text:
Vietnam fifty years on
30 Apr 2015|Peter Edwards
SHARE Share to Facebook Share to Twitter Share to LinkedIn Share to Email
With ImagesWithout Images
Last weekend's commemorations of the centenary of the Gallipoli landings was the ultimate expression of our habit of reflecting on the causes, conduct and consequences of war at the time of major anniversaries. Unfortunately, Australia's major wars of the twentieth century occurred, with remarkable precision, at quarter-century intervals. Thus the centenary commemorations of 1914–18 will overshadow the 75th anniversaries of major turning points in the Second World War and the 50th of those of the Vietnam War.
Fifty years ago this week, Prime Minister Robert Menzies announced the commitment of the first battalion of Australian combat troops to Vietnam on 29 April 1965. Ten years later, on 30 April 1975, the war ended as North Vietnamese tanks crashed through the gates of the presidential palace in Saigon. In a particularly cruel irony, the Australian ambassador closed our Saigon embassy and headed for the airport five days earlier—the 60th anniversary of the Anzac landing.
If Gallipoli had occurred, say, a year earlier or a year later, those anniversaries might now prompt a substantial discussion of the rights and wrongs of the Vietnam War and its implications for many areas of Australian political and social life: grand strategy, military operations, conscription, and the physical and mental health of veterans. Instead, we have only a few references in public discussion.
That gap matters. While the scale of our 1965–72 commitment does not compare with that of 1914–18—to use one crude but telling index, 521 service personnel dead from a population of about 12 million compared with 60,000 from a population of less than 5 million—the impact of Vietnam is more immediate. Any new commitment, especially as part of a coalition led by the United States, is still likely to meet the challenge: 'Is this another Vietnam?' And the current Minister for Veterans' Affairs takes every opportunity to say that our Iraq and Afghanistan veterans must be treated better than those from Vietnam.
So how should we look at the Vietnam War, half a century on? First, it was not a case of Australian involvement in 'other people's wars'. As far as Robert Menzies was concerned, it was more a matter of getting the US to fight Australia's wars. Australian strategy was based on the need to keep Britain and the United States committed to the security of Southeast Asia, which clearly mattered more to Australia than to northern hemisphere allies.
Menzies, it seems, feared American isolationism more than American overreach. He, and those from whom he chose to take advice, found it difficult to believe that the United States, if fully committed to a conflict, could be defeated. It was a huge miscalculation, but understandable given Menzies' personal experience as a young man during WWI, which the US did not enter until 1917, and as Prime Minister in 1939–41, before Pearl Harbor. To him, and others of his generation, what really mattered was Washington's commitment: if the Americans were involved, it seemed, success was certain.
Australia had a very specific reason to be concerned about American policy. In the early 1960s Australians were deeply concerned about another, much closer, Southeast Asian conflict. Australian forces were supporting the new federation of Malaysia against Indonesia's 'confrontation'. It was a low-level conflict, but Australian policymakers constantly feared that Indonesia might raise the stakes, not only on the Malayan peninsula but also across Australia's only land border—between Indonesia's West New Guinea and the Australian territories on the eastern half of the island (today's Papua New Guinea). When Australian ministers asked American officials at what stage Indonesian aggression might prompt support under ANZUS, the Americans clearly hinted that much would depend on Australian support for the American position in Indochina.
The Vietnam War was not about regime change, but about regime defence. There was never any intention to overthrow the communist government in Hanoi: the aim was only to prevent the fall of an anti-communist government in the south. In that sense, Vietnam was more akin to the first Gulf war of 1991 than to the Iraq invasion of 2003.
Above all, we should remember what else was happening in Southeast Asia in 1965. The Indonesian Communist Party was the third largest in the world. President Sukarno said 1965 would be a 'year of living dangerously' with the support of a 'Beijing-Jakarta' axis. Tensions between Kuala Lumpur and Singapore would soon lead to the ejection of Singapore from Malaysia. Thailand faced a substantial communist insurgency in its northeast. It is hardly surprising that many of the region's 'dominoes'—most publicly Singapore's Lee Kuan Yew—fervently urged the Americans not to withdraw. We learn from Jeremy Hearder's new biography of Sir James Plimsoll that Indian generals were expressing a similar view in early 1965.
By 1968–69, much had changed in the region. Indonesia was now securely under the anti-communist President Suharto. Malaysia and Singapore were functioning better apart than together. Thailand had its internal insurgency under control. The formation of ASEAN in 1967 indicated that these non-communist nations were willing to collaborate better. In short, the only dominoes likely to fall with South Vietnam would be Laos and Cambodia.
For Australia and many other countries in the region, the 1965 commitment by the United States and its allies served a purpose, but the strategic gains were achieved by the end of the 1960s. The real tragedy of the Vietnam War was that it continued well into the 1970s, at huge cost to all external participants, and most of all, to the Vietnamese people.
Peter Edwards is the author of Crises and Commitments, A Nation at War and Australia and the Vietnam War. ASPI will soon publish his Strategy paper on Learning from history: some strategic lessons from the 'forward defence' era. Image courtesy of FLickr user tommy japan.
Asia–Pacific
Malcolm Fraser and the American Alliance
The Nashos and Vietnam
Australia, Indonesia and Confrontation
China as Number One, Japan as Normal
Time for a grown-up discussion about national strategy
Gough's remaking of foreign policy
Reflections on Whitlam
Is major war obsolete?


text:
How long did it take on concorde from london to new york?
1 Why does the Concorde nose droop?
2 Was there turbulence on Concorde?
3 Can any Concordes still fly?
4 Who flew on Concorde the most?
5 How many Concordes are left?
6 Why was Concorde so fast?
7 How long did it take Concorde to fly from London to Australia?
8 How long did it take Concorde to fly from London to Sydney?
9 Did anyone survive the Concorde crash?
10 Could the Concorde crash have been avoided?
11 Could any of the Concorde fly again?
12 Will the Concorde ever fly again?
13 Is droop snoot a real term?
14 Was the Concorde a smooth ride?
15 What did Concorde feel like?
16 Why do planes fly at 35000 feet?
17 Did Concorde make a profit?
18 Where can I see Concorde in the UK?
19 What engine did Concorde use?
20 What was Fred Finns job?
Concorde was retired from service in October 2003 after British Airways and Air France blamed a downturn in demand and increasing maintenance costs.
Moreover, how much was a ticket on the Concorde? For an average round-trip, across-the-ocean ticket price of about $12,000, Concorde shuttled its upper-crust passengers over the Atlantic in about three hours: an airborne assemblage of wealth, power, and celebrity hurtling along at breakneck speed.
As many you asked, how fast could the Concorde fly from London to New York? It flew at 1300mph, quicker than the Earth spins. The Concorde soared so high that you could see the Earth's curve. A ticket from London to New York on a flight operated by British Airways cost a whopping $7,574 (Rs5,50,000), which is equivalent to $12,460 (Rs9 lakh) today.
Frequent question, what was the longest Concorde flight? In November 1986 a British Airways Concorde flew around the world, covering 28,238 miles in 29 hours, 59 minutes. Concorde used the most powerful pure jet engines flying commercially.
Quick Answer, how many crashes did Concorde have? The Concorde, the world's fastest commercial jet, had enjoyed an exemplary safety record up to that point, with no crashes in the plane's 31-year history.
Why does the Concorde nose droop?
Droop Nose But Concorde's long, pointed nose had a hinge. As the plane took off, landed, and taxied, the pilots tilted its nose forward so that they could see the runway. For supersonic flight, the nose was hydraulically lifted, streamlining the plane's shape and allowing it to efficiently pierce the air.
Was there turbulence on Concorde?
With four jet engines and afterburners, the plane could fly at twice the speed of sound and cruised at close to 60,000 feet, far above other airliners. … The ride was so smooth that there was hardly any sensation of flight. "No turbulence.
Can any Concordes still fly?
Concorde was retired from service in 2003 and no longer flies. Most remaining Concorde aircraft are now on public display. There now follows a table of the various locations where all existing models of Concorde can be found. Most of these locations are in France, the UK and the USA.
Who flew on Concorde the most?
Fred Finn was on the first and last Concorde flights and holds the Guinness World Record for the most Concorde flights as a passenger! In total, he flew 718 times on the Queen of the Skies between 1976 and 2003 – all of them in the same seat, 9A.
How many Concordes are left?
Three Concordes reside in the United States. All are production models formerly operated by British Airways and Air France.
Why was Concorde so fast?
Concorde was a comparatively light aircraft, with a 185-tonne MTOW compared to 333 tonnes for the Boeing 747-100. As such, its engine technology made a big difference in allowing it to 'supercruise' at more than twice the speed of sound.
How long did it take Concorde to fly from London to Australia?
The flight would be around 13 and a half hours (Ten hours of which would be in the air), and passengers would start with breakfast departing Sydney and would land in London just after lunch (local time obviously, the passengers would have a full day on board).
How long did it take Concorde to fly from London to Sydney?
They read 17 hours, three minutes, 45 seconds. Despite delays, a flypast in Perth and the flypast via Sydney, Concorde still established a record for flying between London and Sydney, breaking by almost 33 hours the old world record set in 1969.
Did anyone survive the Concorde crash?
PARIS (AP) _ Moments after a Concorde jet slammed into her hotel, a 21-year-old British woman jumped from a window, escaping the inferno that engulfed the building. … They were among those who escaped death in the crash Tuesday that claimed the lives of all 109 people on board the supersonic jet and four on the ground.
Could the Concorde crash have been avoided?
The jet could fly at over twice the speed of sound and get between Paris and New York in under three-and-a-half hours. But the disaster could have been avoided – is it wasn't for a rogue piece of metal less than the size of a penny.
Could any of the Concorde fly again?
The possibility of Return to flight for Concorde is extremely unlikely.
Will the Concorde ever fly again?
(CNN) — United Airlines has announced it will purchase up to 50 Boom Overture supersonic jets for commercial use by 2029, heralding the return of supersonic passenger flights nearly 20 years after the Concorde was decommissioned.
Is droop snoot a real term?
The droop-nose or droop-snoot refers to the ability of the Concorde's nose to move up and down, depending on the stage of flight. … When the Concorde approached a runway, the nose would droop down, allowing the pilots to see where the aircraft was headed.
Was the Concorde a smooth ride?
A Concorde captain raved that the plane flew beautifully, and that the only indication of its speed came from looking down at other jets far below that seemed as if they were flying backward — the Concorde was moving about 800 mph faster. … The ride was so smooth that there was hardly any sensation of flight.
What did Concorde feel like?
"Concorde was extremely small, only about 100 seats. It had more like office chairs, bucket seats, and very small windows. It was noisy, extremely noisy, but I challenge anybody not to have a smile from ear to ear when they got on it."
Why do planes fly at 35000 feet?
Due to lower resistance at higher altitudes, commercial airplanes can keep moving forward with minimal fuel expenditure. … A balance between operating costs and fuel efficiency is achieved somewhere around 35,000 feet, which is why commercial airplanes usually fly at that altitude.
Did Concorde make a profit?
The Concorde brought a $17.3-million profit to British Airways last year and a profit of $8.8 million to Air France in 1984, the most recent year for which figures were available.
Where can I see Concorde in the UK?
Visit Concorde in the United Kingdom On display almost as long is the pre-production aircraft G-AXDN. You can find this at the Imperial War Museum in Duxford, where it is open daily for visits.
What engine did Concorde use?
In the 1960s, the British Aerospace/Aerospatiale Concorde advanced commercial aviation immensely when it made supersonic travel a reality, using four Rolls-Royce/SNECMA Olympus 593 engines.
What was Fred Finns job?
Fred went on to work for an American licencing company and travelled the world building international relations. During that time, he regularly flew to South America, including Brazil, Argentina and Chile, Japan, Hong Kong, Dubai and Nigeria, and travelled to and from New York at least twice a week.
How long did concorde take to fly from london to new york?
Quick answer: How fast london to new york concorde?
Frequent question: How long did it take concord to get from london to new york?
You asked: How long did it take concorde from london to new york?
Frequent question: How long to get from london to new york on concorde?
Best answer: How long london to new york concorde?
How long did it take concorde to fly from london to new york?
Why do london numbers keep calling me?
How to tenderize london broil with baking soda?
How do you cut jerky in a top round London broil?
Quick answer: What is the main train station to get from london to bicester village?
What Americans should not do in London?
How much does the winner get for the london marathon?
Is hackney east london?
What time do shops shut in london on a sunday?

redpajama_set_name: RedPajamaCommonCrawl


The Reduced Reach Right-Hand Keyboard reduces reach to the mouse. An updated version of the KB1, ..
Without question, the Laptop Pro is the best Bluetooth keyboard you can get for your Mac. Built fro..
To enhance your typing experience, Adesso designed this keyboard to be fast and "whisper" quiet. Our..
The stylish design of this mini keyboard compliments any desktop or laptop. Users can connect with t..
The Adesso AKB-601UB spill resistant 18-key keypad is the keypad that you deserve to have for many r..
This mini Adesso USB keyboard includes a PS/2 Adapter, so that you can use this keyboard on any PC. ..
The Adesso Mini-Touch keyboard combines the control of an integrated touchpad with the features of a..
The Mini size keyboard is designed with 78 keys, and is equipped with an embedded numeric keypad, fe..
Do you need a pointing device, but you don't have enough room for a separate mouse? In that case, th..


text:
Artificial Intelligence Leads to Discovery that Helps Solve Cosmological Puzzles
By Alyssa Sistrunk on April 20, 2021
With the Helps of machine-learning techniques, a team of astronomers has discovered a dozen quasars that have been warped by a naturally occurring cosmic lens. Quasars are extremely luminous cores of distant galaxies that are powered by supermassive black holes. The long-standing struggle has paved its way towards success.Over the past four decades, astronomers had found about 50 quasars, which occurs when there is a massive expulsion from the galaxies. The latest study, which spanned only a year and a half, increases the number of known quads by about 25 percent and demonstrates the power of machine learning to assist astronomers.
"The quads are gold mines for all sorts of questions. They can Helps determine the expansion rate of the universe, and Helps address other mysteries, such as dark matter and quasar 'central engines,'" says Daniel Stern, Lead author of the new study and a research scientist at the Jet Propulsion Laboratory, which is managed by Caltech for NASA. They are not just needles in a haystack but Swiss Army knives because they have so many uses.
The new quasar quads, which the team has given several nicknames such as Wolf's Paw and Dragon Kite will help in future calculations of Hubble's constant and may illuminate why the two primary alignments are not adjacent to each other. The quasars lie in between the local and distant targets used for the previous calculations, so they give astronomers a way to probe the intermediate range of the universe.
Machine learning is an effective technique but it no way an alternative for human Intelligence. The human minds and their decisions are as capable as any technique to procure or deliver the best of the researches or discoveries.
Published in Artificial Intelligence and News
local and distant targets used for the previous calculations
Machine learning is an effective technique
several nicknames such as Wolf's Paw and Dragon Kite
Alyssa Sistrunk
Alyssa is a proficient is an adept at her job and belongs to the Science background, having completed her Masters in Physics and Electronics. With a legacy of working the writing field for a decade and a half, Alyssa has upskilled herself to deliver on-the-go, even in a time-constricted environment and with minimum budget allocation. Alyssa is credited to working with great houses both print and the electronic media. She shares and applies all her learning experience here at TechnologyAnalysis as she begins a journey in the digital platform.
More from Artificial IntelligenceMore posts in Artificial Intelligence »


WinCraft Duke Blue Devils Womens Round Dangle Earrings $9.99 Add a touch of shine and spirit to any day with these Duke Blue Devils Round Dangle earrings! Measuring at approximately one inch you'll be able to cheer the Duke Blue Devils on from anywhere without going over the top. The printed Duke Blue Devils graphics make these the perfect accessory for any look.
Your Price. Duke Blue Devils Nike Womens Basketball Legend Practice Team T Shirt Detroit Red Wings Striped Fanny Pack.
Magnets from the largest New York Giants Striped Fanny Pack.
Womens Duke Blue Devils Nike Womens Basketball Legend Practice Team T Shirt. Breaking news more every time you open your browser. Your searches. Duke Blue Devils WinCraft Round Dangle Earrings. Results 1 of. Nike Duke Blue Devils Womens Showtime Performance Full Zip Hoodie. Guaranteed. Turn on search history to start remembering your searches. Duke Blue Devils Nike Womens Basketball Legend Practice Team T Shirt Royal. Almost Gone! Duke Dangle Earrings.
Womens Dangle Earrings. We did not find results for Blue.
Wincraft Duke Blue Devils Womens Stadium Compliant Black Crossbody Purse Black. Devils Dangle Earrings WinCraft Duke Blue Devils Wordmark Lanyard with Detachable Buckle. WinCraft Duke Blue Devils Team Wordmark Lanyard with Detachable Buckle. Womens Round Dangle Earrings Nashville Predators White Mini Team Hockey Stick. Womens Nike Heathered Black White Duke Blue Devils Performance Touch Reversible Shorts Wincraft Dangle Earrings.
Maybe you would like to learn more about one of these? Wincraft Duke Blue Devils Official NCAA Car Magnet and Round. Get the best deal for Duke Blue Devils NCAA Magnets from the largest.


text:
International Business Times, Singapore Edition
North Korea Reports 'First' Suspected Case of COVID-19 But Doesn't Give Details, What Are They Hiding?
Experts have doubted the veracity of the claim made by the communist regime of being fully devoid of COVID-19 cases.
By Akshay Saraswat
July 26, 2020 13:01 +08
Kim Jong Un reappears
Despite rumors about its leader Kim Jong Un suffering from COVID-19, the nation of North Korea has continued to claim that it is free of Coronavirus infections. However, the government of the communist state has now revealed that it is faced with what it claims is the first suspected case of COVID-19.
The person suffering from the symptoms has been described as a defector who crossed the border into South Korea three years ago but returned to his home country, by again illegally crossing the border, earlier this month.
"An emergency event happened in Kaesong City where a runaway who went to the south three years ago, a person who is suspected to have been infected with the vicious (Corona) virus returned on Jul 19 after illegally crossing the demarcation line," the official statement of the country's state news agency KCNA read.
North Korea has till now claimed to be free of COVID-19 Pixabay
Country's response
The development has caused tremors in the North Korean administration. Yesterday, the country's leader Kim Jong Un chaired a meeting of the politburo and asked the state machinery to go all out in dealing with a possible health crisis.
As of now, there isn't clarity regarding the testing method followed for assessing the person. The news agency stated that the person's "uncertain result was made from several medical check-ups of the secretion of that person's upper respiratory organ and blood."
What's the truth?
Though the communist state is claiming that this is the first suspected case of the infection that has gripped the entire world, including the closest neighbors of North Korea, there has been widespread skepticism of the claim that the Hermit Kingdom was totally shielded from the virus.
Kim Jong Un was suspected to be suffering from Coronavirus earlier Twitter
With the country being closed to international media and known for being ultra-secretive in its manner of functioning, it is hard to make any estimations of the situation over there. Kim Jong Un has praised his country's efforts at stopping the global pandemic from reaching his country.
North Korea has been the recipient of testing kits from various countries, chiefly Russia. It has also been placing a large number of people in quarantine and imposing severe restrictions on travel in and outside the country.
Suspicious reports
Still, there is a strong suspicion that this announcement of the 'first case' may be a way for the regime to slowly accept the actual situation on the ground. The story of the person being supposedly monitored seems suspicious. A person defecting to South Korea and coming back to his poverty-stricken and tyrannically-ruled country seems very unlikely.
South Korea has not reported any illegal crossings from its side. To make a person returning from the southern nation of the Korean peninsula the carrier of the virus would also be a way for the North to maintain its claim of having been free of COVID-19.
US Election Under Cyber Threat: Notorious Russian GRU Hackers Are Targeting Government Agencies
US Names 2 Chinese Hackers on Prowl Targeting Defense Contractors, COVID-19 Vaccine Data
Why Was North Korean Leader Kim Jong Un Angry For 2 Consecutive Days?
Related topics : Coronavirus
Rachel Levine: Biden Nominates First Openly Transgender to Serve as Assistant US Health Secretary
Levine has been a role model for the transgender community in Pennsylvania...
Joe Biggs Calls Capitol Attack 'Awesome' in Viral Video, Urinates Inside the Capitol
Biggs says that he is going to turn himself in to the FBI.
BREAKING: Trump Decides to Pardon Steve Bannon Hours Before Leaving White House
News outlets say the decision is not final and that Trump has not signed...
Raunchy Couple Caught Having Sex Inside Ferris Wheel in Myrtle Beach; Videos Posted on Porn Website
Eric Harmon and Lori Harmon have posted videos of having sex at multiple...
We Built the Greatest Political Movement in US History, Trump Says in Farewell Speech (FULL TEXT)
'I want you to know that the movement we started is only just beginning.'
750 Ethiopians Hiding in Famous Aksum 'Ark of Covenant' Church Shot Dead - Report
The attacks were carried out by Ethiopian federal troops and Amhara...
Moving Trucks Spotted Outside Trump's Mar-a-Lago, Residents told Road Closure Will Last 'Several Days'
The outgoing President changed his primary residence from New York City to...
Malaysian Government Mulling Harsher Laws Against LGBTQ Community for 'Unhealthy Activities'
Malaysia's Deputy Minister Ahmad Marzuk Shaary called for stricter...
LEAKED: Trump's Unsent Four-Page Letter Firing FBI Chief James Comey Accused Him of Causing 'Near Rebellion'
The draft letter was a personal tirade against Comey which was found to be...
Does Pfizer's COVID-19 Vaccine Stop Coronavirus Transmission? Israeli Study Offers Optimistic Results
The study at Sheba Medical Center in Israel found the Pfizer-BioNTech...


text:
St St Catherine of Siena Parish-About US
To be the preferred choice of a community that lives and learns the catholic faith: a fountain for those who seek spiritual nourishment in a peaceful atmosphere, inspiring all to the love of God's Grace in a culture cordially centered in Christ.
We, the community of St. Catherine of Siena Parish- Kitisuru, in the Archdiocese of Nairobi, guided by our patroness Saint Catherine of Siena and amidst our multicultural diversity, are called to celebrate God's presence in our lives, by being prayerful and proclaiming the good news of Jesus Christ in the spirit of faith and service to all who seek shelter in our paris
Being a church in Nairobi endowed with a diverse range of international cultures, we: •Recognize and welcome our visitors individually every Sunday; •Cultivate a sense of belonging; •Promote spiritual growth; •Demonstrate love and concern; •Value inclusiveness; •Support openness; •Show transparency; and •Encourage unity.
Our Benchmarks
•Our benchmarks shall be: •Christian population on Sundays and weekdays; •Involvement of christians in the liturgy; •Iacramental dispensation; •Financial sustainability; and •Growth and sustainability of church initiatives vis a vis projects
In accordance with the Canon Law, the Finance Council is a collaborative unit which provides the Priest with advice and assistance on financial matters concerning the Church. The council is a requirement of every Church with guidelines laid out in the Archdiocesan Finance Policy document. The specific functions of the council are as follows: 1. Coordination and implementation of all aspects of accounting for the Church. 2. Drawing the Church annual budget of income and expenditure and the financial statements. 3. Helping the Church priest draw a Church inventory. 4. Helping and preparing Church accounts and presenting them to the PPC annually. 5. Making/organizing investments/fundraising respectively for the Church. 6. Advising the Church priest in matters of safeguarding Church properties and assets.
St Catherine of Siena Youth
The youth are like kinetic energy, very strong and ready to spring. If unchecked their energy can be used for the wrong reasons. If tapped and directed towards the right dimensions, the energy can be both a source of self and Church development. The youth therefore must be nurtured in the right perspective in St Catherine of Siena Church
The current membership is unlimited since some are in schools others in colleges while others at home. They leadership has the chairperson, secretary, treasurer. Meetings are held every last Sunday of the month at the Church grounds
Official opening of the new Church
© St Catherine of Siena Parish-Kitisuru,Nairobi,KENYA.


text:
Home » 4th Annual FANtasy 500 Party Rocks Columbia Club Downtown
4th Annual FANtasy 500 Party Rocks Columbia Club Downtown
May 26, 2011 by Katelyn Coyne
The Indianapolis 500 Mile Race is almost upon us. As May draws to a close, the biggest spectacle in racing takes center stage in Indianapolis sports. But before those IndyCars make a seeming endless amount of left hand turns this coming Sunday, its time to celebrate. While the more "mature" population of Indianapolis people will be walking the red carpet at the Snakepit Ball at the Indiana Roof Ballroom, Indianapolis' hip, young crowd will party it up in Indianapolis downtown as well. The 4th Annual FANtasy 500 Party takes over the Columbia Club off of Monument Circle Saturday, May 28, 2011 from 9:00 pm to 3:00 am. This star studded event is only $75.00 per person ($100 for VIP guests), which includes an open bar and hors d'oeuvres.
Hosts Catt Sadler and Carlos Diaz will pump Indianapolis people up for the impending race phenomenon in Speedway, Indiana. They take the stage at the Columbia Club this Saturday at 9 pm to lead the biggest party in racing. They will also be joined by pop super star Christina Milian. This Indianapolis event offers a swank party with famous faces, and everyone in Indianapolis is invited.
Catt Sadler is a well known personality on E!: Entertainment Television, where she hosts The Daily Ten. A Hoosier at heart, Catt graduated from Indiana University in Bloomington, Indiana with a Bachelors degree in Journalism. In fact, Sadler's first ever gig was in the movie Hoosiers at the age of 11. Soon after graduating from one of the top Indiana colleges and universitiesp, Sadler headed west to San Francisco, where she got a gig as a reporter at a local news station. She soon began co-hosting Indiana Lottery's Hoosier Millionaire and was the official emcee of the Indiana Pacers during the 2003-04 season. She also appeared on General Hospital and Night Shift, before hitting big in the entertainment comedy industry on E!
Fans of CNN have recently started signing on to there sister network HLN The "News and Views" Network. HLN viewers will recognize Carlos Diaz from HLN's "Morning Express with Robin Meade," where he serves as the Sports Anchor. This popular morning talk show digs deep into the top stories of the day, with a healthy daily dose of new, weather, sports, entertainment and finance topics. As the go to guy for sports on HLN, Diaz has sports reporting in his blood. He is a former reporter for ESPN's "Sports Center," where he cut his teeth on interviews with Michael Jordan, Tiger Woods and Indianapolis Colts' star Peyton Manning. Diaz also served as an anchor for the NBA's own television network NBA TV.
Christina Milian is a recording artist, actress, dancer and model who hit in big in 2001 with her self titled debut album. The record, which topped the charts in the United States and around the world, featured the hit singles "AM to PM" and "When You Look At Me." Since its release, Milian has recorded two other hit albums and has a fourth in the works. This musician first gained recognition at a young age with a spot on the Disney Channel's "The Mickey Mouse Club." Since then she has performed in a string of television and film including "Be Cool," "American Pie," "Pulse," and "Ghosts of Girlfriends Past."
Come party with these international celebrities at the Columbia Club in Indianapolis downtown. Before the event, take a stroll around the Soldiers' and Sailors' Monument that makes up Monument Circle. This Indianapolis event doesn't get going until relatively late. So grab dinner before hand at any of these Indianapolis restaurants. Or pre-game with drinks from any of these Indianapolis bars.
Stay tuned to FunCityFinder.com for all the latest on fun things to do in Indianapolis. We cover Indianapolis arts to Indianapolis shopping and everything in between. Get out in Indy and find some fun! Make the most of the Circle City!
4th Annual FANtasy 500 Race Party
9 pm to 3 am
Tickets: $75, VIP $100
Columbia Club
Filed Under: Downtown, News, Sports


The upcoming holiday stretch from Thanksgiving to the New Year is a busy travel time for many of us, whether driving down the road to Grandma's to celebrate with family or flying halfway around the world for a winter vacation. To help plan your getaways, we've got tips from our last #TripItChat on Twitter, which was chock full of holiday travel tips for travelers of every sensibility.
Destinations: Should I stay or should I go?
For some people, holiday travel can be a chore, but done the right way it can also be a lot of fun.
Most #TripItChat participants stay close to family over the holidays, but planning a special vacation over the holidays every now and then was also a popular choice.
@Laurberry9 says she usually stays at home for the holidays, but this year she and her family are visiting New York City for the Macy's Thanksgiving Day Parade.
Chat co-host @LeeAbbamonte was the most extreme: He's heading to Antarctica over Thanksgiving.
Despite the festive allure (and inspiration from Lee) of the North and South Poles, the most popular destinations were Christmastime trips to Europe for the markets or flying somewhere warm, like Mexico to escape the cold December winds.
One of the biggest sources of anxiety for any traveler is knowing when to book airfare to get the best deal possible. Prices on booking sites are hard to predict, leaving many of us confused and worried. Luckily we had some great experts take part in our chat and they offered fantastic advice for scoring the best holiday travel deals.
TripIt users know to always book early, then use TripIt Pro to catch price drops. This will save you both anxiety and money.
Travel expert and co-host @ThePointsGuy shared with chat participants that mid-October is actually the best time to book holiday airfare if you want to guarantee a seat at a reasonable price.
If you can hold out, co-host @MiddleSeatView advised people wait for those inevitable last minute deals that are almost always a great bargain. However, to take advantage of those, you must be patient and flexible with no definite plans in mind.
The TripIt chat participants all agreed that they love to travel over the holidays, but opinions were decidedly mixed when it came to choosing a destination. In fact, many travelers choose a climate that's the polar opposite from what they experience at home!
Cold isn't for everyone though, and many users said they use the holidays as a chance to escape the harsh elements. @NYgal33, @turnipseeds and @Breathedreamgo all say they get more than enough cold weather at home – so over the holidays, they head for the nearest sunny beach in order to relax. No matter what your preference is, both travel types can take advantage of frequent flier miles to make their holiday travel dreams a reality.
If #TripItChat participants love one thing, it's accruing (and redeeming!) frequent flier miles. When asked about end of the year tricks, the tips were flying too.
Several folks had the great idea to maximize their miles when doing holiday shopping. If you have a mileage credit card, be sure to use it when buying those expensive presents. Also try to use the online shopping portals most airlines offer to easily earn miles on gifts you're already planning to buy. If you plan ahead, you can really see those miles jump up during the holidays.
Redeeming miles is another story, and many times people find it hard to avoid blackout dates and other restrictions, especially during the holidays. Not all airlines have the same policies; if you plan ahead, you can probably find award travel even over those busy travel days. Even better, flying on the actual holiday itself is often a breeze since many travelers have already arrived at their destinations. You may be able to find some great deals and award seats on these days, especially.
Alternatively, many people decide to do some good and donate their miles to a worthy cause – especially miles that are sitting unused or approaching expiration. This year, TripIt is making that easier than ever through their miles charity drive for the Make a Wish Foundation. To learn more about this important initiative, please visit tripit.com/gift.
The one thing we all hate, especially over the holidays, is battling crowds. Whether that means spending hours in a TSA line at the airport or tripping over tourists once you arrive at your destination, no one likes to deal with a crush of humanity when they're on the road.
To avoid this, the experts once again suggested traveling on the main holiday itself if possible as the airport crowds are pretty thin.
If you're worried about too many tourists where you're going, be sure to choose off-season destinations. @SnarkyNomad suggested Europe, saying that his Christmastime experience in Italy was fantastic due to the low number of tourists. Weather in Europe in December may not be for everyone, but the cold temperatures and overcast skies keeps many away, making it the best time to see the Old World's most famous sites.
Tropical hotspots like Mexico and the Caribbean, however, are packed with travelers trying to get some holiday sun and can be overwhelming at times.
Whether or not people actually use the holidays to plan a great vacation, most of the TripIt chat participants definitely had dream holiday trips in mind. If money and time were no object, they would travel everywhere from the bottom of the world to the tops of the best ski slopes.
For @therebelchick that means Christmas in Paris, while to @redfuzzycow it's a sail to Fiji.
Several people listed Iceland as their dream holiday travel spot.
One of the best and most heartwarming answers though came from @JR_justJR who said his dream location is to have family, friends, good food and fun with him. The where doesn't matter as long as he has all of those ingredients for the perfect holiday.
Still have questions about holiday travel – and ways to make it even more special? Don't forget to join us for the next #TripItChat on November 21st, 2013 at 2:00PM Pacific/5:00PM Eastern when we will be talking about Travel Perks!


text:
<?php

namespace Recca0120\Socialite\Two;

use OAuth\Common\Token\TokenInterface;
use OAuth\OAuth2\Service\GitHub;

class GithubProvider extends AbstractService
{
    protected $scopes = [
        // GitHub::SCOPE_USER,
        GitHub::SCOPE_USER_EMAIL,
    ];

    protected function mapUserToObject(array $user)
    {
        $map = [
            'id'       => array_get($user, 'id'),
            'nickname' => array_get($user, 'login'),
            'name'     => array_get($user, 'name'),
            'email'    => array_get($user, 'email'),
            'avatar'   => array_get($user, 'avatar_url'),
        ];

        return with(new User())->setRaw($user)->map($map);
    }

    protected function getUserByToken(TokenInterface $token)
    {
        $url = 'user';
        $response = $this->request($url, 'GET', null, [
        ]);

        return json_decode($response, true);
    }
}

redpajama_set_name: RedPajamaGithub


The Euan Turner Training Fund is a rolling fund, with no application deadline. Please contact Fiona McCurdy if you have any questions.
This fund has been set up in the memory of Euan Turner, the FST's Health and Safety advisor who passed away in June 2015. The purpose of the Euan Turner Training Fund is to financially support freelance and employed technical, production and stage management personnel in the performing arts sector in Scotland, who might not otherwise be able to afford it, to undertake training for nationally recognised health and safety qualifications.
Euan spent more than 20 years in health and safety, mostly in theatres. He was known for his common-sense and accessible way of introducing health and safety in theatre and for making sure that everyone involved in a production understood their responsibilities relating to health and safety. He also understood that the costs of full H&S training can be prohibitive for freelancers and those working for smaller theatre companies. With this fund, FST would like to celebrate the memory of our dear colleague by making it easier for those people to access the training.
Please note we have recently revised the terms of eligibility and levels of funding available as part of this fund making it open to more applicants and making it more generous.
We would like to encourage organisations to recommend the Euan Turner Training Fund to freelance technical/stage management staff you regularly work with as well as considering it for your own employed staff.
We would also encourage freelance technical, production and stage management practitioners to apply.
Freelance or work as a casual member of staff in the performing arts.
Are employed full or part-time in a theatre or performing arts organisation with a turnover of under £750,000 per annum.
Additionally, employed staff in organisations with a turnover of over £750,000 can apply for a limited number of places on more advanced training courses as outlined below.
Is available for individuals who have at least 12 months professional experience in production, stage management or technical roles in the performing arts.
Training must be provided by an accredited training provider in the UK.
In order to apply for support towards attending either the NEBOSH or NCRQ courses you must hold an IOSH Managing Safely qualification and demonstrate how it would give added benefit to your work, your organisation and the wider sector – e.g. how you may share your learning with others.
As the main purpose of the fund is to enable people who would not normally be able to afford it to get their first entry-level H&S qualifications, the majority of awards will be for studying for IOSH Managing Safely. We will therefore make a limited number of awards (around 2 per annum) for study for the higher level NEBOSH or NCRQ qualifications.
FST is very grateful for the fundraising and generous donations by Euan's family and friends, FST members and performing arts colleagues in the wider sector, which have made this fund possible.


text:
\section{Introduction \label{s-intro}}

According to the accepted conviction, the universe in our neighborhood consists solely of matter, and the existence of
macroscopically large antimatter objects is fully excluded. This is in accordance with the conventional picture
that the excess of baryons over antibaryons in the Universe is generated by Sakharov's mechanism \cite{1967JETPL...5...24S}.
In models
with explicit C and CP violation, the baryon asymmetry
\begin{eqnarray}
\eta = (N_B - N_{\bar B} ) / N_\gamma \approx 6 \cdot 10^{-10}
\label{beta}
\end{eqnarray}
is a universal constant over the whole universe. Here $N_{B(\bar B)}$ are the number densities of baryons or antibaryons, and
$N_\gamma = 411/$cm$^3$ is the current number density of photons in the cosmic microwave background (CMB) radiation.

If the charge symmetry is broken spontaneously, then domains of matter and antimatter may exist but the size of domains
is expected to be cosmologically large, at the Gigaparsec level  \cite{1998ApJ...495..539C}.
Therefore, the accepted faith is that if even
macroscopically large objects or regions consisting of antimatter exist, they should be far away from us at the edge
of the universe or at least at distances beyond 10 Mpc \cite{1976ARA&A..14..339S}.

On the other hand, about a quarter of a century ago, a physical mechanism was suggested leading to the possible formation of compact
antistars over normal matter-dominated background \cite{1993PhRvD..47.4244D, 2009NuPhB.807..229D}.
According to the proposed scenario, the baryogenesis
in the bulk of the universe proceeded in the usual way giving rise to the observed small baryon asymmetry (\ref{beta}),
while in a small by volume part of the universe, bubbles with a very high baryonic number  (called HBB) might be created.
The model allows for the formation of HBBs with both signs of the baryon asymmetry, positive (matter) and negative (antimatter). HBBs
with a size comparable to the cosmological horizon at the QCD (quantum chromodynamics) phase transition at $T\sim 100$~MeV  mostly give rise to primordial black holes (PBHs) which could make a sizeable fraction (if not all) of cosmological dark matter. Such PBHs could have masses in a wide range from a fraction to thousands of solar masses \cite{2016JCAP...11..036B,2020JCAP...07..063D}.
Of course, there is no noticeable difference between a PBH and an anti-PBH.

Smaller HBBs could form
compact stars or antistars.  They would be created in the very early universe after the QCD  phase
transition at $T \sim 100 $ MeV. Probably, they can be now observed as peculiar stars in the Galaxy: too old stars, very fast-moving stars,
and stars with a highly unusual chemical content \cite{2004PThPh.112..971M,2005PhRvD..72l3505M,2020PhRvD.102b3503A}, for a review see \cite{2018PhyU...61..115D}.
They should also populate the galactic
halo. The fraction of these strange stars and/or antistars among the stellar population is model-dependent but may be quite high.

The possibility of the existence of a population of antistars in the Galaxy and observational limits on their density were analyzed
in several papers \cite{2007NuPhB.784..132B,2014JETPL..98..519D,2014PhRvD..89b1301D,2015PhRvD..92b3516B}.
It was concluded that quite a noticeable fraction
of antistars relative to ordinary stars is not excluded by the present observations.
As discussed in detail in ref. \cite{2015PhRvD..92b3516B}, the restrictive limits derived for the ''normal'' antistars from gamma-ray background (e.g. \cite{2014HyInt.228..100V})  are
not applicable for antistars produced in scenarios \cite{1993PhRvD..47.4244D}-\cite{2014PhRvD..89b1301D}, and such antimatter objects may abundantly populate the Galaxy without contradicting the gamma-ray background limits.

Recently, the idea that antistars may be our Galactic neighbors attracted new attention. In ref.
\cite{2020PhLB..80735574S},
it was suggested
that cosmological dark matter could entirely consist of macroscopic antimatter objects and in ref.
\cite{2021PhRvD.103h3016D}
a possible indication to antistars in the Galaxy based on gamma-ray  \textit{Fermi}/LAT measurements was reported. Quoting the latter paper:
``We identify in the catalog 14 antistar candidates not associated with any objects belonging to established gamma-ray source classes and with a spectrum compatible with baryon-antibaryon annihilation.''

In this paper, we propose
a new signature tagging electromagnetic signal from annihilation in outer layers of antistars. The idea is to search for antistars in the Galaxy through X-rays in the  $\sim(1-10)$ keV energy band. This X-ray radiation is expected to be produced  in the process of the cascade transition
from bound states of antiproton-proton (protonium) or antihelium-proton atoms before $p \bar p$-annihilation and must accompany the gamma-ray radiation from the annihilation.

Note that the \textit{Fermi} candidate antistars are not true stars but large regions in the sky plane (of order tens angular minutes in diameter corresponding to \textit{Fermi}/LAT gamma-ray error boxes) comprising a huge number of stars. Obviously, not only antistars but also objects consisting of ordinary matter can be sources of gamma-quanta with energies above 100 MeV. Therefore, the objects showing the X-ray signature proposed in our paper will lead to an unambiguous indication of their antimatter nature and much better localization if they are detected in future observations.

\section{Line emissions from protonium decays}

Usually, the antimatter objects are being looked for through the
search for energetic photons with energies of hundreds MeV from $\pi^0$ decays into two $\gamma-$quanta,
with $\pi^0$ emerging from $p \bar p$ - annihilation.
The energy spectrum of such photons is shown in Fig.\ref{f:anncrosssec}. This spectrum was calculated by Geant4\footnote{{\tt version Geant4.10.06 (06.12.2019); https://geant4.web.cern.ch}}
\cite{Allison:2006ve} simulation of the low-energy antiproton annihilation in a small liquid hydrogen target.
The spectrum suggests that
the mean energy radiated in gamma-rays per one annihilation is $\Delta E_\gamma=617.5$~MeV. The mean number of $\gamma$-quanta per one annihilation is $\langle N_\gamma\rangle=4.12$ with the mean number of $\gamma-$quanta above 100 MeV is $\langle N_\gamma\rangle(>100 \mathrm{MeV})=2.63$ per event. Note that the target's material and structure do not significantly affect the annihilation spectrum which is appropriate for the considered problem.

However, before annihilation, protons and antiprotons could form atomic-type excited bound states (`protonium', Pn), similar to $e^+e^-$-positronium (Ps) atoms.
One could expect that in the process of de-excitation of Pn, an antistar could emit not only $\sim 100$-MeV gamma-rays but a noticeable flux of X-rays with energies in the keV range.

Let us briefly remind the basic physics of $p\bar p$ annihilation through a protonium state (see, e.g, \cite{2002PhR...368..119K} for a comprehensive review).
A protonium atom can form during the interaction of a $p$ with neutral (or molecular) antimatter. In the ionized matter-antimatter interaction, the annihilation mainly proceeds through the direct hadronic channel, the cross-section of the radiative recombination of a Pn atom formation from the $p\bar p$ interaction being $(m_e/m_p)^{3/2}\approx 10^{-5}$ times smaller (see \cite{1976ARA&A..14..339S}  for the matter-antimatter annihilation cross-sections).
\begin{figure}
    \centering
    \includegraphics[width=\textwidth]{p+p-toGamma_1.pdf}
    \caption{Gamma-ray spectrum from hadronic $p\bar H$ annihilation. The mean number of $\gamma$-quanta per event is $<N_\gamma>=4.12$. The mean number of $\gamma-$quanta above 100 MeV is 2.63 per event. The mean energy radiated in gamma-rays per one annihilation is $\Delta E_\gamma=617.5$~MeV. Calculations by Geant4 code.}
    \label{f:anncrosssec}
\end{figure}

A Pn atom forms when a proton (antiproton) interacts with an anti-hydrogen (hydrogen) atom, $\bar p+H\to (p,\bar p)+e^-$. The formation of a Pn atom effectively occurs when the energy of the proton in the lab frame is below the electron's ionization threshold in atomic hydrogen, $E=1$Ry$\simeq 13.6$ eV. At lower proton energies, the cross-section increases as $\sim 1/\sqrt{E}$ \cite{2005PhRvA..71e2717O}.
Therefore, in the present paper, we will mainly focus on astrophysical situations where the antistar's atmosphere (or its stellar wind) is neutral or interacts with the neutral interstellar medium (ISM).

The fraction of energy from the bolometric luminosity released in X-ray from the Pn cascades (the cascade yield),
$f_\mathrm{X}=L_\mathrm{X}(Pn)/L_a$, depends on the pressure \cite{1989NuPhA.503..885R}. However, an upper limit on the bolometric X-ray yield per unit cascade can be estimated as the binding energy of a Pn atom, $\approx 12.5$~keV (ignoring small QED corrections $\mathcal{O}(\alpha^2)$). Therefore, the maximum X-ray yield per one Pn atom is $R_{p\bar p}=(1/4) \alpha^2m_pc^2=12.5$ keV ($\alpha$ is the fine structure constant, $m_p$ is proton's mass). As the cascade time of a Pn atom is very short \cite{1989NuPhA.503..885R}, in rarefied media the X-ray luminosity in X-ray lines will be determined by the formation rate of Pn atoms, $\dot N_a$:
$L_\mathrm{X}\le 12.5\,\mathrm{keV}\times \dot N_a $, i.e. the maximum possible X-ray fraction in the Pn-cascade during matter-antimatter annihilation is $f_\mathrm{X,max}=\alpha^2/8\approx 6.7\times 10^{-6}$.

The line energies for the K (Lyman) $2p\to 1s$, L (Balmer) $3 d \to  2p$ and M (Paschen) $4f\to 3d$ transitions in a Pn atom are 9409 eV, 1737 eV and 607 eV, respectively. Calculations of the X-ray line yields from the Pn decays produced in $p\bar H$ interactions at low densities \cite{1990PhRvA..41.3460C} suggest that most intensive X-ray lines should be Balmer (L) lines (up to 97\%), the 2p-states of the $p\bar p$ atom being rapidly annihilated.
The produced X-ray line width is determined by the $p\bar p$ annihilation from the 2p-state and is about $\Delta E\sim \mathcal{O}(0.1$~eV) (see the discussion and experimental measurements in  \cite{2002PhR...368..119K}).
As the total energy released in gamma-rays during $p\bar H$ annihilation is about 617 MeV (see Fig. \ref{f:anncrosssec}), the expected fraction of X-ray line emission flux from one Pn annihilation is $f_\mathrm{X,H}\approx0.95\times (1.7\, \mathrm{keV}/617.5\,\mathrm{MeV})\approx 2.5\times 10^{-6}$, i.e. a factor of three lower than the simple estimate given above.

\section{keV X-ray emission from protonium cascades in Galactic antistar candidates\label{s-galactic}}

Presently, it is difficult to reliably assess the number and physical parameters of antistars in the Galaxy. Estimates in paper \cite{2020PhRvD.102b3503A} are model-dependent and based on the assumption that gamma-ray emission from hadronic annihilation occurs in the putative antistar candidates during Bondi-Hoyle-Littleton accretion of the interstellar gas.
It is straightforward to estimate the expected X-ray flux associated with the gamma-ray annihilation emission in the case where the $p\bar p$ annihilation was preceded by the protonium formation.

A crude estimate of the X-ray flux emitted in 1.7-keV narrow line from the gamma-ray sources -- candidates to antistars found from \textit{Fermi} 10-year LAT catalogue in ref. \cite{2021PhRvD.103h3016D} is:
\beq{e:fermi}
  F_\mathrm{X}(1.7\,\mathrm{keV})\sim f_\mathrm{X,H}\times F_\gamma (0.1-100\,\mathrm{GeV})\approx  10^{-17}[\mathrm{erg\,cm^{-2}s^{-1}}] \myfrac{F_\gamma(0.1-100\mathrm{\,GeV})}{4\times 10^{-12}\mathrm{erg\,cm^{-2}s^{-1}}}

\end{equation}
(see Table \ref{tab:sources_specs} for individual candidates).
This low flux is unlikely to be uncovered with the current instrumentation even with the stacked detection strategy.

The forthcoming JAXA/NASA XRISM (X-Ray Imaging and Spectroscopy Mission) telescope will be able to provide a 5-4 eV resolution in the 0.3-12 keV energy range \cite{2018_XRISM}. The expected effective area of the \textit{Resolve} spectrometer is $\sim 210$~cm$^2$ \footnote{{\tt https://xrism.isas.jaxa.jp/research/documents/index.html}}. For approximately $10^6$~s observations, only a few 1.7-keV photons from a source with an X-ray flux of $\sim 3\times 10^{-17}$~erg cm$^2$ s$^{-1}$ can be collected.
A more promising could be measurements from the ATHENA X-IFU X-ray spectrometer which is expected to have a spectral resolution of $\sim 2$~eV and an effective area of $\sim 8000$ cm$^2$ in the keV range \cite{2016SPIE.9905E..2FB,2020AN....341..224B}.
The 1.7 keV Balmer line of protonium falls within the sensitivity limit of the advanced-technology Lynx X-ray Observatory \cite{2019JATIS...5b1001G}, which will be able to measure X-ray fluxes down to $\sim 10^{-19}$~erg cm$^2$ s$^{-1}$ with an angular resolution of better than $\sim 1''$. While the X-ray line fluxes of the individual source candidates estimated in Table \ref{tab:sources_specs} are below the expected sensitivity of the XRISM telescope one may try to search for antistars through stacked source detection in serendipitous surveys of the next generation X-ray observatories. In this case, the appropriate choice of the antistar candidates can be made from the unidentified \textit{Fermi} source sample.

Note also that the most prominent 1.7-keV X-ray line from Pn decay in antistars should not interfere with other X-ray emission lines expected from stars. As no real stellar antistar counterparts have been identified inside large \textit{Fermi} error boxes, it is reasonable to compare real \textit{Chandra} X-ray spectra from different stars. For example, observations of solar-type dwarfs show that at energies around 2 keV only MgXII ($\lambda = 8.421$ \AA $\approx 1.46$~keV) emission is visible in spectra of young star EK Dra, the older stars demonstrating no visible emissions \cite{2010PNAS..107.7158T}. A giant binary nearby (about 13 pc) star Capella  \cite{2007A&A...461..679R} used for the grating observations calibration \cite{2003ARA&A..41..291P} demonstrates a rich variety of coronal X-ray lines, with MgXII and SiXIV ($\lambda = 6.182$ \AA $\approx 1.99$~keV) around 2 keV. Therefore, the possible 1.7 keV emission from a solar-type dwarf antistar and even an evolved anti-giant is unlikely to interfere with stellar coronal X-ray lines from highly ionized species.

\begin{table*}
\centering
\caption{\label{tab:sources_specs}
Estimate of possible Pn X-ray flux $F_X$ from 4FGL \textit{Fermi} antistar candidates. Energy flux $F_\gamma$ (0.1-100) GeV from \cite{2021PhRvD.103h3016D}.}
\begin{tabular}{lcc}
\hline
\hline
 Name              & $F_\gamma$ (0.1 - 100 GeV) & $F_X$ (1.7 keV) \\
 &   erg cm$^{-2}$ s$^{-1}$ & erg cm$^{-2}$ s$^{-1}$  \\
\hline
 4FGL J0548.6+1200 & $(4.2\pm 0.9) \times 10^{-12}$ & $\sim 1\times 10^{-17}$ \\
 4FGL J0948.0-3859 & $(2.5\pm 0.7) \times 10^{-12}$ & $\sim 6.3\times 10^{-18}$  \\
 4FGL J1112.0+1021 & $(2.5\pm 0.5) \times 10^{-12}$ & $\sim 6.3\times 10^{-18}$  \\
 4FGL J1232.1+5953 & $(1.8\pm 0.3) \times 10^{-12}$ & $\sim 4.5\times 10^{-18}$ \\
 4FGL J1348.5-8700 & $(3.0\pm 0.6) \times 10^{-12}$ & $\sim 7.5\times 10^{-18}$ \\
 4FGL J1710.8+1135 & $(2.5\pm 0.6) \times 10^{-12}$ & $\sim 6.3\times 10^{-18}$ \\
 4FGL J1721.4+2529 & $(3.3\pm 0.5) \times 10^{-12}$ & $\sim 8.3\times 10^{-18}$  \\
 4FGL J1756.3+0236 & $(4.4\pm 1.0) \times 10^{-12}$ & $\sim 1.1\times 10^{-17}$ \\
 4FGL J1759.0-0107 & $(5.9\pm 1.3) \times 10^{-12}$ & $\sim 1.5\times 10^{-17}$\\
 4FGL J1806.2-1347 & $(9.4\pm 2.2) \times 10^{-12}$ & $\sim 2.4\times 10^{-17}$ \\
 4FGL J2029.1-3050 & $(2.6\pm 0.6) \times 10^{-12}$ & $\sim 6.5\times 10^{-18}$ \\
 4FGL J2047.5+4356 & $(1.4\pm 0.4) \times 10^{-11}$ & $\sim 3.5\times 10^{-17}$ \\
 4FGL J2237.6-5126 & $(2.3\pm 0.5) \times 10^{-12}$ & $\sim 5.8\times 10^{-18}$ \\
 4FGL J2330.5-2445 & $(1.6\pm 0.4) \times 10^{-12}$ & $\sim 4.0\times 10^{-18}$\\
 \hline
\end{tabular}
\end{table*}

\section{Associated $e^+e^-$ emission and optical lines}

During the formation of a Pn atom from the interaction of a proton with $\bar H$ in the upper atmosphere of an antistar, a slow positron $e^+$ is ejected. It should form a positronium $e^+e^-$ atom in the surrounding medium before annihilation. Since during the Pn cascade transitions and annihilation, on average, three gamma-quanta with energy $E_\gamma\approx 200$~MeV are created per 600 MeV \textbf{(see Fig. 1)}, the accompanying $e^+e^-$ annihilation flux from the \textit{Fermi} antistar candidates is expected to be:
\beq{e:e+e-}
\left.\frac{dN}{dAdt}\right|_\mathrm{e^+e^-}\approx 2\times\frac{1}{3}\left.\frac{dN}{dAdt}\right|_{\gamma}\approx  6\times10^{-9}\frac{\mathrm{ph}}{\mathrm{cm^2s}}
\myfrac{F_\gamma(0.1-100\mathrm{\,GeV})}{3\times 10^{-12}\mathrm{erg\,cm^{-2}s^{-1}}}\myfrac{200\mathrm{\,MeV}}{E_\gamma}\,.
\end{equation}
(The factor 2 above is due to at least two photons are emitted in the Ps annihilation).
This is much smaller than the current 511~keV detection capabilities \cite{2016A&A...586A..84S}.

Other possible traces of the Pn atom cascade decays could be searched for in the optical-UV range. Indeed, a Pn bound state is expected to be formed highly excited, $n\gtrsim 30$ \cite{2002PhR...368..119K}.  The Pn energy levels are
\beq{}
E_n\approx -\frac{12.5}{n^2}\mathrm{keV}\approx -13.9 \,\mathrm{eV}\myfrac{30}{n}^2\,,
\end{equation}
and the cascade transitions $(n,l=n-1)\to (n-1,l-2)$ pass through the optical-UV range: $\Delta E_n\approx 0.93\,\mathrm{eV}\myfrac{30}{n}^3$.
The spacing of the optical lines is $\Delta E/E=\Delta \lambda/\lambda=2/n$ is much larger than their expected Doppler width, which could be their distinctive feature.
Clearly, the number of quanta in an optical emission line from the \textit{Fermi} antistar candidates should be approximately equal to the number of Pn atoms, therefore
$
\left.\frac{dN}{dAdt}\right|_\mathrm{opt}\approx  \left.\frac{dN}{dAdt}\right|_{\gamma}\approx 3\times 10^{-9}\frac{\mathrm{ph}}{\mathrm{cm^2s}}\,.
$

For a NIR line at $\lambda = 4\mu \mathrm{m}$ with Doppler width $\Delta\lambda/\lambda=3\times 10^{-6}$ this photon flux corresponds to m$_\mathrm{AB}\sim 24.3^\mathrm{m}$ magnitude. While well within the rich by modern telescopes (e.g., JWST\footnote{{\tt https://www.stsci.edu/jwst/science-planning/proposal-planning-toolbox/sensitivity-and-saturation-limits}}), this flux in emission line is too small to be distinguishable on the background of stellar photons (for example, a solar-type star at a distance of 10 kpc would have m$_{AB}(4\mu \mathrm{m})\approx 18^\mathrm{m}$ \cite{2018ApJS..236...47W}). Therefore, the measurement of such weak emission lines is challenging and requires a dedicated technique (for example, the use of stellar coronographs to shield the stellar light, e.g. like the coronograph to be installed on the Nancy Grace Roman Space Telescope\footnote{{\tt https://roman.gsfc.nasa.gov/coronagraph.html}}).

\section{Helium-antiproton and antihelium-proton cascade X-ray lines from antistars}

Enhanced production of helium and metals is an important feature of the non-standard nucleosynthesis in HBBs with high $\eta$ \cite{2004PThPh.112..971M,2005PhRvD..72l3505M,2020PhRvD.102b3503A}. Therefore, it is instructive to consider the X-ray lines arising from cascade decays of $^4\bar{\mathrm{He}}p$ and $^4$He${{\bar p}}$ atoms that can be created in the interaction of ISM with antistars. The possible AMS-02 detection of non-thermal antihelium-4 nuclei\footnote{S. Ting, Latest Results from the AMS Experiment on the International Space Station (2018)}
may indicate the presence of antistars in the Galaxy because its secondary production in the universe is challenging (see, e.g., the discussion in \cite{2019PhRvD..99b3016P}). Note that the magnetically active antistars may accelerate antihelium nuclei in stellar flares.

In a $^4$He$\bar p$ atom, the hadronic annihilation starts dominating the cascade transitions already at the third level. The $^4$He $\bar p$ atom transitions series M (4-3) at 4.86 keV [yield (57 $\pm 3)\%$] and  L (3-2) 11.13 keV [yield (25 $\pm 5)\%$] \cite{1991ZPhyA.338..217S} are certainly of interest given that the forthcoming X-ray spectroscopic mission \textit{XRISM} \cite{2020arXiv200304962X} is sensitive in 0.3-12 keV energy range.
A simple estimate of the fractional flux in these lines relative to the annihilation gamma-ray flux can be done in the same way as for $p\bar{p}$ decays presented in the end of Section 2:  $f_\mathrm{X,He}(4.86\mathrm{keV})\approx0.57\times (4.86\, \mathrm{keV}/617.5\,\mathrm{MeV})\approx 4.5\times 10^{-6}$, $f_\mathrm{X,He}(11.3\mathrm{keV})\approx0.25\times (11.3\, \mathrm{keV}/617.5\,\mathrm{MeV})\approx 4.6\times 10^{-6}$, i.e. about twice as high as for $p\bar{p}$ decay X-ray lines. These estimates depend on the assumed He abundance, and for the solar He abundance must be decreased accordingly. However, they are around the same as for $f_\mathrm{X,H}$.
These lines can be even more important from the observational viewpoint because the protonium $p\bar p$ 3d-2p transition line energy 1.73 keV is close to the detector's Si K-shell complex lines and, therefore, a high energy resolution is needed to distinguish the lines.
Note also that in a hot medium with ionized hydrogen, when protonium atoms will not be formed, even a small mixture of He$^+$ ions would give rise to the effective (with atomic cross-sections) formation of He$\bar p$ atoms. Then only $^4$He$\bar p$ cascade X-ray lines will be produced.

A dedicated search for $^4$He$\bar p$ 4.86 keV and 11.13 keV lines in all-sky surveys like \textit{Spectrum-RG} \cite{2021arXiv210413267S} could also constrain the collective contribution of X-ray emission from antistars with enhanced He abundance.

Like in the case of antiprotonium, $^4$He$\bar p$ atoms are formed at excited levels with principal numbers $28<n<35$. After an antiproton is captured, the remaining electron is rapidly ejected due to the internal Auger effect, and the process of ion ($^4$He$\bar p$)$^+$ radiative deexcitation begins along the circular sequence from $n\sim 30$ \cite{1988PhLB..203....9R}. Neglecting the strong interaction shift, the energy between consequent levels is
\beq{}
\Delta E_n\approx 3.72 \mathrm{eV} \myfrac{30}{n}^2\frac{2n-1}{(n-1)^2},
\end{equation}
and these lines can be probed in the optical range too.

\section{Possible astrophysical sources}

As shown above, it is challenging to test the Pn formation before hadronic annihilation in the   \textit{Fermi} Galactic antistar candidates. However, there could be favorable astrophysical conditions for the Pn creation from the interaction of hypothetical antistars with ISM.

Consider first an antistar with mass $M$ and the standard (solar) abundance residing in the Galactic ISM with density $\rho_0$ (or number density $n_0$) and moving with the velocity $v$. There can be distinct cases of the star's interaction with ISM depending on the evolutionary state of the antistar (main-sequence or evolved) and its space velocity.

If the star is on the main sequence and has an insignificant mass loss via stellar wind, the interaction with ISM will be characterized by the gravitationally
captured mass-rate (the Bondi-Hoyle-Littleton accretion). The relevant physical scale is the Bondi radius,
\begin{equation}
    \label{e:RB}
    R_B=\frac{2GM}{(v^2+c_s^2)}
\end{equation}
where $v$ and $c_s$ is the star's velocity and ISM sound speed, respectively, $G$ is the Newtonian gravitational constant. The Bondi mass accretion rate is
\begin{equation}
    \label{e:dotMB}
    \dot M_B=\pi R_B^2 \rho_0\sqrt{v^2+c_s^2}
\end{equation}

If a star has significant proper mass-loss rate $\dot M_w$, the interaction with ISM will be characterized by the radius $R_w$, where the dynamical pressure of the stellar wind  is balanced by the ISM pressure, $\rho_w v_w^2\sim \rho_0c_s^2$:
\begin{equation}
    \label{e:Rw}
    R_w=\sqrt{\frac{\dot M_w (v_w/c_s)}{4\pi \rho_0 c_s}}
\end{equation}
If $R_w>R_B$, the ISM accretion is insignificant and the stellar wind directly interacts with ISM. In our estimates, we will consider the standard galactic ISM with particle number density $n_0\sim 1$ cm$^{-1}$ (corresponding to a density of $\rho\sim 10^{-24}$ g cm$^{-3}$) and sound velocity $c_\mathrm{ISM}\sim 1$~km s$^{-1}$. The interaction with such an ISM depends on the stellar space velocity $v$ and stellar wind mass-loss rate $\dot M_w$. We will consider four different cases: an antistar with or without stellar wind and typical galactic disk dispersion velocity $v\sim 10$ km s$^{-1}$ or halo velocity $v\sim 10^{-3}c$ ($c$ is the speed of light), summarized in Table \ref{tab:table}. Note that in both cases stellar velocities are supersonic.

\begin{table}[]
    \centering
    \caption{Possible cases of interaction with ISM of an antistar with velocity $v$ and wind mass-loss rate $\dot M_w$ (see text). The last column shows expected X-ray flux from Pn cascade transitions from a Galactic antistar at 1 kpc. }
    \label{tab:table}
    \begin{tabular}{lcccc}
    \hline\hline
          Velocity   & Stellar wind & Gamma-ray annihilation & Pn cascade X-ray& X-ray flux, $d=1$ kpc\\
    of antistar&  $\dot M_w$ [$M_\odot$~yr$^{-1}$] & luminosity, $L_a [\mathrm{erg\, s^{-1}}]$ & luminosity, $L_X [\mathrm{erg\, s^{-1}}]$ & $F_X [\mathrm{erg\,cm^{-2} s^{-1}}]$\\
    \hline
     $10$ km s$^{-1}$ &  $\approx 0$  & $\sim 10^{32}$ & $\lesssim 2.5\times 10^{26}$ &$\lesssim 2.5\times 10^{-18}$\\
         10 km s$^{-1}$ &  $\approx 10^{-10}$ & $\sim 4\times 10^{36} \dot M_{w,-10}$ & $\lesssim  10^{31}\dot M_{w,-10}$ & $\lesssim  10^{-13}\dot M_{w,-10}$ \\
         $10^{-3} c $ & $\approx 0$ & $\sim 0$ & $\sim 0$\\
         $10^{-3} c $ & $\approx 10^{-10}$ & $\sim 4\times10^{36} \dot M_{w,-10}$ & $\lesssim  10^{31}\dot M_{w,-10}$ & $\lesssim  10^{-13}\dot M_{w,-10}$  \\
         \hline
    \end{tabular}
\end{table}

\begin{enumerate}
    \item Low-velocity  case, $v\sim 10$~km s$^{-1}$,
    weak stellar wind\footnote{Solar wind mass-loss rate is  $\sim 10^{-14} M_\odot$ per year.}, $\dot M_w\approx 0$.

    In this case, the Bondi radius is $R_B\approx 2\times 10^{14}[\mathrm{cm}] m v_6^{-2}\approx 2.7\times 10^3 R_\odot v_6^{-2}$ (here $m\equiv (M/M_\odot)$, $v_6\equiv v/(10^6\mathrm{cm\, s^{-1}})$, $R_\odot \approx 7\times 10^{10}$~cm is the solar radius). The BHL accretion rate from ISM onto such a star is $\dot M_B\approx 1.8\times 10^{11}[\mathrm{g\, s^{-1}}]m^2v_6^{-3}$. The total annihilation rate is thus $\dot N_a\sim 10^{35}\mathrm{s}^{-1}$, and the bolometric annihilation luminosity is \textbf{$L_a\sim 617\,\mathrm{MeV}\times \dot N_a\sim  10^{32}\mathrm{erg\,s^{-1}}$}. The maximum possible Pn-cascade X-ray luminosity is then
    $L_\mathrm{X}=f_{\mathrm{X,H}}\times L_a\approx 2.5\times 10^{26}[\mathrm{erg\, s^{-1}}]m^2v_6^{-3}$.

        \item Low-velocity case, $v\sim 10$~km s$^{-1}$, moderate stellar wind $\dot M_w\approx 10^{-10} M_\odot$~yr$^{-1}$. The wind terminal velocity is about the ISM sound speed, no strong shock is formed.

In this case, $R_w\approx 7 \times 10^{16}\mathrm{[cm]}\dot M_{w,-10}^{1/2}n_0^{-1/2}(v_w/c_s)^{1/2}\gg R_B$. Here $\dot M_{w,-10}\equiv \dot M_w/(10^{-10} M_\odot$~yr$^{-1})$. The cross-section of Pn formation under these conditions is about $10^{-16}$~cm$^2$ \cite{2005PhRvA..71e2717O}.
    The formation of Pn states occurs in a layer with a width of $\sim 1/(n_0\sigma)\sim 10^{16}\mathrm{cm} < R_w$. The Pn formation rate is $\dot N_a=\dot M_w/m_p\sim 4\times 10^{39}M_{w,-10} \,\mathrm{s^{-1}}$ suggesting  a bolometric annihilation gamma-ray luminosity of $L_a\sim 4\times 10^{36} [\mathrm{erg\, s^{-1}}]\dot M_{w,-10}$. The Pn-cascade X-ray luminosity is $L_\mathrm{X}\lesssim  10^{31}[\mathrm{erg\, s^{-1}}]\dot M_{w,-10}$.

    \item High-velocity case, $v\sim 10^{-3}c$, weak stellar wind $\dot M_w\simeq 0$.

    This case is more relevant if antistars populate the Galactic halo and move with the halo virial velocities $v\sim 10^{-3} c$.    In this case, the Bondi radius is very small, $R_B\sim 4 R_\odot v_{-3}^{-2}$ (here $v_{-3}=10^{-3}(v/c)$), the BHL accretion is inefficient, $\dot M_B\sim 10^7 [\mathrm{g\, s^{-1}}]m^2n_0v_{-3}^{-3}$, the associated annihilation luminosity is very weak.

    \item High-velocity case, $v\sim 10^{-3}c$, moderate stellar wind, $\dot M_w\simeq 10^{-10} M_\odot$~yr$^{-1}$.

    If an antistar with stellar wind moves with the Galactic virial velocity through ISM, a strong bow shock is formed ahead of the star. The matter behind the shock front is fully ionized.
    The front shock radius is estimated from the dynamical wind pressure balance: $R_{sh}=\sqrt{\dot M v_w/(4\pi \rho_0 v^2)}\simeq 7 \times 10^{16}\mathrm{[cm]}\dot M_{-10}^{1/2}\rho_{-24}^{-1/2}v_{-3}^{-1/2}(v_w/v)^{1/2}$, where
    $\rho_{-24}=\rho/(10^{-24}\mathrm{g\,cm^{-3}})$ is the ISM density. For slow winds expected from red giants $v_w/v\sim 3\times 10^{-5}$, and the shock radius is $R_{sh}\sim 4\times 10^{14}\mathrm{[cm]}\dot M_{-10}^{1/2}\gg R_B$.

    This case is more complicated than the interaction of a cold slow stellar wind with ISM. The energy of protons downstream the shock is $E_p=(3/16) m_pv^2\sim 170$~eV.
    $\sigma\sim 10^{-23}$~cm$^2$ \cite{1976ARA&A..14..339S}, and the protons penetrate much deeper into the stellar wind before annihilating through the hadronic channel.
    The cross-section of the Pn formation strongly depends on the proton's energy and below $\sim$~1 Ry~$=13.6$~eV sharply increases up to a few $\times 10^{-16}$~cm$^2$.

    However, the hot protons rapidly loose energy by interacting with neutral stellar wind. The proton stopping length in hydrogen is [M.J. Berger et al. 1993 ICRU Report 49]
    \begin{equation}
    \label{e:lp}
        l=\frac{E_p}{dE_p/dx}=\frac{E_p}{4\pi r_e^2 m_ec^2\beta_p^{-2}(\rho_w/m_p) L(\beta_p)}
    \end{equation}
    Here $\beta_p=v_p/c=3/4(v/c)\sim 10^{-3}$ is the proton's downstream thermal velocity, $L(\beta_p)$ is the proton's stopping number. For low proton  energies, it can be evaluated only from experiments, and is dominated by nuclear scatterings. For an estimate of the stopping length of slow protons, we can use the ionization energy loss of slow protons in electron gas $L(\beta_p)\approx \log(2m_ev^2/\hbar\omega_0)$, where $\omega_0\approx 5.6\times 10^4\sqrt{n_e}$~rad s$^{-1}$ is the electron plasma frequency \cite{Lindgard54}. For the assumed parameters, $L(\beta_p)\sim \mathcal{O}(10)$.

   It is convenient to recast equation (\ref{e:lp}) in the form
   $$
   l=\frac{1}{n_0\sigma_T L(\beta_p)}\myfrac{1}{3}\myfrac{m_p}{m_e}
   \myfrac{v_w}{v}^2\beta_p^4
   $$
   ($\sigma_T=(8\pi/3) r_e^2$ is the Thomson cross section). Then
  $l\lesssim 10^{11}\mathrm{[cm]} (\beta_p/10^{-3})^2(v_w/10\, \mathrm{km\, s}^{-1})^2$, which is much smaller than the shock front radius $R_{sh}\sim 4\times 10^{14}$~cm. Therefore, the ISM protons are expected to form Pn atoms inside the wind in analogy with the low-velocity case considered above.
\end{enumerate}

If a typical antistar has an atmosphere like that of our Sun, then modelling by Kurucz's ATLAS code\footnote{http://kurucz.harvard.edu/programs.html} shows that the bulk of proton annihilations takes place in essentially neutral plasma. Then the data on antiproton annihilations in laboratory neutral media is quite applicable for proton annihilations in Solar-like atmospheres of antistars. Different possible atmospheric structures of antistars or their coronas deserve a special investigation.

Also note that at advanced evolutionary stages, antistars can experience a huge mass-loss, $\dot M_w\sim 10^{-6} M_\odot$ yr$^{-1}$, for a short time (e.g., at the asymptotic giant branch). In this case, as seen from Table \ref{tab:table}, the annihilation luminosity can reach $10^{40}$ erg s$^{-1}$, comparable to the gamma-ray emission of the entire galaxy. Presently, this is definitely not the case in our Galaxy, but if antistars are sufficiently abundant, there can appear a bright extragalactic gamma-ray and X-ray source. Future sensitive instruments can probe this possibility.

\section{Constraints from electron-positron  annihilations}

The interaction of an antistar with ISM should be necessarily accompanied by electron-positron annihilation. Therefore, the existing observations of the $e^+e^-$ Galactic emission should be taken into account when constraining the possible Galactic antistar populations.

The characteristic 511 keV annihilation radiation from the Milky Way was discovered about 50 years ago in balloon-borne experiments. Since then it has been measured by many space missions (for a review, see \citep{2011RvMP...83.1001P,2020NewAR..9001548C}). The recent analysis of {\sl INTEGRAL SPI} Ge detector data \citep{2016A&A...586A..84S} has confirmed the presence of the main extended 511 keV components with a total significance of about 58 $\sigma$. The 511 keV fluxes estimations depend on the models of the extended Galactic emission. The total 511 keV flux from the Milky Way was estimated to be  $(2.74 \pm 0.25) \times 10^{-3}$ ph cm$^{-2}$ s$^{-1}$. The bulge component contributed about $(0.96 \pm 0.07) \times 10^{-3}$ ph cm$^{-2}$, and the 511 keV flux ratio of the bulge to disk components was derived to be $(0.58 \pm 0.13)$.

The total 511 keV Galactic disk emission suggests an annihilation flux of $F_\mathrm{e^+e^-}\sim 2\times 10^{-3}$ cm$^{-2}$ s$^{-1}$.
For a fiducial distance of 10 kpc this rate corresponds to a total
positron production $\dot N_\mathrm{e^+e^-}\sim 10^{43}$~s$^{-1}$. If all positrons were formed in Pn
$p\bar p$ annihilations in a purely hydrogen matter, the upper limit on the protonium production rate would be $\dot N_\mathrm{Pn}\sim  10^{43}$~s$^{-1}$, corresponding to  $\sim 2\times 10^{-7} M_\odot$~yr$^{-1}$. Therefore, an antistar with higher wind mass-loss rate is excluded by the $e^+e^-$ Galactic emission.

Recently, ref. \cite{2021arXiv210903791S} reported an improved \textit{INTEGRAL} upper limit on the 511-keV flux from the Galactic satellite dwarf galaxy Ret II of
$F_{511}<1.7\times 10^{-4}$ ph cm$^{-2}$ s$^{-1}$.
Given a distance of 30 kpc to this galaxy, this flux is translated to an $e^+e^-$ annihilation rate of about $\dot N_\mathrm{e^+e^-}\sim 10^{43}$ s$^{-1}$, comparable to the detected Galactic value.  The gamma-ray flux in the GeV range measured by Fermi-LAT from Ret II galaxy is inconclusive \cite{2020JCAP...02..012H}. The authors \cite{2021arXiv210903791S} do not exclude the 511 keV flux variability on a decade-long time-scale. In the frame of the astrophysical models discussed above (i.e., the interaction
of antistars with ISM), the $e^+e^-$-flux variability might be due to the intrinsically variable stellar wind mass-loss rate.

\section{Conclusions}

Antistars in the universe can be created in
the modified Affleck-Dine baryogenesis mechanism \cite{1993PhRvD..47.4244D, 2009NuPhB.807..229D}.
Presently, they could be observed as old halo stars with unusual chemical composition.

In the present paper, we explored the possibility that the interaction of antistars with ISM gas can proceed with the formation of excited protonium atoms which rapidly cascade down before hadronic annihilation from 2p-states.
The formation of Pn atoms most effectively occurs during the interaction of protons with neutral (or molecular) antimatter. This can happen if an antistar has a noticeable wind mass loss.
We considered the case where, in analogy with ordinary stars, antistars in the mass range from $\sim 0.8$ to $8 M_\odot$ at the end of their core nuclear burning can have cold low-velocity stellar winds  $\sim 10^{-8}-10^{-5} M_\odot$~yr$^{-1}$ \cite{1995A&A...297..727B,2008A&A...487..645R} (AGB antistars).
The interaction of cold stellar winds from antistars with ISM can proceed through the formation of excited protonium $(p\bar p$) atoms. The protonium atoms cascade to the 2p-state producing mostly L (Balmer) 3d-2p X-rays around $\sim 1.7$~keV before the $p\bar p$ hadronic annihilation.

Antistars formed in HBBs should have an enhanced helium abundance. Therefore, the 4.86 keV M (4-3) and 11.13 L (3-2) narrow X-ray lines from cascade transitions in $^4$He$\bar p$ atoms can also be associated with gamma-rays from hadronic annihilations. These lines are interesting from the observational point of view because
the protonium 3d-2p transition line energy 1.73 keV is close to the Si K-shell complex lines, which could hamper disentangling it from the background.

The expected Pn-decay X-ray line flux from individual Galactic \textit{Fermi} antistar candidates reported in \cite{2021PhRvD.103h3016D} is estimated to be much lower than the sensitivity of current X-ray detectors. However, searches for the cascade X-ray transitions from Pn and $^4$He$\bar p$ atoms associated with hadronic  annihilation gamma-rays can be exciting targets for the forthcoming X-ray spectroscopic missions like
\textit{XRISM}, \textit{Athena} and \textit{\textit{Lynx}}.
Sensitive wide-field X-ray surveys can also help to constrain the collective contribution of antistars in the universe.

\section*{Acknowledgement}
The authors thank the anonymous referee for careful reading of the paper and suggestions for improving the presentation of the results.
We are grateful to Andrey Sokolov for help in simulating the gamma-ray spectrum from hadronic $p\bar H$ annihilation.
The work of AD was supported by the RSF Grant 19-42-02004.
SB acknowledges the support of RSF Grant 19-12-00229 in his work on stellar atmospheres. The work of KAP is supported by the Ministry of Science and Higher Education of the Russian Federation under contract 075-15-2020-778 (astrophysical appearance of antistars).

\providecommand{\href}[2]{#2}\begingroup\raggedright

redpajama_set_name: RedPajamaArXiv


Coming in a gunmetal grey, these boots are a great addition to any winter outfit. The upper is made from a soft leather and with an open zip style on either side of the boot with elastic, these boots are extremely easy to slide on and off! Also comes with a textile lining to keep your feet warm throughout winter!


Where to Buy' Slim Quick Keto : Weight Loss Diet Pills, (Store)!
1.1 What is Slim Quick Keto?
1.3 Why do you have to use this product?
1.4 What area unit the advantages of Slim Quick Keto?
1.8 Where to Purchase Slim Quick Keto?
Weight decrease is on name today and so packs of individuals realize the right upgrade on the online these days which supplies anchored and real results. Slim Quick Keto is another weight reduce before condition which is able to do strategy to revamp the patient ingestion routine development within the body regarding emotional that fat doing fighting the pointless sugars and starch grouping within the body.
This improvement may be a ketogenic eat less carbs which is able to permit mishandling your spatial relation levels and muscle versus fat degree thus you may simply shed pounds and obtain an ideal body form that you legitimatise. these days underground travel diaries area unit arduous primarily in context of its surface properties since it doesn't hurt your interior organ and temperament. It simply targets wedged zones wherever enough fat is secured and unharness it helpfully through that you may ne'er feel any uneasiness and dangerousness.
Slim Quick Keto Reviews has sturdy upgrades thus you don't ought to worry regarding its responses. it's a typical upgrade which is able to modification over your starches into an important spatial relation level. This upgrade can check your longing and can assemble the age of BHB that is faithful lose fat and rising your general temperament. after, it's right by and by time to state bye to your daring fat and categorical welcome to your hot body form.
It is a unique quite weight loss supplement then that claimed by others for it uses basic ingredients for its effectiveness. it's conjointly safe for its shoppers while not the presence of adulteration or chemicals which may cause you to skeptical. It not solely brings speedy weight loss however conjointly helps you build your muscle mass.
Slim Quick Keto contains Beta-hydroxybutyrate. BHB is that the essential substrate that kicks the metabolic state of acetonemia energetically. returning to the circumstance from already, just in case you either take supplemental structures or if your body is creating beta-hydroxybutyrate, it will begin handling in your body realizing imperativeness.
Beta-hydroxybutyrate floats around in your blood, and primarily, will cross clear indispensable limits to own the flexibility to be became essentiality dependably. A champion among the foremost imperative areas wherever this happens is within the neural structure. The blood-cerebrum limit (BBB) is frequently a solidly coordinated interface, anyway since BHB is such diving being consequently hydrophilic , your mind is aware of to convey it get to thus it will die essentiality to the assemblage at no matter purpose. this is often one in all the essential reasons why extended BHB levels provoke swollen mental insight.
Why do you have to use this product?
Improved mental power, with further energy our brain won't suffer the fatigue, we'll be ready to do away with the mental fogginess, and it actually will facilitate in boosting the standard of life.
No negative reaction, here you're not aiming to suffer any adverse reaction. All due to the natural ingredients that area unit added with nice accuracy and when careful experimentations. this is often a secure product.
Proven results, as we tend to saw that almost all people that used Slim Quick Keto had gotten the goose results. So, you may not be associate degree exception. You 2 area unit aiming to thin.
What area unit the advantages of Slim Quick Keto?
Energy Booster: It is true that Slim Quick Keto goes to burn the fat which fat is employed for the assembly of energy. Moreover, as we tend to aren't diet and ingestion pour the correct food, you're aiming to expertise a surge within the energy and power. this is often natural with this pill, and it's aiming to assist you keep active and alert.
Boosted Mental Acuity: The aspect effects of additional energy aren't simply the strength, however our brain is a smaller amount doubtless to suffer from fatigue, and it's aiming to helps North American country in deciding and keeping North American country recent feeling all day long.
Rapid Weight Loss: The process of weight loss with the merchandise is incredibly fast, as you recognize that Slim Quick Keto Diet goes to burn the fat directly. You don't need to stay up for the starvation. So, as we tend to skip a number of steps here, we tend to area unit aiming to get fast results.
Always use a sealed pack delivered to your step.
Do not use if you're on medication before consulting with a doctor.
Though it's made from all-natural ingredients, however if you face any allergies please consult a MD.
Keep yourself hydrous and nourished.
It is a replacement supplement thus until currently there haven't been any problems with aspect effects and it's not been tested a lot of, so, you must bear in mind.
Do not use it for youngsters below eighteen years or for pregnant and nursing ladies.
Where to Purchase Slim Quick Keto?
If you have got unwanted fat in pestiferous districts and you're unbelievably curious to get rid of it from your body then Slim Quick Keto Pills sweetening is for you. you'll be able to purchase this weight decrease formula from the official website. every and each basic detail is presently documented on the location. simply in a very tick your weight decrease supplement are asked for and sent to you in 2-3 days.
We know that victimization any weight loss supplement is straightforward, same goes for slender fast Keto likewise. However, we all know that this is often the supplement that's aiming to facilitate with simple and healthy weight loss and it's aiming to assist you boost energy power and no aspect effects. we tend to believe that you just should provide this product a strive before you begin taking this pill.
you'll have to have to play max coins to kick the jackpot feature.
and follow your ki (life energy), the endeavor is effortless.
Once your teen masters one habit and demonstrates that success is possible, s/he can go onto the next one.
Check the payback before playing, and make certain you get the best payback to be able to play.
Thanks for sharing your thoughts on maryland live casino your account.
to pay a visit this web page, it includes precious Information.
Hola! I've been reading your web site for some time now and finally got the courage to go ahead and give you a shout out from Houston Tx!
The popular US musical TV show titled "Glee" has recently made an episode that is a tribute to Lady Gag and her songs.
totally, however this article offers fastidious understanding even.
helⅼo!,I really likke your writing vеry so much!
share we communicate more aboսt yoսr article оn AOL?
my problem. MayƄe that's you! Taking a look ahead tо looҝ yⲟu.
What i don't realize is actually how you're not actually much more well-liked than you may be right now. You're so intelligent. You realize thus considerably relating to this subject, produced me personally consider it from numerous varied angles. Its like women and men aren't fascinated unless it's one thing to do with Lady gaga! Your own stuffs nice. Always maintain it up!
nice Keep up the wonderfull work!


JULIA SMEAD: I describe our practices for the Benedictine Gathering here in the interview. Our schedule is that the group gathers about 6 p.m. in the church for a chanted service of Vespers, a meal, study of one chapter of the Rule of St. Benedict, and chanted Compline.
For years, the group met without hands-on clergy. Recently Fr. Jonathan Duncan has become a regular attendee, giving the group welcome instruction in proper Gregorian Chant.
After our parish finished its new building we now meet at my church and we chant!
Litany is chanted with incense.
Now as a group, we've purchased real dinner plates. This is an opportunity to do our best to the glory of God.
and read to the group during the meal.
Following the last prayer at Compline there is asperges (sprinkling with Holy Water. The practice of asperges -- often done at Mass -- is a common Benedictine monastic practice at the end of Compline) as individuals enter the Great Silence that governs the nighttime hours.
Live in the Dallas-Fort Worth area? Anyone interested in experiencing the Benedictine traditions is welcome to join this ad hoc community for its monthly gathering. Send your RSVP to breadforthejourney@sbcglobal.net.


text:
The Four Paladins () are the four legendary generals in the fellowship of King Anawrahta during the Bagan Dynasty. They are one of the most famous national heroes of Burma and played significant roles in the early tales of the Bagan Empire's expansion. In Burmese legends, each of them is said to be equivalent to the combined might of a legion.

Members

 Kyansittha (ကျန်စစ်သား) — Paragon of both physical and mental strength
 Nga Htwe Yu (ငထွေရူး) —  Paragon of agility
 Nga Lon Letpe (ငလုံးလက်ဖယ်) — Paragon of might
 Nyaung-U Hpi (ညောင်ဦးဖီး) — Paragon of stamina

Mission to Pegu
The mission to Pegu is the most famous episode in the military career of the paladins. In the early 1070s, the king of Pegu made a distress call to Bagan when his kingdom is invaded by the Yuan-Khmer raiders called 'Joom' (ဂျွမ်း) from Norther Thailand. King Anawrahta promised that he would send a relief cavalry of four legions to defend Lower Burma. The Peguan king waited hopefully for the mighty Bagan Imperial army, but disappointed with the arrival of only the Four Paladins and a few platoons. However, in front of all the people of Pegu, the warriors of Bagan easily repelled the invaders in just one day. They also took the four Joom generals( Aukbraran, Aukbrare, Aukbrabon, and Aukbrapike) captive, and presented them to the king of Pegu. The Peguan ruler, pleased by the legendary valor of the paladins, sent his young daughter Khin U, jewels and holy hair relics as tributes and gifts for Anawrahta.

However, unknown to them, the return journey to Bagan will eventually lead to the dissolution of their friendships and the squad of the Paladins.

References

Asian mythology
Burmese folklore

redpajama_set_name: RedPajamaWikipedia


PLUS REALTY - USAG Humphreys & Osan AB area.
to resolving maintenance issues and even assisting with utility payments.
We're confident that we can help make your tour in Korea a comfortable one!
So come in and challenge us today!
And remember, PLUS REALTY is at your service.
USAG Humphreys & Osan AB area.
Camp Humphreys 2,064 sqf. KRW1,600,000.
Copyright ⓒ NEXTBIZ INC. All rights reserved.


text:
Q: Why is my if function closing my batch file? Whenever I activate this code it instantly closes the console.
set RAND=%RANDOM% %%100
if %RAND% gtr '25'

I want it to keep running if the if is false or go to an alternative location if it is true.

A: Two lines of code - four problems
set RAND=%RANDOM% %%100
if %RAND% gtr '25'

First, to set a variable to the result of a calculation, you need set /a. As it stands, rand would be set to 12345 %100 - a string (one % because % escapes %)
Your second line would then be invoked as
if 12345 %100 gtr '25'

which violates the if syntax - the %100 would confuse it as it expects a comparison operator (==, equ, neq, gtr, lss, leq, geq) in that position so it will generate an error message and stop. If you're running using point, click and giggle then the window will instantly close. You need to run batch programs from the command prompt while debugging.
Next problem is that 25 is never going to be equal to '25' - the quotes are part of the string being compared. put them on both sides or omit them from both sides. Batch only uses strings - the set /a syntax understands and controls the conversion operations required to change from string to numeric representation (integers only) and the if will attempt to convert arguments to numeric for comparison - on failure of either side, if reverts to a string-comparison.
And finally, you've not provided if with anything to do should the comparison have evaluated to true - which is another violation of the if structure.

A: Put pause at the end of the file... Pause doesn't allow the batch file to close unless you press a key (like Spacebar).
@echo off
cls
echo This is just an example
pause
exit

redpajama_set_name: RedPajamaStackExchange