negative magnetic channel,
firstly appeared near the negative sunspot N (panels ({\it a}) and ({\it b})). Afterwards, another set of brighter and shorter hot loops,
which connect the positive magnetic flux patches in between P and P1 to the negative magnetic channel, appeared close to the positive sunspot P (panel ({\it c})).
These hot loops appearing at different locations may be indicative of multiple magnetic reconnection processes occurring at different locations and different times.
As the flare progressed, longer hot loops apparently rooted in P and N were gradually formed and finally shown as a remarkable sigmoid structure (panels ({\it d}) and ({\it h})).
The sigmoid formed along the main PILs and had an inverse S-shape, which suggests negative, left-handed twist.

The evolution of the flare ribbons is shown on Figures 2({\it e})-({\it g}). The flare ribbons first appeared at the region where the negative magnetic channel
was in contact with P1 (panel ({\it e})). These ribbons were distributed on either side of the main PILs
and in line with the footpoints of the hot loops that appeared near N (panels ({\it a}) and ({\it e})).
Then, they developed parallel to the main PILs in opposite directions and formed a two ribbon flare (panel ({\it f})).
It is worth mentioning that a conjugate compact footpoint brightenings appeared at P and N (panel ({\it f})),
which were consistent with the footpoints of the formed sigmoid (panels ({\it d}) and ({\it h})).
Subsequently, more intense flare brightenings occurred at the footpoints of the hot loops that appeared close to P (panel ({\it g})).
At the same time, the area of the conjugate compact footpoint brightenings were further expanded.
It is evident from the inserted $H_{\alpha}$ images that the most pronounced flare ribbons correspond to the conjugate compact footpoint brightenings
and the footpoints of the hot loops. They showed up as four compact footpoint beightenings in the $H_{\alpha}$ observation at about 21:44:54 UT.
This flare was confined, the two main ribbons did not separate perpendicular to the PILs and there were no clear CME signatures.
These observations taken together with the photospheric observations introduced before are highly reminiscent of the tether-cutting reconnection scheme \citep{moore01,liu13,chen14,chen18}.
More precisely, our observations fit very well with the physical picture that a confined flare is triggered by the tether-cutting reconnection process.
Therefore, we argue that the confined flare associated with the formation of the sigmoid in the present study are the results of
a sequential tether-cutting reconnection processes occurred between the magnetic fields connecting P to the negative magnetic channel
and the magnetic fields connecting P1 and its nearby positive flux patches to N.
Moreover, these reconnection may be driven by the strong shearing motion during the flux emergence.

\subsection{Chromospheric Evaporation at the Conjugate Footpoint Brigthenings}
Chromospheric evaporation, first described by \citet{ne68}, refers to the process during a solar flare
that chromospheric materials are heated and then expand rapidly upward into the low-density corona,
thus fill up the coronal loops giving the hot and dense post-flare loops that can be visible at the EUV and SXR wavelengths.
This process occurs when the flare energy deposit in chromosphere by non-thermal electrons or thermal conduction exceeds what can be shed by radiative losses.
The blueshifts that correspond to plasma upflows in emission lines formed at flare temperatures provide strong evidence for chromospheric evaporation.
It is recognized that the evaporation is identified as explosive when emission lines formed at flare temperatures exhibit blueshifts
while emission lines formed at chromospheric and transition region temperatures exhibit redshifts; the evaporation is considered as gentle
when emission lines formed at all temperatures exhibit blueshifts \citep{fis85,bro09,mil09,chen10,li11,young13,tian15}.

Using spectroscopic observations from the \emph{Hinode}/EIS, chromospheric evaporation at the conjugate footpoint brightenings is well diagnosed.
Figures 3({\it a} \sbond {\it c}) show the spatial distribution of line intensity, Doppler velocity, and line width
for the \ion{Fe}{15} 284.16 \AA\ line in the impulsive phase of the flare. The conjugate footpoint brightenings are the sites of rapid chromospheric heating,
they are also shown as a pair of intense, compact brightenings in the \ion{Fe}{15} 284.16 \AA\ emission line (panel({\it a})).
It is evident from the Doppler velocity map (panel({\it b})) that the conjugate footpoint brightenings are dominated by blueshifts.
In particular, these blueshifts are accompanied by relatively large line widths (panel({\it c})).
We selected two points, which denoted by the crosses and marked ``1" and ``2",
to extract the \ion{He}{2} 256.32 \AA, \ion{Fe}{15} 284.16 \AA, and \ion{Fe}{16} 262.98 \AA\ line profiles.
Point 1 lies in the positive footpoint of the conjugate  footpoint brightenings while point 2 lies in the negative footpoint of the conjugate footpoint brightenings.
EIS scanned points 1 and 2 at 21:32:47 UT and 21:37:20 UT, respectively. The \ion{He}{2}, \ion{Fe}{15}, and \ion{Fe}{16} line profiles at point 1
are displayed on Figures 3({\it d} \sbond {\it f}) and at point 2 are displayed on Figures 3({\it g} \sbond {\it i}).
We fitted all the line profiles at points 1 and 2 using a single Gaussian function.
The fitting results are shown as red curves in Figures 3({\it d} \sbond {\it i}). It is seen that the chromospheric \ion{He}{2} line shows significant redshifts
while the coronal \ion{Fe}{15} and \ion{Fe}{16} lines show significant blueshifts at both locations.
The redshift velocities are measured to be 14.1 and 14.0 km s$^{-1}$ at points 1 and 2, respectively.
The blueshift velocities are measured to be -28.9 km s$^{-1}$ and -11.2 km s$^{-1}$  for the \ion{Fe}{15} line,
-30.3 km s$^{-1}$ and -17.6 km s$^{-1}$ for the  \ion{Fe}{16} line at points 1 and 2, respectively.
These results reveal that explosive evaporation occurred at the conjugate footpoint brightenings in the impulsive phase of the flare.

\subsection{Coronal Condensation Resulting in the Filament Formation}
The explosive evaporation occurring at the conjugate footpoint brightenings may provide heated material to make the formed sigmoid overdense,
which is conducive to trigger thermal instability or thermal non-equilibrium, causing catastrophic cooling and coronal condensation.
Figure 4 presents the formation and evolution of cool condensations in the sigmoid and the formation of a filament.
At 22:50:38 UT, about 34 minutes after the flare ended, a set of bright loops gradually appeared (panel ({\it a1})).
At the same time, the initial condensation (as indicated by the red arrow in panel ({\it b1})), which can be clearly identified in the AIA 335 \AA\ observation,
formed at about the middle portion of these bright loops. Thereafter, the condensations continued to grow and moved in opposite directions along these bright loops
( see panels ({\it a2} \sbond {\it a3}), ({\it b2} \sbond {\it b3}), and the associated animation), forming a long filamentary structure (panel ({\it c2} \sbond {\it c3})).
These condensations are short-lived. They finally moved toward and fallen rapidly to the footpoints of these bright loops.
As a result, the bright loops faded and the long filamentary structure disappeared.
Following the disappearance of the long filamentary structure, another set of bright loops, which has an overall inverse S-shape, gradually appeared (panels ({\it a3} \sbond {\it a4})).
Similarly, the cool condensations firstly formed at about the middle portion of these inverse S-shaped bright loops,
they then continued to grow and moved in opposite directions along these bright loops (panels ({\it a4}) and ({\it b4})),
resulting in the formation of two long, almost parallel filamentary structures (panel ({\it c4})). As the condensations persistently formed and moved in opposite directions along the two
filamentary structures, a filament with an inverse S-shape was formed (panels ({\it a5} \sbond {\it a6}), ({\it b5} \sbond {\it b6}), and ({\it c5} \sbond {\it c6})).
The formed filament was rooted in the locations corresponding to the conjugate footpoint brightenings (see Figure 1({\it c})),
with its positive ends anchored in the positive sunspot P and its negative ends anchored in the negative sunspot N (panel ({\it c6})).
The filament is sinistral, indicating negative, left-handed twist \citep{mar98}, which is in line with the sigmoid.

The gradual emergence of the bright loops should be the result of the gradual cooling of the formed sigmoid over time after the flare.
Apparently, the first appeared bright loops are low-lying relative to the inverse S-shaped bright loops.
The successive appearance of cool condensates in the low-lying bright loops and then inverse S-shaped bright loops
are consistent with the observation of \citet{liu12} and the simulation of \citet{kar08}. They implied that cool condensations firstly formed at
those low-lying loops are due to their shorter lengths and/or their greater densities from gravitational stratification.
To trace the dynamic evolution of the cool condensations in the low-lying and the inverse S-shaped bright loops, spacetime plots along slice ``AB" and ``CD" in Figures 4({\it a1}) and ({\it a5})
were constructed from AIA 335 \AA\ images, and the result was provided in Figures 5({\it c}) and ({\it d}).
The cool condensations moved in opposite directions along the low-lying and the inverse S-shaped bright loops are clearly shown on the spacetime plots.
we find that the cool condensations moved along the low-lying bright loops to their positive ends with a mean velocity of about 43.3 km s$^{-1}$
and to their negative ends with a mean velocity of about 39.4 km s$^{-1}$; the cool condensations moved along the inverse S-shaped bright loops to their positive ends
with a mean velocity of about 36.6 km s$^{-1}$ and to their negative ends with a mean velocity of about 37.1 km s$^{-1}$.

As the sigmoid gradually cooling over time after the flare, similar to the off-limb condensation events \citep{ber12,liu12,li18}
that the peak brightness of the appearing bright loops should progressively shift in time
from the AIA broadband channels with higher characteristic temperatures to the channels with lower characteristic temperatures.
However, this trend can not be definitively detected in this on-disk observation owing to intermittent magnetic activities still occurred after the flare.
It is interesting to note that a transient brightening (as denoted by the blue arrow in Figure 5({\it a}))
appeared in the inverse S-shaped loops during the formation of the filament.
It cooled down over time and finally formed cool condensations (as pointed out by the red arrow in Figure 5({\it b})) in the inverse S-shaped loops.
This transient feature is very similar to the long, transient brightening simulated by \citet {luna12}.
They suggested that this long, transient brightening is the consequence of the evaporation and condensation.
In the red dashed rectangle, enclosing the long, transient brightening in Figure 5({\it a}), the light curves of the AIA 211, 193, and 171 \AA\ channels were calculated
and displayed in Figure 5({\it e}) as blue, red, and green curves, respectively. It is obvious that the peak brightness of the long, transient brightening progressively shifts in time
from the 211 \AA\ channel, through the 193 \AA\ channel, to the 171 \AA\ channel. The long, transient brightening peaked first in the 211 \AA\ channel at about 23:21:36 UT.
With a delay of about 72 seconds, it peaked in the 193 \AA\ channel at about 23:22:48 UT. Then, it peaked in the 171 \AA\ channel at about 23:23:17 UT,
29 (101) seconds later than the peak of AIA 193 (211) \AA\ light curve. These results strongly suggest that hot plasma evaporated from the chromosphere cools down
and condenses in the sigmoid to form the cool dense filament, probably due to the onset of thermal instability or thermal non-equilibrium.

\section{Conclusion and Discussion}
In this study, we report a clear observation of a solar filament formed through chromospheric evaporation and subsequent coronal condensation after an M-class confined flare.
Our investigations show that this confined flare is triggered by a sequential tether-cutting reconnection processes as strong magnetic shear occurring during flux emergence in the NOAA AR 11967.
Owing to the tether-cutting reconnection, an elongated magnetic structure is newly created above the flaring PIL, which separately bridges its footpoints at two conjugate compact brightening regions.
The spectroscopic observations from the \emph{Hinode}/EIS reveal that explosive chromospheric evaporation takes place at the two compact brightening regions in the impulsive phase of the flare.
In this course, because the explosive injection of heated chromospheric plasma from its footpoints, the newborn elongated magnetic structure soon manifests as an X-ray sigmoid.
After the flare, cool material continuously condenses in the middle section of the sigmoid and then moves in opposite directions along the magnetic field lines of the sigmoid,
eventually resulting in the formation of a filament in the 304 \AA \ passband. This indicates that the evaporated hot plasma, which trapped in the sigmoid,
cools down to at least $\sim$ 0.05 MK within tens of minutes, possibly due to the onset of thermal instability or thermal non-equilibrium.
These observations demonstrate that magnetic reconnection not only directly create the desirable magnetic field structure for filament formation,
but also indirectly supply cold and dense material for the forming filament in tens of minutes through resultant chromospheric evaporation and subsequent coronal condensation.

Observational evidence of chromospheric evaporation has not been detected in filament formation events,
but has been documented in numerous flare events of different magnitude \citep{ding96,mil09,ning09,cheng15,li15,zhang16,huang20}.
In the framework of the standard flare model \citep{pri02}, electrons are accelerated at or near a magnetic reconnection site in the corona,
the accelerated electron beams propagate downward along newly reconnected magnetic field lines and then bombard the chromosphere to generate chromospheric evaporation.
Meanwhile, thermal conduction from the reconnection site may also contribute to the heating.
In our observation, in the course of the formation of the sigmoid by the sequential tether-cutting reconnection processes,
it is quite possible that reconnection-accelerated electron beams or thermal conduction from the reconnection sites
may travel or spread along the magnetic field lines of the sigmoid in opposite directions and toward their conjugate chromospheric footpoints.
As a result, the conjugate chromospheric footpoints of the sigmoid would be heated, manifesting as the conjugate compact footpoint brightenings.
Owing to the heating, as confirmed by the \emph{Hinode}/EIS spectroscopic observation that explosive evaporation occurred at the conjugate footpoint brightenings,
heated chromospheric plasma may thus be evaporated into the sigmoid and make it overdense.
Subsequently, thermal instability or thermal non-equilibrium might be triggered, causing catastrophic cooling and coronal condensation to form the cold, dense material of the filament.

The evaporation-condensation model is a promising candidate that accounts for the filament formation.
However, unambiguous observations directly validating this model have been missing up to now.
A handful of previous observations have shown that coronal condensation can lead to the formation of prominences \citep{ber12,liu12,viall20},
but the origin of the hot plasma involved in the coronal condensation has been questionable. In these observations and previous simulations \citep{ant91,kar08,luna12,xia16},
the formation of the filament magnetic structure and its cold dense material have been treated separately.
In actual fact, the formation of filaments are the results of both magnetic and thermal evolution.
\citet{kan17} proposed a reconnection-condensation model, which treated the formation of the filament magnetic structure and its cool dense material together,
to explain the formation of filaments. It is worth noting that any artificial localized heating in the chromosphere
is not considered in their model. Their model does not include the chromosphere and the resultant prominence mass only reaches the observed lower limit of typical prominence densities.
The magnetic reconnection in their model forms the filament magnetic structure and directly triggers thermal instability causing coronal condensation.
The reconnection induced topology changes triggering thermal instability and the formation of cool plasma condensations was subsequently confirmed in coronal rain observations \citep{li18,mas19,li21}.
In the present study, the formation of the filament magnetic structure and its cold dense material are treated together from the perspective of observation for the first time.
Our observations demonstrate that the formation of the filament magnetic structures by magnetic reconnection also has a profound influence on the subsequent thermal evolution occurring in it.
Different from \citet{kan17} and \citet{li18}, the magnetic reconnection in our observation might affect the subsequent thermal evolution in the filament magnetic structures
by heating their chromospheric footpoints during their formation.
This is consistent with the evaporation-condensation model \citep{ant91,ant00}.
This observation, for the first time, presents unambiguous observational evidence that both chromospheric evaporation
and subsequent coronal condensation take place in the formation of a filament, in support of the evaporative-condensation model.

The formed filament was short-lived. It only lived for about an hour and then gradually disappeared.
In the framework of the evaporation-condensation model, numerous simulations have shown that deep magnetic dips are necessary for supporting the cool condensations \citep{luna12,zhou20}.
In this scenario, a typical dynamic phenomenon that can usually be seen during the filament formation is the longitudinal oscillation of the filament \citep[see the review by][]{chen20a}.
In the absence of magnetic dips, the formation of long-lived filaments requires constant chromospheric footpoint heating to maintain a stable cycle,
in which plasma evaporates from the chromosphere, condenses into the filament in the corona, and drains back to the chromosphere along the magnetic field lines of the filament \citep{kar01}.
In the present study, any oscillations during the formation and disappearance of the filament are not observed.
Moreover, continual chromospheric footpoint heating and coronal condensation are not occurred after the filament formed.
It is likely that the filament might not contain deep magnetic dips, which are suitable for supporting the cool condensations.
The cool condensations could not be stably supported in the filament and thus drain in opposite directions along the filament, ultimately causing it to be short-lived.
The real and detailed magnetic field structure of the filament needs to be further investigated.

Generally, the formation of a quiescent prominence is days and even weeks long and the quiescent prominences are long-lived.
\citet{ber12} found that quiescent prominences can be formed via in situ condensation of hot plasma contained in the core of the
coronal cavity. However, the origin of the hot plasma is not yet identified. Although flux emergence and local reconnection have been suggested,
the possibility of chromospheric evaporation can not be ruled out. In the quiet Sun, the explosive events, such as reported in this paper, never happen.
But during the formation and evolution of the quiescent filaments, photospheric magnetic flux cancellation,
which might be closely related to the magnetic reconnection occurring in the lower atmosphere of the Sun, was found to be abundant near the PILs \citep{mar98,mac10}.
This process can also heat the footpoints of the reconnected coronal loops \citep{yang16,yang18}.
It is possible that gentle evaporation might be driven by the magnetic reconnection occurring in the lower atmosphere of the Sun during the formation of the magnetic structure of
the quiescent prominences. In addition, \citet{zhou20} recently proposed that turbulent heating on the solar surface can randomly evaporate materials from the solar surface to the corona,
leading to quiescent prominence formation. So far, observational evidence of chromospheric evaporation has not been observed during the formation and evolution of quiescent prominences.
The applicability of the evaporative-condensation model to quiescent prominences needs to be verfied by more high-resolution spectral and imaging observations in the future.
In the active region, the explosive events reported in this paper could frequently happen, and they will be more likely to be associated with active region filament formation.

\begin{acknowledgments}
We thank the referee for valuable suggestions and comments that greatly improved the paper.
The authors thank the scientific/engineering team of \emph{SDO}, \emph{Hinode}, \emph{GOES}, NVST, and GONG for providing the excellent data.
We would like to thank Dr. Hechao Chen for his fruitful comments.
This work is supported by the National Key R\&D Program of China (2019YFA0405000), the Natural Science Foundation of China, under grants 12073072,
11633008, 11933009, 12173084, 11873088, and 11703084; the CAS ``Light of West China" Program;
the Open Research Program of the Key Laboratory of Solar Activity of Chinese Academy of Sciences (KLSA202018);
the CAS grant ``QYZDJ-SSW-SLH012"; the Yunnan Natural Science Foundation, under grants 202001AU070052 and 202101AV070004;
and the Project Founded by China Postdoctoral Science Foundation 2020M671639.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


text:
Police identify man killed while trying to roll under Union Pacific train in Salt Lake City
By: Taylor Hartman
SALT LAKE CITY — A man who died while rolling underneath a Union Pacific train has been identified by police.
According to Det. Wilkings with the Salt Lake City Police Department, 22-year-old Jeremy Thomas was found near 800 South and 600 West on August 25 after he tried to cross the railroad tracks by going underneath a parked train.
"It looks like he kind of squatted down and tried to roll underneath it like in the movies or something," Lt. Russ Amott said in August. "The train caught him, pulled him under the tracks and he was killed."
Thomas did not have identification on his person when he died. Wilkings confirmed that investigators believe he may have been a transient.
Police said at the time the man was found they are not investigating the incident as a suicide.


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