text:
Miami Heat: News, Schedule, Roster, Score, Injury Report
The Miami Heat, owned by Micky Arison, is part of the NBA's Eastern Conference. They belong to the Southeast Division along with the Atlanta Hawks, Charlotte Hornets, Washington Wizards, and Orlando Magic.
The Miami Heat entered the NBA in 1988 as an expansion team along with the Charlotte Hornets. They reached the Playoffs only twice in the first eight years, but fell in the first round on both occasions.
In the 1995 season, they were acquired by Carnival Cruise Lines and saw a turnaround in fortunes. In the next season, they reached the Conference Finals, following Michael Jordan's Chicago Bulls. En route, they cobbled up a 32-9 way record, earning them the moniker "Road Warriors."
The Miami Heat constantly fell to the New York Knicks in the Playoffs between 1998-2000, before dropping off until the acquisition of Dwyane Wade in 2003. They made four consecutive Playoffs and won their maiden NBA title in 2006. A year later they were swept in the first playoff series.
This was the beginning of a slump in their fortunes. The team notched up an abysmal 15-67 league record in 2007-08. They made the Playoffs again in the next 2 years but didn't achieve success until the formation of the Big 3 in 2010.
Miami Heat used the $48 million cap space and recruited LeBron James and Chris Bosh. They reached four consecutive finals and won two championships in 2012 and 2013.
After LeBron James' departure, they made the Playoffs just twice. In the first year, the Miami Heat became the first team since the 2005 season's Los Angeles Lakers to miss out on the Playoffs after featuring in the previous final.
LeBron James (2012, 2013) is the only Miami Heat player to win the league MVP award. The legendary Pat Riley currently serves as the president of the Heat, while Erik Spoelstra has been the trusted head coach since 2008.
Team's Sponsors
The Miami Heat have Ultimate Software as their main sponsors, who also advertise on their uniforms. Besides, the technology company, Miami has partnerships with companies such as Tissot, Dell, and several other companies.
Achievements and History
Conference Eastern
Division Southeast
President Pat Riley
General Manager Andy Elisburg
Head Coach Erik Spoelstra
Arena American Airlines Arena
Championships (3) (2006, 2012, 2013)
Conference Titles (5) (2006, 2011, 2012, 2013, 2014)
Division Titles (14) (1997, 1998, 1999, 2000, 2005, 2006, 2007, 2011, 2012, 2013, 2014, 2016, 2018, 2020)
Website www.nba.com/heat
Miami Heat Current Roster
Pos. No. Name Height Weight DOB (YYYY-MM-DD)
F/C 13 Adebayo, Bam 6 ft 9 in (2.06 m) 255 lb (116 kg) 1997–07–18
F/C 17 Alexander, Kyle (TW) 6 ft 10 in (2.08 m) 216 lb (98 kg) 1996–10–21
F 22 Butler, Jimmy 6 ft 7 in (2.01 m) 230 lb (104 kg) 1989–09–14
F 99 Crowder, Jae 6 ft 6 in (1.98 m) 235 lb (107 kg) 1990–07–06
G 7 Dragić, Goran 6 ft 3 in (1.91 m) 190 lb (86 kg) 1986–05–06
F 40 Haslem, Udonis 6 ft 8 in (2.03 m) 235 lb (107 kg) 1980–06–09
G 14 Herro, Tyler 6 ft 5 in (1.96 m) 195 lb (88 kg) 2000-01-20
F 44 Hill, Solomon 6 ft 6 in (1.98 m) 226 lb (103 kg) 1991–03–18
G/F 28 Iguodala, Andre 6 ft 6 in (1.98 m) 215 lb (98 kg) 1984–01–28
F 5 Jones, Derrick 6 ft 6 in (1.98 m) 210 lb (95 kg) 1997–02–15
F/C 0 Leonard, Meyers 7 ft 0 in (2.13 m) 260 lb (118 kg) 1992–02–27
G 25 Nunn, Kendrick 6 ft 2 in (1.88 m) 190 lb (86 kg) 1995–08–03
G/F 4 Okpala, KZ 6 ft 8 in (2.03 m) 215 lb (98 kg) 1999–04–28
F/C 9 Olynyk, Kelly 6 ft 11 in (2.11 m) 240 lb (109 kg) 1991–04–19
F 55 Robinson, Duncan 6 ft 7 in (2.01 m) 215 lb (98 kg) 1994–04–22
F 30 Silva, Chris 6 ft 8 in (2.03 m) 234 lb (106 kg) 1996–09–19
G 2 Vincent, Gabe (TW) 6 ft 3 in (1.91 m) 200 lb (91 kg) 1996–06–14
Jimmy Butler Finally Reveals the Mystery Behind His Popular Meme
WATCH: 76ers' Joel Embiid Mocks Miami Heat by Urging Them to Take a Timeout During Blowout Win
Will Joel Embiid and Ben Simmons Play Tonight? Miami Heat vs Philadelphia 76ers: Injury updates, Expected Lineups, and Game Prediction
'Are You Seeing This?' – Heat's Duncan Robinson Shares Hilarious Reaction from His Mother to Trade Rumors About Him
'Shut Up And Put On Your Mask': Heat's Duncan Robinson Shares an Unheard Story About Fred VanVleet
Joel Embiid Matches a 32-YO Rare Franchise Record in the Sixers' Win Over Miami Heat
Will Ben Simmons Play Tonight? Philadelphia 76ers vs Miami Heat: Injury Updates, Lineups, and Game Prediction
WATCH: LeBron James' Crazy Angry Moments and On-Court Fights
Miami Heat Look in Serious Trouble Thanks to NBA's COVID Protocols
NBA Trade Rumors: 3 Teams That Can Save Bradley Beal from the Washington Wizards
How Did Thomas Bryant Get hurt, Details of his Injury & What Does it Mean For Washington Wizards?
'Playing Dumb and Lazy'- Jimmy Butler Unhappy With Miami Heat's Early Defensive Struggles
Will Bradley Beal Play Tonight? Miami Heat vs Washington Wizards: Injury Update, Lineup and Game Prediction
'Jimmy Hated Miami': Dwyane Wade Reveals How He Influenced Jimmy Butler to Join the Heat
Jimmy Butler Disappointed with Miami Heat Not Playing Hard
"They Won't Let Michael Jordan Into the Club..": When the NBA Legend Was Embarrassed at Dwayne Wade's Party
Giannis Antetokounmpo Reveals Why He Re-Signed with the Milwaukee Bucks
Duncan Robinson Leaves Behind Luka Doncic and Damian Lillard in Incredible Three-Point Record
Will Jimmy Butler Play Tonight? Miami Heat vs Boston Celtics: Injury Reports, Lineups, and Predictions
'May Need Some of that Oxigen Water'- D-Wade's Hilarious Request to Steph Curry After his Recent Splendid Showing
Will Jimmy Butler Play Tonight? Miami Heat vs Oklahoma City Thunder: Injury Updates, Lineup and Prediction
NBA Champion Evaluates LeBron James, Rajon Rondo, and Others On a Unique Scale
Udonis Haslem Gives a Befitting Response Over Claims of Dirk Nowitzki Hating LeBron James & Miami Heat
Will Luka Doncic Play Tonight? Chicago Bulls vs Dallas Mavericks Injury Report, Lineup & Predictions
Dwyane Wade Endorses Tyler Herro After His Stunning Performance Against Milwaukee Bucks
Mavericks' Luka Doncic Jokes About Making Profit with His $50,000 Rookie Card
'Dirk Lost It'- Former Mavericks Champion Reveals Hilarious Post Part Stories from 2011
Watch: Luka Doncic Sends Bam Adebayo Back to Miami With Crazy Footwork
WATCH: Mavericks' Luka Doncic Takes Out His Frustration on Advertisement Banners During Win Against Heat
Will Kristaps Porzingis Play Tonight? Dallas Mavericks vs Miami Heat: Injury Updates, Expected Lineups, and Game Prediction


text:
Holy☆Hearts!
ActionComedyFantasy
Kyuno, who's aiming to become a Sister, just became a Sister-in-training, and started her dormitory life with Ginger and Alicia, aiming to be the same, however... (Source: SCX-Scans)
Messiah: Seiiki Ishuu
MysteryShoujo
In the fifth unit of the special police bureau lies a group of special individuals known as the "Sakura." Formed for the purpose of carrying out secret missions, they gave up their nationality, erased their past and concealed their real identities. There will be no salvation for the "Sakura" who failed in his mission, except for their one and only "Messiah"—the only existence that can pull them back from the path of death…
Kiss wa Naisho ni
When Ayumi's dad remarried, he brought home not only a new mom for Ayumi, but an older brother too! Takeru's handsome, nice, and really popular with the girls. So popular that his phone never stops ringing! Ayumi can't help but be bothered by his popularity, but if he's a player why should Ayumi care? Isn't it wrong for siblings to have those kinds of feelings for one another? (Source: MU)
Berry Dynamite
The comedy story follows Mai and Kurumi—two polar opposites who act friendly onstage as the hit singing duo "Star Berry," but bicker offstage. What Mai really wants to become is a rock singer, but the easily flustered Kurumi would rather sing idol songs. (Source: MU)
End of Eternity: The Secret Hours
ActionAdventureSci-Fi
In a world called Barzel exists a particular profession called Private Military Firms or more commonly known as PMFs. They take on any particular job ranging from stealing to security as long as the price is right. Lynbell, Zephyr and Vashyron joined alliances to take on jobs and have been doing decently even in this highly competitive and cut throat industry. However, lately, there has been a mysterious figure who has always been one step ahead of them, taking their jobs and keeping them from making money. And now, it seems that person is their new client. (Source:MU)
Wabisabi
1. Wabisabi 2. Futari no Sotsugyoushiki 3. Tsuki no Shita no Miyabi-chan 4. Yawaraka na Yoru 5. Kinou, Konna Yume wo Mita 6. Sweet Memories 2011 7. Koi wa Shian no Hoka 8. Yumemiru Toki ga Sugitemo 9. Renai Kinshi Kenpou 10. Ano Ko no Shitekurenakatta Koto 11. Ganbaru Hito wo Ouen suru Hito. 12. Zutto Zutto
CODE:RED
Akuma ni Chic x Hack
DemonsFantasyRomance
The "fantasy love story" follows a young demon princess who falls in love with a human boy. As a young girl, the princess met the young boy and couldn't forget him. After she grows up she descends to Earth and meets him again. (Source: ANN)
Sora ni Taiyou ga Aru Kagiri
Rieko Edogawa is a second year student at East Edogawa Academy - a private school. She is full of energy and courage, and she is so popular that there is not a soul in her town or school that doesn't know her. But Rieko's one weakness is Teppei Sakamiya, her childhood friend. She has liked him for a long time, but Teppei can only see her as a good friend. Meanwhile... Naoto Akutsu, a transfer student, appears... (Source: ShoujoMagic)

redpajama_set_name: RedPajamaCommonCrawl


text:
About Us » Journey So far (Achievements)
Drishtee's journey
Drishtee started its journey as a technology solution provider in the year 2000, bringing services offered by the government at the doorstep of the villagers. The model pioneered an ICT revolution in the country which was later carried forward by the Government as the Common Service Center (CSC) model. The modest start, in a remote central Indian district of Dhar, has yielded more than 150,000 similar centers across rural Indian subcontinent, Africa and South east Asia.
However, villages in India continued to face a basic sustainability challenge, forcing migration of members of families to cities in search of livelihood. We understood from the rural communities that the spirit of entrepreneurship, which had been their mainstay of livelihood generation, was slowly dying. This slow death was partly due to the subsidy culture adopted by the Government but the major reason was the absence of supply chain. As cities grew, markets retreated and became more sophisticated. To confront this challenge, Drishtee reorganized itself to be an efficient last mile distribution network in 2007. It took us nearly 4 years and innumerable failures to become an effective last mile for the rural stores. But the plan was to become the most preferred first mile out of the village as well. While, the community cries for access to market, we realized that their output was not market ready. There was shortage of skills needed to effectively compete in the urban market.
In 2012, we launched an integrated approach for lasting impact. We called it the 4 C approach – Community, Capacity, Capital and Channel. We started moving forward by engaging deeply with rural communities and making them co-owners in all our initiatives. It was they who guided us to identify their skills and gaps. We launched a separate organisation, DSDC (Drishtee Skill Development Center) focused on training rural youth in rural skills such as textile, agriculture and construction. With support of Government and GIF, we fist started training in textiles. Today, that effort with continued unflinching support from GIF has resulted in a producer's organisation, DRAP, which aims to break even in terms of its operational expense within the coming financial year. Similarly, the initial training in organic and smart farming techniques resulted in an experimental model by the name of Madhukrishi. Gharaunda is a an example of innovative rural housing. While, a portion of the trained candidates have so far been utilized to develop model enterprises, we are also providing trained candidates to small corporate and social entities who are working in the related sectors. In the case of agriculture, we aim to train and place men and women as agriculture extension workers. These young (would be ) master farmers come from the poorest families and general tend to go back to become change agents in their own villages, after working for a few years in local agriculture organisations.
Apart from capacity gaps, community needed access to bank linkage and easy access to capital. Way back in 2012, there were merely 10% of Indians having a bank account. In rural areas nearly 96% were unbanked. Drishtee partnered with the largest bank in India, State Bank of India, to start e-banking kiosks. There are several other organisations who partnered with different banks which has today resulted in a complete turnaround. Today, less than 40% of rural India remains unbanked. The technology enabled platform not just provides for opening of bank accounts but all other financial services such as credit, savings, insurance, remittance etc. Drishtee presently has trained and setup 1600 customer service points across 6 states. Overall, 2.3 Million bank accounts have been opened. We are aiming to work towards 100% banking coverage by the end of 2020.
Drishtee has traveled some distance in its 16 year journey. Each step has had several challenges and many failures. But this journey could not have been as enjoyable had it not been for the support of millions of rural families and several like minded partners, who have joined us and walked alongwith us in complete trust.


I'm drawn to ads on TV that are creatively thought out. Ads that weren't simply put together because some focus group said they liked the color blue, but rather ads that give you something to think about along with promoting the product.
In a nutshell? I love ads that don't "dumb it down" for the television viewing audience. I realize ads are a necessary interruption of whatever program I've chosen to watch. I find it refreshing when an ad comes along that is original, that I don't mind seeing more than once.
This 30-second Toyota Venza ad (click above to watch it), put together by Saatchi & Saatchi, is fantastic but maybe not for the reasons Saatchi & Saatchi had hoped. When looking up this ad, I searched using several phrases to find it on YouTube, and only then did I discover the ad was for Toyota Venza. You see, the ad was memorable, but not the name of the vehicle…at least to me.
So why is this ad great? Because it thoroughly pokes fun at Facebook users that basically do their "living" on Facebook rather than in real life. And with over 955 million users on Facebook (source), most everyone can relate to this ad. Yes, I'm on Facebook, but for so many reasons I have a love-hate relationship with Facebook.
1) the girl saying she read an article – well actually "just the majority of an article." We've all either been guilty of saying this, or have had things shared with us from others who have said this. This was spot on!
2) the girl talking out loud about the size of the puppy she's looking at on her computer (no doubt an image that one of her friends posted on Facebook). Again, simply spot on because it references that part of "social sharing" that doesn't necessarily better us with knowledge. It's just a tiny puppy. But we have to share it with each other online because it is cute. Again, we are all guilty of this, especially me every time I share a picture of my cats.
This ad makes me smile each time I see it on television.
Bravo to Saatchi & Saatchi!
Have you seen this ad? Do you like it? Love it? Indifferent?
PS – Nobody asked me to talk about this ad. I have no relationship whatsoever with either Toyota or Saatchi & Saatchi. This is simply me sharing what I like.
Ha Ha this is a good one! And what a great idea to post about the standout commercials1 i must say some days I like the commercials better than the shows. The bottom line is if you can get me to hit rewind on my DVR to watch a commercial it's a good one!


Burke Brown's recent designs includes work with the Metropolitan Museum of Art, Mabou Mines, Rattlestick Playwrights Theater, Ars Nova, NYSF-Public Theater, Apollo Theater and the Baryshnikov Arts Center. His work has been presented at the Joyce Theater, Kennedy Center, Lincoln Center, New York City Center, Yerba Buena Center and across North America, Europe and Russia.
His regional work includes work at Center Stage, Cleveland Playhouse, Magic Theatre, Northern Stage, Asolo Repertory Theatre, Two River Theater Company, and Playmakers Repertory Company.
His international work includes productions at the Abbey Theatre in Dublin, the Golden Mask Festival in Moscow, the Seoul Performing Arts Festival in South Korea, the Festival of Two Worlds in Spoleto, Italy, Erratica in London and the Bayerisches Staatsballett in Munich.
Recent dance design includes work with English National Ballet, Alvin Ailey American Dance Theater, Ailey II, Parsons Dance, Hubbard Street Dance Chicago, Houston Ballet, St. Louis Ballet, Kansas City Ballet, Compañia Nacional de Danza (Mexico), and Aszure Barton & Artists.
Mr. Brown volunteers with the 52nd Street Project and is the Director of Wingspace Theatrical Design Professional Mentorship Program.
Mr. Brown has a Bachelors of Arts in International Studies and Theater Studies from Guilford College in Greensboro, NC. He received his Masters of Fine Arts from the Yale School of Drama. Originally from North Carolina, Burke Brown has lived in Beijing, Miami, New Haven and Brooklyn. His current whereabouts are unknown.


Decoded 50ml e liquid – Big Foot.
Flavours of Donuts, Cinnamon and Sugar. Big Foot eliquid is the taste of the bakery in a bottle. With a mini donut flavour that has a buttery pastry taste, sprinkled with brown sugar. It evolves with every vape taking on sweeter notes as time passes. You'll be hunting down another bottle before you know it.


In its technical committees, the Technical Division Engineering and Operation of Automated Systems deals with selected current topics along the value chain, the lifetime cycle and the operational axis stretching from the field level to the management level of measurement and automation equipment. Within the "Engineering" division, they deal with the individual engineering phases from blueprint to commissioning, such as planning, programming, testing, commissioning and documentation, and in particular with the software tools used there. Of special significance are the safety aspects, which have found their way into Standards such as VDI/VDE 2180. The subject areas monitoring, diagnosis, asset management and process control are dealt with in the "Operation" division.
Cooperation with other associations such as NAMUR are of great importance in this technical division.


Alex Austerberry, formerly of the Saracens Sports Foundation and men's academy, leaving his RFU post to take the reins from Rob Cain. Good to see us building talent in all areas - hopefully he can build on the brilliant season last time round and bring another trophy home in 2019!
Edited 1 time(s). Last edit at 02/08/2018 13:13 by Barty II.
I'd heard that there were even folks from overseas showing an interest in becoming the Coach.
Yeah from my understanding we were quite surprised at the volume of candidates. Says a lot for how it's been run, and the closer ties between the lads & lasses.
Good to have Alex back home again. Another returning to the fold. Great news all round.
A fearsome all female tribe roaming North London....or an episode from Game of Thrones?
Forget to mention.....seems like another good appointment by Saracens!
The (on-field) good news keeps on rolling in.


Finding different ways to save can be tough, however, we want to encourage you to stay on track and jumpstart your finances. With these fun money challenges, you can motivate yourself to become the savvy saver we know you can be!
Instead of changing your spending habits overnight, try this challenge. Over the course of the year, you'll have a grand slam total of $1,378. Start by putting one dollar in a jar the Monday of week number one. Increase it by a dollar each consecutive week to watch your savings grow. This means week two will get two dollars, then up to fifty-two on the last week. Instead of using a jar, keep your money safe by opening a savings account with Axiom Bank!
Those extra coins and dollar bills can add up in a hurry if you let them. Have your partner add to the stash as well to increase the amount saved. You can let this fund go towards a trip or that new couch you've wanted. Challenging yourself to add to it every day, whether it's a few leftover pennies or a couple dollar bills, will keep you engaged in your game.
Track every single expense, even if it's just a quarter. Try starting out with thirty days and lengthen the amount of days you track as time goes on. When you see what you spend on, you'll notice the items you can do without. Categorizing necessities against luxuries is a big step in deciding what you will continue to put cash towards. The AxiomGO app offers a built-in budgeting tool, My $ Manager, that allows you to set spending limits by category and helps you track your expenses.
Eating out can put a dent in your wallet – and fast! Challenge yourself to eat at home for 30 days. You can find healthier recipes to test out and try new foods. Look up different money saving recipes online. Dining in can be a great way to spend quality time with your kids or loved one.
These money challenges have been tried and tested to help all types of savers. Put some of these ideas into action to grow your account. Once you have some cash to stash away, our savings accounts can help you have an accessible, safe place to put your new-found funds. Stop in one of our branches today or contact us to discuss your options!


recommended for up to 2,500 sq.ft.
recommended for up to 4,000 sq.ft.
One of the best ways to attract the highest number of potential buyers to your listing!
Aerial stills and property videos.
Show the specific layout of the home as viewed from above.
1, 2, and 4 sided Generic Feature Sheet Layouts.
We add your info and supply you with a print ready file.
Additional Images added to any tour package.
Virtual Tour uploaded following photo-shoot.
Return to property for twilight photography.
Photograph property on weekend or public holiday.
Your Tour: Its Interactive! Change the order of your images, title them, add a property description, change the music, add different season images, Google Analytics and more!


text:
Liechtenstein's LGT goes live with Avaloq Banking Suite in Austria
The Avaloq Banking Suite is now available in Austria: The Austrian unit of LGT, the international private banking and asset management group owned by the Princely House of Liechtenstein, has gone live with the Avaloq Banking Suite. The roll-out complements similar activation projects for LGT with Avaloq in Liechtenstein, Switzerland, Singapore and Hong Kong. All of the group's core strategic markets now use the same banking system.
LGT is a leading financial services group that has been fully controlled by the Liechtenstein Princely Family for over 80 years. By introducing the Avaloq Banking Suite, LGT has strengthened its client-centric sales and service model. The solution allows a comprehensive 360-degree view of client activities and enables a much quicker time-to-market for new products.
The solution addresses market needs specific to Austria, such as the local tax system and current and future financial regulations. This means that the bank's advisers automatically meet regulatory requirements. The going live marks the market entry of Avaloq in Austria. Its scalable solution is now also available to other private as well as retail banks.
Jürg Hunziker, CEO of Avaloq, said: "We are delighted that LGT has further extended its significant relationship with Avaloq with the successful implementation of our solution in Austria. When a customer extends a relationship in this way, it underscores the depth and strength of our proposition in helping banks to truly transform their processes through new digital opportunities and market-leading technologies. Avaloq is now able to support Austrian banks as the sector increasingly looks to digitise its infrastructure."
Dietmar Baumgartner, Co-CEO of LGT in Austria, added: "The integration of Austria into LGT's Group-wide core banking system makes it possible to benefit from synergies and further simplifies internal processes. The harmonization of the banking software also facilitates the introduction of new applications in the future. Austria is a key jurisdiction for LGT and we are delighted that we have now finalised the implementation phase of the solution in this growing market."


Virginie Castaway is about a lifestyle inpired by beauty and a spiritual energy. Australia is where Virginie found inspiration in har art and balance in herself. Sydney was the place that Virginie Castaway was born.
if Virginie could describe the personality of her designs in a few words, it would be - stylish, sensual, confident and romantic ... . "


text:
https://apnews.com/Globe%2520Newswire/9b45c1ed79b92add1173511ba74065ac
Press release content from Globe Newswire. The AP news staff was not involved in its creation.
Globe Newswire
GlobeNewswire: Technology
PRESS RELEASE: Paid content from Globe Newswire
Shepherd, Smith, Edwards & Kantas Files Lawsuit Against Kalos Capital and its Registered Representative, Kristian Finfrock, for Wrongful Sale of Alternative Investments, Including GPB Capital
Shepherd Smith Edwards & Kantas LLPJanuary 7, 2020 GMT
EVANSVILLE, Wis., Jan. 07, 2020 (GLOBE NEWSWIRE) -- The law firm of Shepherd, Smith, Edwards & Kantas ("SSEK") has filed another case against Kalos Capital for one of their registered representatives pushing clients into so-called "alternative investments," most notably, GPB Capital. According to the complaint filed with FINRA, Kristian Finfrock, who has been a broker with Kalos since 2012, placed more than $750,000 of a retired and ill client's life savings into illiquid alternative investments, including $185,000 into GPB Capital. Other than GPB, most of the alternative investments were non-traded REITs, including HPI Real Estate Opportunities Fund, Shopoff Land Fund, Cottonwood Residential, AEI Capital Corporation and ARC Trust.
Mr. Finfrock, although a registered representative of Kalos, works under the company name "Retirement Income Strategies." However, it is typically unsuitable and inappropriate for retired investors to place any significant savings into illiquid, opaque and very risky alternative investments, such as those Finfrock and Kalos allegedly sold to this client. In addition to Evansville, Finfrock and Retirement Income Strategies purport to have offices in Madison, Middleton and Brookfield.
It appears from SSEK's investigation that Kalos was encouraging its representatives from all over the country to sell expensive and illiquid alternative investments to customers where such investments were clearly unsuitable and often misrepresented.
GPB Capital Holdings
GPB Capital Holdings is a New York based alternative asset manager that purportedly invests in waste management and car dealerships. GPB is under investigation by FINRA, the SEC, the FBI and several state regulators. According to GPB, it raised $1.8 billion from investors and reportedly paid out more than $165 million in commissions to brokers, such as Kalos. Unfortunately, the value of GPB's Funds have dropped dramatically in recent months as the company continues to miss filing deadlines and is accused of being a Ponzi scheme.
Investment Loss Lawyers
Please contact the lawyers at SSEK if you suffered losses from investing in a GPB fund, or any other alternative investment, that was recommended to you through Kalos Capital, Kristian Finfrock, or any other brokerage firm and/or financial adviser. Our lawyers represent investors whose brokers and firms inappropriately recommended investments to them, such as GPB Capital. Contact SSEK to request your free, no obligation case consultation.
ContactSam Edwards800-259-9010 sedwards@sseklaw.com


text:
"Without help from Pharmacist Support, I'd never have achieved any of the things I have in both my professional and personal life. "
Anne Cawdron is a recently retired pharmacist with 40 years' experience in the sector. On 4th October, Anne completed the Virgin London Marathon with her friend Carol to raise funds for Pharmacist Support.
Hi Anne, firstly congratulations on completing the Virtual London Marathon and raising £2340.95 for Pharmacist Support. You must be so proud.
Thanks, it was an amazing day. We started off at 8:00 in low cloud and then the sun came out and it was an absolutely perfect running day. We'd chosen a route that was as much downhill and flat as possible, working our way from Buckstones (a local beauty spot), round Scammonden Reservoir to Barkisland, Norland and Sowerby Bridge, out to Hebden Bridge on the Rochdale canal and back finishing near our running club.
It was a very scenic route and one that went through significant places for us and where friends could join us or cheer us on.
What an achievement! Have you always been into running?
I didn't start running until 2008 when I entered a 5k Race for Life with some pharmacy colleagues. I wasn't able to run 5k at that stage so vowed I'd do it again the next year but be able to run the whole thing. I've been running regularly since then.
You signed up to the Virgin London Marathon back in January before it was cancelled. How did it feel running the marathon without the roaring crowds?
We had so much support; friends who ran with us and others who met us at strategic points with drinks, food, painkillers, plasters and encouragement. This support was fantastic and made it so very special; there were three of us who completed the full distance together and we kept meeting people we knew, and some we didn't know (also running the Virtual Marathon), along the way, especially on the canal.
We had quite a cheering squad at the finish, consisting of family and friends, with a much-needed cup of tea. I'm still buzzing – it was such a moving experience.
Could you tell us a little about your impressive 40-year career in the world of pharmacy?
I retired at the end of 2019 after coming to the end of almost 40 years being qualified. I have loved being a pharmacist, feeling part of a local community, available as a source of healthcare advice, providing an understanding ear and, at times, a shoulder to cry on.
I've been privileged to know and work with lots of local pharmacists in a profession where we can often feel quite isolated. I was involved with the local Halifax branch of the RPSGB for many years (and secretary for quite a few), and arranged professional and social meetings for local pharmacists as well as attending meetings in London and getting to know some of the great and good in pharmacy. I was on Calderdale / Kirklees LPC for several years and latterly a member of CPWY [Community Pharmacy West Yorkshire] the LPC covering all West Yorkshire.
Most of my career has been in Community Pharmacy, both as an employee and as a contractor. I've often found the job challenging but always rewarding. One of the highlights was being a pre-registration tutor and I was a member of the GPhC Standard Setting Panel until quite recently. I like to think I've played a small role in shaping the future of pharmacy and future pharmacists.
Although I've stopped actively working, I plan to continue working with Pharmacist Support.
What were your reasons for running the Virtual London Marathon and raising awareness for pharmacists on the frontline?
Pharmacists in all sectors are under unprecedented stress. Covid-19 has catapulted pharmacy into new ways of working and the profession has risen to the challenge. Pharmacy doors have not closed, patients might have had to wait outside them, but the doors have stayed open. Pharmacy staff have worked extended hours to keep on top of the workload and ensure that patients have got the advice and the medication they need where and when they need it.
During the outbreak I volunteered my services at a local pharmacy, firstly as a dispenser then returned to working as a pharmacist when the GPhC introduced a Temporary Register of recently retired pharmacists. The pressure of work was intense, coupled with a shortage of PPE and sanitiser and inability to adequately social distance in a busy dispensary, it was a hugely stressful time for everyone working in Pharmacy during that period.
I believe it is important that there is an organisation where pharmacists can go for advice and assistance that understands those pressures and the role of the pharmacist. When I needed help it was there for me; I'd hate to think that help was no longer available for other pharmacists in the future that might need it.
So, you had used Pharmacist Support services before?
Yes, almost 20 years ago I received invaluable help from Pharmacist Support, at that time known as the Royal Pharmaceutical Society Benevolent Fund. Without that help I would never have achieved any of the things I have in both my professional and personal life. I always told myself that I would like to "give back" when I had the opportunity so, since stopping full time work, I have been privileged to be able to volunteer with Pharmacist Support.
Seeing what the charity does at close hand inspires me to fundraise so other pharmacists and their families may be able to benefit from the kind of help that was given to me.
When you volunteered in a pharmacy during the outbreak, what did you do to look after your own wellbeing when working under such highly pressurised circumstances?
I tried to fit in some form of exercise every day so I either did an online yoga class or went for a run or a walk. Prior to the pandemic I hadn't really embraced modern technology for exercise, but I started (and have continued) to use YouTube and Zoom for yoga and exercise classes while face to face classes have not been possible.
What piece of advice would you give to a pharmacist or pharmacy student struggling with their wellbeing right now?
Get outdoors whenever you can; it's not original advice and often repeated, but for good reason. There's something about being outside, seeing nature and watching the seasons change that seems to put everything into perspective.
Get in touch about your Story
Please tick the following to enable us to contact you:*
I am happy for Pharmacist Support to contact me
For more information about data consent and how your data is stored, please view the website privacy policy.


text:
\section{Introduction}\label{introduzione}

The issue of determining the universe evolution has brought physicists to formulate various approach spanning from modifications of the Einstein-Hilbert action, quintessence fields to barotropic fluids, and so forth \cite{rev1,rev1bis,rev2,rev2bis}. A recent wide interest has been devoted to stemming the universe dynamics from quantum effects, through a process named decoherence \cite{deco}. The problem of postulating a self consistent evolution of the net quantum fluid is associated to the lack of a complete quantum gravity approach \cite{a,patrizia}. All the possibilities, developed in the literature are typically overshadowed by several bugs. However, a broad interest has been pursued in order to reach suitable quantum signatures in observational cosmology. Indirect hints of plausible quantum shadows may be viewed in constraining the cosmological constant $\Lambda$ from cosmological observational bounds \cite{lambda}. Phrasing it differently, theoretical predictions of a gravitational vacuum state are essentially incompatible with cosmic observational limits. Moreover, both $\Lambda$ and matter orders of magnitude are surprisingly close to each other, albeit the cosmological constant does not evolve in time \cite{lambda2}. A way out for alleviating the above mentioned problems takes into account an additional classical fluid, dubbed dark energy associated to an evolving negative equation of state \cite{darkenergy}. This represents a basically classic approach since the fluid enters the Friedman equations postulating an additional contribution to the whole energy momentum tensor \cite{darkenergy2}. The possible signature of quantum effects at high redshift provides that dark energy may be viewed as a resulting effect of some quantum process \cite{ioesalv}. In such a way, the existence of a hidden quantum mechanism behind the nature of the cosmological constant may be of great interest to describe the dark energy nature \cite{quantumlambda}. A straightforward approach lies on applying the standard quantization to the dynamical equations, passing from the full infinite-dimensional configuration space of general relativity to the so called minisuperspace approach. In that case, the degrees of freedom are mostly reduced and the universe wave function 	 is determined up to boundary conditions, essentially related to the dynamical quantities which define the universe expansion history. Another relevant example is the study of the entanglement effects in primordial cosmology \cite{jae1,jae2}. They have been extensively investigated in the development of modern quantum information \cite{entareview}. The idea of entanglement strives with classical intuition, although recently increasing experimental tests have been performed. The corresponding excellent experimental outputs definitively forecast the prominent role played by entanglement, in various contexts, spanning from quantum physics to cosmology \cite{entareview2}.

In this work, we basically ask for  quantum correlations that can emerge   in  the framework of  cosmology. We assume that quantum information entropy may enter the  energy-momentum tensor as source for the universe dynamics \cite{cosmoenta}. Hence, it turns out that primordial entangled states may contribute with a non-zero density matrix whose trace enters the net energy density, driving the cosmic speed up at different stages of the universe evolution. While at late times the cosmological constant is essentially recovered as limiting case, at higher redshift it becomes a consequence of the adiabatic exchange between cosmological components. The dark energy contribution can be viewed, in general, as an evolving term obtained  as an effect of quantum information \cite{cosmoenta2}. To demonstrate this fact, we here first build up the Von Neumann entropy as a source for the cosmological entropy \cite{cosmoenta3}. Our strategy is to take the Von Neumann entropy between two entangled states, which correspond to two different epochs of the universe evolution. Afterwards, we infer the corresponding dark energy temperature and  interpret it as the quantum information temperature, in the special case of homogeneous and isotropic universe. In particular, specific classes of dark energy models  are  considered, scaling the density term as pure matter, dark energy and the sum between them. In so doing, we  show that the entanglement mechanism is applicable  to the  degrees of freedom  of macroscopic systems, for the whole  universe evolution, under the standard  of decoherence \cite{sett}. This effect, in the cosmological puzzle, is due to the interaction between {\it qubits} with their environment \cite{sett2}, which is the universe itself.

In the paper, we study the density, pressure and equation of state associated to the dark temperature and  compare  results with the  linear entropy, as limiting case of the Von Neumann entropy. Moreover, we consider the adiabatic hypothesis to define either the adiabatic index or the sound speed. From those theoretical constraints, we set stringent limits on the cosmological  parameters. We find that the model works fairly well in reproducing both early and late time cosmological  evolution. Indeed, the cosmological constant is recovered as a limiting case and is interpreted as zero-value of the evolving information density, entering the energy-momentum tensor. Analogously, the  approach can be adopted for early stages and one demonstrates that inflation is also recovered if an effective field is defined from entanglement. We show that the numerical results inferred at late times are perfectly compatible in determining the spectral index of inflation and turn out to reproduce the inflationary accelerated scenario.

The  layout of the paper  is the  following. In Sec. II, we discuss  quantum states that can be built up in view of  the Von Neumann entropy. In particular, we take into account the role played by the entanglement, using  two quantum states in  homogeneous and isotropic cosmology. Afterwards, we combine these requirements with the standard Friedman equations. In Sec. III the role of  dark temperature and its evolution is considered giving a statistical explanation to the Von Neumann entropy by means of associated probabilities of structure formations. In Sec. IV, the case of adiabatic expansion is reviewed with particular emphasis for the consequences in late and early time cosmology. Conclusions are drawn in Sec. V.

\section{Building up entangled states for cosmological eras}

Let us  introduce a strategy for characterizing cosmological quantum states and for describing \emph{a posteriori}  entanglement effects between them.  In view of this, a heuristic procedure consists in  choosing the minimal number of quantities capable of describing the universe at different stages of its evolution according to  the cosmological principle. Thus, a possible
\textit{vector field} obtained by observables is:
\begin{widetext}
\begin{eqnarray}\label{setto}
\boxed{\left\{\Theta\right\}\,=\,\left\{H(z), q(z), \Omega_{m}(z), \Omega_{k}(z), T(z), \ldots\right\}\,,}
\end{eqnarray}
\end{widetext}
where  in the  brackets there are  \emph{cosmographic parameters}, i.e. quantities that can be, in principle, measured without imposing   \emph{a priori}  a cosmological model\cite{cosmografia}. They are the Hubble parameter $H$, the {\it deceleration} parameter, the matter density $\Omega_{m}$  and  the spatial curvature density  $\Omega_{k}$ respectively\footnote{Clearly, the "dimensions" of the vector (\ref{setto}) can be improved according to the degree of "refinement" of our considerations: less parameters mean coarse-grained models.} \cite{cosmografia2}. We include also $T$,  the cosmic  temperature  following from the definition of cosmic  entropy \cite{entropiaetemperatura}.
 Let us assume now now some prescriptions  that we are going to adopt throughout the paper.

\begin{enumerate}
  \item Provided two distinct epochs of the universe evolution, a plausible state which involves a two dimensional vector defined over a given complex Hilbert space $\mathbb{C}$ is:
\begin{equation}\label{phi}
 |\phi\rangle\equiv \left(
\Omega_{m}+i\Omega_{k},\\
\Omega_{k}+i\Omega_{m}\right)^T,
\end{equation}
where the observable quantities  are the spatial curvature ($\Omega_{k}$) and matter ($\Omega_m$) at those epochs.

  \item Following the basic requirements of quantum mechanics,  to get a linear independent and non-normalized vector in the  Hilbert space, we can adopt the following construction:
\begin{eqnarray}
|\tilde e_A\rangle&=&\left(
\Omega_{m}+i\Omega_{k},
i\Omega_{m}+\Omega_{k}\right)^T, \\
|\tilde e_B\rangle&=&\left(
\Omega_{m}-i\Omega_{k},
-i\Omega_{m}+\Omega_{k}\right)^T.
\end{eqnarray}

  \item Related to the above prescription, one can assume the validity of the Gram-Schmidt procedure which turns out to give orthonormal bases of the form:
\begin{eqnarray}
|e_A\rangle&=&
N_A |\tilde e_A\rangle,\label{ortho1}\\
|e_B\rangle&=&
N_B (\Omega_m^2+\Omega_k^2) |\tilde e_B\rangle
+N_B 2i\Omega_m\Omega_k |\tilde e_A\rangle,
\label{ortho2}
\end{eqnarray}
with normalization factors: $N_A=\frac{1}{\sqrt{2(\Omega_m^2+\Omega_k^2)}}$ and $N_B=\frac{1}{\sqrt{2(\Omega_m^2+\Omega_k^2)(\Omega_k^2-\Omega_m^2)^2}}$.

\item For any epochs, e.g. inflation, reheating, recombination, dark energy domination and so forth,  there would exist a different Hilbert space, which is built up guaranteeing that the cosmological principle holds. To account for the cosmic dynamics we assume that, as the universe undergoes a phase transition, the \emph{interaction} of any phase is modeled by the entanglement between quantum states. Hence,   entanglement replaces the effects due to phase transitions in the standard cosmology picture.

\item  As a result, we infer a corresponding \emph{multipartite} system. To allow the entanglement process, in particular, we need to consider at least two epochs, leading to an associated Hilbert space of the form: $\mathbb{C}^2\otimes \mathbb{C}^2$, whose orthonormal basis is given by:
\begin{eqnarray}
 |e_A\rangle_{1} |e_A\rangle_{2},\;
  |e_A\rangle_{1} |e_B\rangle_{2},\;
   |e_B\rangle_{1} |e_A\rangle_{2},\;
    |e_B\rangle_{1} |e_B\rangle_{2},
 \label{basis}
\end{eqnarray}
with $1;2$ indicating the epochs involved.
\end{enumerate}
The cosmic state is univocally assigned to a certain time of cosmological evolution as one defines the functional dependence of the variables associated to that state. If the cosmic \emph{evolution} is due to the correlation among states, with constraints compatible with present observations, we soon get that any coarse-grained quantum state is modeled by means of  the vector  \eqref{setto}. The principal consequence of assuming a vector of such a form is that the corresponding thermodynamical properties emerge from the \emph{information entropies} \cite{nuew}, defined as byproducts of the  entangled wave functions. This procedure does not need \emph{a priori} a process of quantization of gravity
\cite{nicroro2,nicroro3}, requiring, instead, that the universe is characterized by a quantum description at the level of primordial cosmology \cite{queb}.

The entangled \emph{correlation} is hereafter named \emph{entangled states ansatz}, where the two epochs are built up in terms of the following wave function:
\begin{equation}
|\Psi\rangle = \alpha|e_A\rangle_1|e_B\rangle_2 + \beta|e_B\rangle_1|e_A\rangle_2\,,
\label{stato}
\end{equation}
where, $\alpha,\beta\in\mathbb{C}$ lead to $|\alpha|^2+|\beta|^2=1$, corresponding to the standard normalization procedure.

The aim of this paper is to start from the above assumptions and to describe  quantum thermodynamics in  cosmology. This means to find  effective relations between the Von Neumann entropy and cosmological densities in view   of  dark energy evolution stemming out from early epochs.

\subsection{The early phases of cosmic evolution}

The strategy to match entanglement with early universe thermodynamics consists in comparing thermodynamical potentials with quantum entropies. To do so, let us take into account the above described $N$-dimensional Hilbert space and let us associate to a certain event a given probability $\mathcal P_k = \frac{1}{N}$, $\forall k$. We require that a particular observable is associated to $\mathcal P_k$ and even that $\mathcal P_k\neq 0$ for entangled quantum states only.

Thus, considering non-local entangled states with $\mathcal P_k\neq 0$, we associate any probability to the cosmological quantities of  interest, for example distribution of  galaxies, cosmic structures, and so on. For those reasons, \emph{selection criteria}, i.e. techniques to quantify \emph{how much} a given cosmological quantum state is actually non-pure, become essential to characterize the \emph{cosmological density matrix}.

Hence, specializing our attention to two distinct epochs in which the universe is described by a set of observable quantities, we associate to them two quantum states. Those states depend upon a finite number of cosmological quantities which  describe the universe dynamics even at a classical regime. Phrasing it differently, one looks for the possibility to define the set of parameters,  which enable either a classical or quantum descriptions of the whole universe, into a single paradigm.

Under the hypothesis of a homogeneous and isotropic space-time, the simplest assumption is to take into account the matter density, constituted by baryons and cold dark matter, and the spatial curvature only. So that, considering the Friedman-Robertson-Walker (FRW) metric:
\begin{equation}\label{hgjhg}
ds^2=dt^2-a(t)^2\left(dr^2+r^2\sin^{2}\theta d\phi^2+r^2d\theta^2\right)\,,
\end{equation}
we assume that all fluids entering the standard energy momentum tensor are perfect. Thus, the  equation of state for any species is defined by $\omega_i\equiv\frac{P_i}{\rho_i}$, whereas the pressure for the dark component must exhibit repulsive effects in order to counterbalance the attraction of gravity \cite{iorepulsivo,ionorepulsivo}. Considering the conservation law given by the contracted Bianchi identities $\nabla^\alpha T_{\alpha\beta}=0$, one gets the relation
\begin{equation}\label{utyyyy}
\frac{d\rho}{dz}=3\left(\frac{1+\omega}{1+z}\right)\rho\,,
\end{equation}
where $\omega$ is the adiabatic index of tjhe equation of state and $z$ is the redshift.
The Friedman equations are

\begin{eqnarray}
\label{ave2}
H^2 &=& {8\pi G\over3}\rho\,,\\
\dot H + H^2&=&-{4\pi
G\over3}\left(\rho+3P\right)\,,\nonumber
\end{eqnarray}
characterizing the universe dynamics at all stages of  evolution. Here, we assume the Hubble parameter definition $H=\dot a/a$ and the spatial curvature to be negligibly small\footnote{This assumption does not contradict the above construction of quantum states, but  simply reduces the dimensions of parameter phase space   simplifying  the form of wave function.}. Associated to any species, one  has a corresponding temperature as a  function of $\omega_i$ or, more practically,  as function of $z$. Even though the \emph{dark temperature}, i.e. the temperature of dark energy and dark matter, may be, in principle, the dominant term for some epochs of the universe, no significative  modifications are today expected as provided by observations.

To match  the  quantum state description, given by Eq. \eqref{stato}, with the classical description related to   Eqs. \eqref{ave2}, we can easily assume that the density matrix is an \emph{energy source} for $\rho$. This can be obtained by assuming that the eigenvalues of the density operators are the \emph{present observed densities}.

We will  use of the above recipe  to find out an expression for $P, \omega$ and $\rho$ in the case in which the dark energy term is derived from quantum effects. The idea is supposing that the Von Neumann entropy is a suitable measure for entanglement  and contributes to the whole entropy of the universe, assuming that the eigenvalues of the density operator enter Eqs. \eqref{ave2}. Assuming the Von Neumann entropy as density source for the Friedman equations is not a mere imposition. It is possible to  demonstrate, indeed,  that under the hypothesis of binomial probability distribution, one recovers the Von Neumann entropy as an entropy source. This fact enable us to describe the universe through a multipartite state.

\section{The quantum \emph{dark temperature}}

We focus now on the consequences on thermodynamics related to  Eq.\eqref{stato}. In particular, let us  redefine the concept of temperature and  discuss the role of the Von Neumann entropy in the cosmic evolution. In particular, we have to note that microphysics of dark energy is still unknown due to the fact that a  self-consistent theory of quantum gravity is currently unavailable. Plausibly, a full quantum theory of gravitation would provide a final description of the \emph{effective} dark energy evolution, describing the reasons for a too large quantum cosmological constant contribution if compared with cosmic observations. A description  based on  \emph{decoherence} can help in this perspective. Decoherence allows the emergence of classical features  when some physical degrees of freedom interact with the quantum system by the phenomenon of entanglement, i.e. some  degrees of freedom entangle with the environment. Our prescription is that different epochs of the universe evolution provide some physical degrees of freedom which are intimately interacting with the universe environment. In other words, one expects that  macroscopic physical properties  can emerge from this process. In particular, thermodynamical properties.
Combining the first and second laws with $V=a^3$ the volume, we  obtain the relations for the entropy
\begin{subequations}
\begin{align}
Td\mathcal S&=d(\rho V)+P dV = d[(\rho+P)V]-V dP\,,\\
{\partial^2 \mathcal S \over \partial T \partial V}&={\partial^2 \mathcal S \over \partial V \partial T}\,.
\end{align}
\end{subequations}
The second relation comes from the  integrability. Immediately we have
\begin{equation}
dP=\left({\rho+P\over T}\right)dT\,,
\end{equation}
whose form can be integrated to give:
\begin{equation}
d\mathcal S= {1\over T} d[(\rho + P)V]-(\rho + P)V {dT\over
T^2}=d\bigg[{(\rho+P)V\over T} + C \bigg]\,,
\end{equation}
where  $C$ is an integration constant. The entropy density naturally follows as
\begin{equation}\label{entrotermo}
\mathcal S \equiv{\rho + P\over T}\,.
\end{equation}
The above calculations are standard. We need now a mechanism such that classical aspects emerge as consequence of quantum evolution. In other words, we need to relate Eq. \eqref{entrotermo} to the above quantum description. One can assume the  process of decoherence which supposes that the universe is localized in a given  state  defined in one of the minima of an effective potential. In one of these minima, for example, the universe can start the today accelerating phase. In particular, during the evolution in such a state the  equation of state persists in its negative form, whereas afterwards it changes its sign. This happens because there exists a given probability that the universe evolution falls into a superposition of localized states, which correspond to a ground state. The assumption of different vacua can be replaced considering entanglement as responsible for the same process.

\subsection{The  Von Neumann entropy at early time cosmology}

In order to motivate how Eq. \eqref{entrotermo} is fueled by quantum entropy, we relate $\mathcal S$ to its quantum counterpart. To get the form of quantum information entropy, let us assume that a cosmological structure, at a given epoch, forms with a  probability $\mathcal P_1$ given by:
\begin{subequations}\label{prob1}
\begin{align}
\mathcal P_2&=1-\mathcal P_1\,,\\
\mathcal P_1&=\rho_n\,,
\end{align}
\end{subequations}
where $\rho_n$ is the \emph{normalized} density of microstates associated to the system under examination, i.e. the set of eigenvalues of the density operator. Under this scheme, the probability of non-forming a given galaxy can be reported as $P_2$.
If one assumes that the net information contribution  $\mathcal I$ for structure formation must be positive definite, a possible relation with the entropy is $I\propto \exp S$, where $S$ is the information entropy that (in principle) is different from $\mathcal S$. In so doing, one gets:
\begin{equation}\label{entropy32}
S=\ln\rho_n\ln(1-\rho_n)\,,
\end{equation}
which comes from  the binomial distribution:
\begin{equation}\label{bi}
P(X)={N\choose X}\rho_n^N(1-\rho_n)^{N-X}\,,
\end{equation}
with the ansatz that $S\propto \mathcal P(X)$ and $N=2, X=1$.
If the density of microstates is small enough, Eq. \eqref{entropy32} becomes:
\begin{equation}\label{entropy33}
S\propto-\rho_n\ln\rho_n\,,
\end{equation}
which is much more accurate as soon as $\rho_n\rightarrow0$.
Since the definition \eqref{entropy33} is general, one can reverse the approach and may imagine that the Von Neumann contribution well adapts to Eq. \eqref{entropy33}. Thus, if we assume that the standard entropy density, evaluated by Eq. \eqref{entrotermo}, is entirely due to the information entropy, one can conclude that
\begin{equation}\label{uguaglianza}
\mathcal S\propto \exp I =S\,.
\end{equation}
In this picture, the cosmic entropy comes out from   quantum contributions without considering  any decoherence process. In what follows, we therefore assume the density entering Eqs. \eqref{ave2} is given by $\rho\equiv\sum_n \rho_n$.

\subsection{From information to quantum entropy}

An immediate extension of what we described in terms of probability is based on introducing the \emph{reduced density matrix} $\hat{\rho}$. A mixed configuration  is
\begin{equation}\label{mixed}
\text{Tr}\hat{\rho}^2 \neq \text{Tr} \hat{\rho}\,,
\end{equation}
so that we can define the $m$-particle reduced density matrices by:
\begin{equation}\label{e:yy}
  \rho_m \equiv \sigma\ket{i}\text{Tr}\{a_\star\,\,
  \rho\,\,a^\dag_\star \}\bra{j}.
\end{equation}
where $a_\star\equiv \left\{a_{i_1}, a_{i_2},...,a_{i_m}\right\}$, $a_\star^\dag\equiv \left\{a_{i_1}^\dag, a_{i_2}^\dag, ..., a_{i_m}^\dag\right\}$, $\ket{i}\equiv\ket{i_1, i_2, ..., i_m}$ and $\bra{j}\equiv \bra{j_1, j_{2}, ..., j_m}$, with $\sigma\equiv \frac{1}{(m!)^2}$.
An important property is that,  under the above  reduced density matrices unitarily transform being $\rho' = U(\Lambda)\rho U^\dag(\Lambda)$.  This means that they are  invariant under Lorentz transformations.
In other words,  taking into account a  Lorentz transformation $\Lambda$, all quantum operators and in particular creation and annihilation operators, transform according to  standard Lorentz transformation. Moreover:
\begin{eqnarray}
\mathcal U(\Lambda)\ket{0}=\ket{0}\,,
\end{eqnarray}
where the last condition leads to the Lorentz invariant vacuum and allows to determine all states acting as creation and annihilation operators on it. This holds if and only if the vacuum unitarily transforms via the relations: $ \ket{\Psi}' = \mathcal U(\Lambda)\ket{\Psi}, \bra{\Psi}'=\bra{\Psi}U^\dag(\Lambda)$.

\subsection{The Von Neumann entropy and its consequence in cosmology}

From the above considerations, the von Neumann entropy may be considered as a natural consequence of the information \emph{broadcasted} by the density matrix. We follow this recipe to adapt the Von Neumann entropy in the framework of primordial cosmology. To do so, we basically adopt the idea: \emph{if a quantum (cosmological) state exists under the hypothesis to be a non-pure state, then it shows an entropy of the form}:
\begin{equation}
S \equiv -\text{Tr}{(\hat{\rho}\ln\hat{\rho})} = -\sum^N_{n=1} \rho_n\ln\rho_n.
\end{equation}
Here, $\rho_n$ are the eigenvalues of $\rho$, with the additional normalization condition $
\text{Tr}\hat{\rho} = 1$.
The density matrix is commonly associated to physical states, so that it should be Hermitian, with the property:
\begin{equation}\label{hermitiano}
\rho \circeq V[diag({\bf \rho}_n)]V^{\dagger}\,,
\end{equation}
which implies that the eigenvalues ${\bf \rho}_n\equiv\rho_1,..., \rho_{N}$ are invariant under unitary transformations.
The same property is accounted for Lorentz transformations $\mathcal U(\Lambda)$. In this case, we require that
\begin{eqnarray}\label{lorentz}
\hat{\rho}^\prime &= \mathcal U(\Lambda)\rho
\mathcal U^\dag(\Lambda) &= \mathcal U(\Lambda)V[diag({\bf \rho}_n)][{\mathcal U(\Lambda)V}]^{\dagger}\,,
\end{eqnarray}
which preserves the eigenvalue values, providing the above  property that the von Neumann entropy turns out to be \emph{Lorentz invariant} and therefore \emph{it can be used in  cosmology}. As well as $\hat\rho$, even the Von Neumann entropy of every \emph{reduced density matrices}, i.e. $S_r\equiv -\text{Tr}{(\rho_R\ln\rho_R)}$, with $R\in[1;{\ensuremath{\mathbb N}}]$,  satisfies the Lorentz invariance. The universe can be therefore  parameterized by means of $\hat\rho$. The strategy lies on assuming a set of Lorentz invariant (separate) measurements for arbitrarily chosen epochs of its evolution.

Hence, parameterizing by the Von Neumann entropy,   assuming  $\mathcal S=S$,  and inverting Eq. \eqref{entrotermo}, we have:
\begin{equation}\label{temp}
T=-\frac{P+\rho}{\rho\ln\rho}\,,
\end{equation}
with the request that the sum of eigenvalues gives rise to $\rho$. Here $T$ is the dark temperature. Eq. \eqref{temp} can be recast in terms of  redshift, by means of Eq. \eqref{utyyyy}:
\begin{equation}\label{tempz}
T=-\frac{(1+z)}{3\rho\ln\rho}\frac{d\rho}{dz}\,,
\end{equation}
or alternatively, in a more compact form, adopting the identity $a\equiv(1+z)^{-1}$ by:
\begin{equation}\label{tempcompact}
\boxed{T=\frac{d\ln\Big[\ln\rho\Big]^{\frac{1}{3}}}{d\ln a}\,.}
\end{equation}
Measurements of cosmic microwave background radiation allow to constrain the temperature of the universe. The temperature involved in the standard measure is considered as due to all constituents of the universe. Thus, our outcome enters the net temperature as well, contributing with a term of dark temperature, i.e. associated to quantum imprints at early stages.

The functional behavior of $T$ in terms of $z$ is not known \emph{a priori}. We may suppose to take a generic polynomial expansion of $T$. In particular, the simplest assumption can be $T\propto a^n$, giving:
\begin{subequations}
\label{soluz}
\begin{align}
\rho&=\rho_C \exp(f_3(a))\,,\\
\rho_C&=(1-\rho_0)f_3(1)\,,
\end{align}
\end{subequations}
where we made use of the function:
\begin{equation}\label{f}
f_\sigma(a)\equiv\exp\left({\sigma\,a^n\over n}\right)\,.
\end{equation}

\begin{figure}[ht]
\includegraphics[scale=0.6]{rhoplot.eps}
\caption{{\it{The evolution of the function $\rho(z)$; the qualitative values here reported are $\rho_C=10^2; 25; 10^6$ for $n={1\over 2};\,1;\,{1\over 3}$ respectively red, dashed and black lines. }}}
\label{figura2}
\end{figure}

It could be convenient to focus on a first-order expansion leading to the approximate solutions:
\begin{subequations}\label{appr}
\begin{align}
\rho^{(1)}&\approx (1-\rho_0)(1-3f_2(1)z)\,,\\
T^{(0)}&\approx\Big|\frac{\log f_3(1)}{\log(1-\rho_0)}\Big|\,,
\end{align}
\end{subequations}
where we use  $a\equiv(1+z)^{-1}$ and  consider that $\rho$, at $a=1$, is forced to be $\rho(a=1)=1-\rho_0$. This is an arbitrary choice which enables one to fix $\rho(a=1)$ with different values, corresponding to the magnitudes imposed from observations. Examples are: $\rho(a=1)=1$ (dark energy and  matter contribution); $\rho_0=0$, $\rho(a=1)=0.7$ (dark energy contribution); $\rho=0.3$, $\rho(a=1)=0.3$ (matter contribution);  $\rho_0=0.7$ and so forth. This specializes $\rho_0$ to be the counterpart of our quantum dark fluid and gives to the approach the role of additional fluid entering the  energy-momentum tensor.

Under the above simple hypothesis, it is easy to show that  approximate ranges of values for $n$ are given by:
\begin{subequations}\label{enne}
\begin{align}
n&\in[-0.255\,;\,0[\,,\\
n&\in[-0.295\,;\,0[\,,
\end{align}
\end{subequations}
which guarantee that the paradigm gives rise to  pure dark energy (first case),  pressureless matter (second case), as a byproduct of the entangled state ansatz.

Another particularly interesting case is to consider as entropy source the \emph{linear entropy}. It represents the first prototype of entanglement entropy and may be viewed as a first approximation towards the definition of the Von Neumann entropy. In such a case, we have:
\begin{equation}\label{linearentropy}
S_L=\frac{N}{N-1}\left(1-\mu\left[\rho\right]\right)\,.
\end{equation}
Here, we can interpret $\mu[\rho]$ as a general function of $\rho$, that can be approximated to the first-order Taylor expansion, having $\mu\sim\rho$. The corresponding entropy function estimates quantum correlations, given a set of subsystems in the same way of Von Neumann entropy.
In this case, for the dark temperature, we  have:
\begin{equation}\label{temp}
T=\frac{a}{3\mathcal N}\frac{d\ln(1-\rho)}{da}\,,
\end{equation}
or alternatively, with respect to the redshift $z$:
\begin{equation}\label{tempz}
T=-\frac{(1+z)}{3\mathcal N}\frac{d\ln(1-\rho)}{dz}\,,
\end{equation}
where we consider, in both the approaches, the re-scaling constant $\mathcal N\equiv \frac{N}{N-1}$, which depends upon the degrees of freedom $N$ of the system. Following the same procedure that we used for the Von Neumann entropy, and assuming for example $N=4$, we  get:

\begin{subequations}\label{soluzu2}
\begin{align}
\rho&= 1 + \rho_C\exp{\Big[\frac{4\,(1+z)^{-n}}{n}\Big]}\,,\\
\rho_C&=-\rho_0\exp{\left(-\frac{4}{n}\right)}\,,
\end{align}
\end{subequations}
with the reported limits over $n$, Eqs. \eqref{enne}, which still continue holding. Even in this case, we find that $\rho$ can be only matter, dark energy or both, by tuning the solution through the free constant $\rho_0$.

\section{The  adiabatic expansion }

Standard thermodynamics assumes that, provided a particle ensemble, the dynamical equilibrium corresponds to a precise maximum of entropy. At early stages of  evolution, the thermal equilibrium is reached. Indeed, one usually assumes that above $100$ GeV, the  distributions are  the standard Fermi-Dirac and Bose-Einstein ones
\begin{subequations}\label{distribuzione}
\begin{align}
f_{BE}(p)=\frac{1}{e^{(\epsilon-\mu)/T}-1}\,,\\
f_{FD}(p)=\frac{1}{e^{(\epsilon-\mu)/T}+1}\,.
\end{align}
\end{subequations}
The entropy definition can be generalized as
\begin{equation}\label{entrgen}
dS=\frac{dU+pfV-\mu dN}{T}\,,
\end{equation}
by adding also the chemical potential $\mu$. From the second law of thermodynamics, the chemical equilibrium is reached as soon as the whole initial chemical potentials are summed up becoming equivalent to the net final ones. In this case, through Eq. \eqref{distribuzione}, given the mass and the momentum $m$ and $p$ respectively, for non-relativistic particles, we consider the energy $\epsilon(p)\sim m+\frac{p^2}{2m}$ and we easily get, for $n$ identical terms:
\begin{equation}\label{rhoux}
\rho=mn+\frac{3}{2}nT\,,
\end{equation}
supposing that $\epsilon(p)\propto \rho$. In particular, during early phases, neglecting the particle chemical potentials, one arrives to the definitions of pressure, density and number of particles:

\begin{subequations}\label{definizioni}
\begin{align}
P=\frac{g}{(2\pi)^3}\int{d^3pf(p)\frac{p^2}{3\epsilon}}\,,\\
\rho=\frac{g}{(2\pi)^3}\int{d^3pf(p)\epsilon(p)}\,,\\
n=\frac{g}{(2\pi)^3}\int{d^3pf(p)}\,,
\end{align}
\end{subequations}
which are valid if  the equilibrium hypothesis holds.

The  expressions in Eqs. \eqref{definizioni} are evaluated under the hypothesis of adiabatic regime where the  entropy is forced to be a constant, hereafter $\bar S$. By means of the fact that $dS=0\Leftrightarrow S=\bar S$, we  can invert the expression for the entropy obtaining
\begin{equation}\label{prevst}
P=\bar S T-\rho\,,
\end{equation}
and, being  $\rho=-\frac{S}{\ln\rho}$, we  have:
\begin{equation}\label{obt}
P=\bar S\left[T+(\ln\rho)^{-1}\right]\,.
\end{equation}
The above formula provides two relevant limits:
\begin{description}
  \item[At early phases] $P\,\sim T$\,,\\
  \item[At late phases] $P\,\sim \frac{1}{\ln\rho}$\,,
\end{description}
which correspond respectively to a pressure which, at late times depends essentially upon the density in a non-linear way. as a consequence,  evaluating the equation of state $\omega\equiv P/\rho$, we have:
\begin{equation}\label{bd}
\omega\equiv-\frac{\bar S}{\rho\ln\rho}\,.
\end{equation}
In particular, since $\bar S\equiv -\rho\ln\rho$,  it follows that $\omega=-1$ and we recover a   cosmological constant contribution.

In other words, our paradigm suggests that the cosmological constant exists even at the level of early phases as consequence of the entangled state ansatz, albeit it evolves in time throughout the universe expansion history, leading to a dark energy evolving time at small redshift regime.  In other words, \textit{the cosmological constant is the consequence of the adiabatic evolution}.

Assuming a  perfect fluid,  the corresponding speed of sound is \cite{octo}:
\begin{equation}\label{speedofsound}
c_s^2 = \left(\frac{\partial P}{\partial \rho}\right)\,.
\end{equation}
It must be compatible with small density perturbations, which barely propagate in the universe \cite{sound}. Hence, the speed of sound may be supposed to be negligibly small at all stages of the universe evolution, having $c_s= \sqrt{\gamma (C_p-C_V)T}\sim0$,  so that we infer:
\begin{equation}\label{adyab}
c_s^2=\bar S\Big[\frac{\partial T}{\partial\rho}+\frac{\rho}{\bar{S}^2}\Big]\,.
\end{equation}
At late times,  the entropy is large enough to enable the speed of sound to vanish.  In other words,the approach points out that  entropy is proportional to the square of the
velocity and temperature gradients. One can find analogous results even in other effective thermodynamical models, e.g.  in the case of ideal-gas-like universe with zero speed of sound or in   geometrothermodynamics \cite{dgeometro}.

\subsection{The cosmic evolution at  late-time dark energy}

Without  fixing \emph{a priori} the value of $\rho_0$, the pressure associated to  dark component becomes:

\begin{equation}\label{prex}
P=-\frac{(1-\rho_0)\exp(f_3(a)-f_3(1))(f_3(a)+a^{-n})}{a^{-n}}\,.
\end{equation}
This expression for the pressure ensures that  $z$ lies inside the observational intervals and generalizes the case where the entropy has been taken constant. The corresponding value of $P$ tends to $P\sim -0.7$, in the case of $\rho_0=0.3$. This means that dark energy can  be obtained by our quantum fluid as a dark fluid. The functional form of the pressure slightly departs from a constant value, leading to a possible constant dark energy term, different from a pure cosmological constant.

The corresponding functional form of the pressure $P$ is slightly evolving and turns out to be:
\begin{equation}\label{prex}
P\approx -\rho_\Lambda\,,
\end{equation}
in a wide range of redshifts, compatible with those where dark energy dominates. Here, we can assume $\rho_\Lambda\equiv \rho_0-1$. This result  gives an important outcome: from our model it is possible to recover the cosmological constant behavior in an effective semiclassical approximation. The $\Lambda$CDM model can be therefore mimicked by quantum effects due to entanglement with a dark energy fluid which naturally has a negative sign for the  dark energy pressure. In other words,  the $\Lambda$ term can be recovered through the  information entropy.

\subsection{The cosmic evolution at early inflationary phase}

The present approach can be adopted also  at inflationary epoch. The prescription assumes, as  source of inflation, the energy density \eqref{soluz} derived from entanglement. To show this, one can evaluate the corresponding energy density  by defining an effective potential which depends on a scalar field $\phi=\phi(a)$.  We interpret the inflaton field as an effective byproduct of the entangled state ansatz. So, assuming a generic primordial scalar field as source for the inflationary phase, we have

\begin{subequations}\label{assunzioninflazionarie}
\begin{align}
a&(t)\propto t^s\,,\label{uno1}\\
\rho&=\frac{1}{2}\dot \phi^2+V(\phi)\,,\label{uno2}\\
P&=\frac{1}{2}\dot \phi^2-V(\phi)\,,\label{uno3}\\
r&=16\epsilon\,,\label{uno5}\\
n_s&=1+2(\eta-3\epsilon)\,,\label{uno4}
\end{align}
\end{subequations}
with $s>1$, as in the case of standard inflation and $n_s$ the usual spectral index, with $\epsilon\propto \left(\frac{V^\prime}{V}\right)^2$ and $\eta\propto \frac{V^{''}}{V}$ \cite{inflazione1}. Inflation occurs if  Eqs. \eqref{assunzioninflazionarie} are capable of rapidly accelerating the universe. We thus notice that those quantities enter the amplitude of the primordial power spectrum \cite{inflazione2} by:
\begin{eqnarray}\label{uno6}
\Delta^2_{\cal R}=\frac{1}{8}\left(\frac{\kappa }{\pi \sqrt{\epsilon}}\right)^2H^2\,.
\end{eqnarray}
Thus, by comparing Eqs. \eqref{assunzioninflazionarie} with the prescriptions of our model, we get as effective potential:
\begin{equation}\label{qualcosa}
V(a)=\frac{(1-\rho_0)}{2}\exp(f_3(a)-f_3(1))\left(2+a^nf_3(a)\right)\,,
\end{equation}
which has been evaluated as a  function of the scale factor $a(t)$ and corresponds to $\rho-P$. The associated numerical limits on the spectral index $n_s$ are:
\begin{equation}
n_s\in[0.9968,1.0074]\,.\label{uno7}
\end{equation}
The above values have  been defined through the intervals given in Eqs. \eqref{enne}, by fixing $s\approx 1.3$. In particular, the maximum $n_s$ has been found in the case: $n\approx -10^4$, whereas the minimum $n_s$ as: $n_s=-0.295$. Both the values are derived at  $t\approx 10^2\,t_{Pl}$, with $t_{Pl}$ the Planck time and conventionally $\rho_0=0.7$.

Although only indicative, those values may be directly compared with the observational values of $n_s$, estimated by Planck$+$WP data \cite{Planckdata,Planck2015}. In the former case, one has $n_s=0.9603\pm0.0073$. A quick look at our numerics enables us to conclude that they lie in a an acceptable interval, within the $1\sigma$ confidence level.

On the other side, we get:
\begin{equation}
|r|\sim 0.0044\,,\label{uno8}
\end{equation}
which is compatible with the Planck constraint: $r<0.11$ \cite{Planckdata,Planck2015} at $2\sigma$ confidence level.

With those results in mind, the amplitude of the primordial power spectrum does not depart significatively from the expected values. Hence,  one concludes that our approach is well defined, even at the level of early time cosmology confirming to be suitable to  describe the universe dynamics at inflationary  time.

\section{Conclusions}

In this paper, we considered the imprint of quantum cosmology as a concrete prerogative to explain the universe dynamics. in this perspective, we adopted the  Von Neumann entropy into the context of general relativity, assuming that it can be considered as a source for the dark energy evolution. In particular, the basic assumption is that   dark effects propagate  up to our time starting from primordial quantum counterparts. In particular, we considered  the \textit{entangled state ansatz} assuming  that any  two epochs of the cosmic evolution are correlated  through the entanglement. In so doing, writing up the density matrix for  simple pairs of entangled wave functions, associated to distinct epochs, we are able to characterize the Von Neumann entropy as the  quantum information source driving the cosmic speed up. So that, in our treatment we assume that early phases of the universe evolution were described in terms of entangled quantum states, whose net effect is producing a \emph{thermodynamic source} described by  entropy contributions. We do not assume any microscopic landscape for characterizing $S$. In so doing, we frame the entanglement measure in terms of $S$, showing a coarse grained mechanism behind the  acceleration of the Hubble fluid. In such a picture, we even considered the linear entropy as a limiting case of the Von Neumann entropy for the specific case in which it is linearly expanded around the chemical potential $\mu[\rho]\sim\rho$. We required that late-time effects are comparable with those at early phases, having that the entropies, contributing to the net densities, evolve in a way compatible with observations. The adiabatic evolution can be investigated in such an approach   by defining a  {\it dark temperature} that matches information entropy   with standard thermodynamics. We interpreted it as the temperature due to quantum information, associated to the dark constituents of the universe. Its magnitude turns out to be negligibly small, leading to the gravitationally repulsive effects of dark energy. We even showed that the entropy density may be easily compared with an information entropy, by comparing $S$ with the given probability of forming structures.  We thus demonstrated that the cosmological constant $\Lambda$ can be  achieved in the simplest case of adiabatic evolution. This may be viewed as the possibility to \emph{fuel} the $\Lambda$ term by means of the information density, defined as a measure of the entanglement-degrees related to the thermodynamical state of the universe. Analogously, we showed that inflation is also recovered in this approach. Specifically, we defined an effective potential in terms of the scale factor $a(t)$, interpreting the inflaton as a field related to the entanglement processes. The numerical values of $n_s$, $r$ and $\Delta^2_{\cal R}$ are compatible with current observations as well as the constraints used for late-time cosmology.
In future works, we will develop the approach taking into account observational data at early and late epochs.

\section*{Acknowledgements}

S.C. acknowledges the support of  INFN ({\it iniziativa specifica} QGSKY). This paper is  based upon work from COST action
 CA15117 (CANTATA), supported by COST (European Cooperation in Science and Technology).

redpajama_set_name: RedPajamaArXiv


Posted in: Cool Stuff, Engine Shop, Restorations.	Tagged: Knucklehead, run-stand.
This is the other Kuncklehead that Highway Choppers is working on. The motor is done and now they are working on the chassis.
Posted in: Engine Shop.	Tagged: Engine Rebuild, run-stand, Shovelhead.
Another engine rebuild that we did recently.


A gorgeous blend of edible sugar sea glass in shades of blues and greens.
Sea glass is hard and crunchy, with a sweet sugary flavor.
Please keep in mind that these are sprinkles, each individual piece is smaller that actual sea glass. They are about 1/4"(.5 cm) wide.


Re-envisioning a classic, the pin on ball compass still features the same direction finding reliability and hands-free ease of use, now with a stabilizing button and a sleek, modern look. Features: Pins-on for hands-free use. Waterproof, rotating ball works from any angle. Cardinal points. Dimensions: 1"x1"x1". Limited Lifetime warranty.


text:
Larry James Sechrest (; 12 de octubre de 1946 - 30 de octubre de 2008) fue un economista estadounidense que defendió las ideas de la Escuela austriaca. Fue profesor de economía en la Universidad Estatal de Sul Ross y fue director del Instituto de Libre Empresa de la universidad.

Carrera
Después de trabajar como instructor en la Universidad de Texas en Arlington, Sechrest se unió a la facultad de la Universidad Estatal Sul Ross en 1990. En 1991, se convirtió en director de su Instituto de Libre Empresa. En 1993, Quorum Books publicó su libro "Banca libre: teoría, historia y un modelo de laissez-faire". Se convirtió en profesor titular en 2002.

Sechrest era un libertario (libertarianism) y promovió las ideas de la escuela austriaca de la economía. Sus primeras influencias incluyeron a los economistas austríacos Ludwig von Mises, Friedrich Hayek y Murray Rothbard, así como a no economistas como Edmund Burke y Ayn Rand. Apoyó la banca libre y el anarcocapitalismo.

En 2004, Sechrest generó controversia con un artículo que escribió para la revista  Liberty. En el artículo, titulado "Una pequeña ciudad extraña en Texas", describió la ciudad de Alpine, Texas, donde se encuentra el estado de Sul Ross. Elogió el clima, los espacios abiertos y la baja tasa de criminalidad, pero dijo que los residentes eran "estúpidos" y "consanguíneos", y denominó el área como "el hogar orgulloso de algunos de los terrones más tontos del planeta". Extendió esta crítica a su empleador, la universidad, declarando que sus graduados "todavía operaban a un nivel de décimo grado" y solo obtuvieron títulos "a través de la malversación de profesores y administradores". Cuando las copias del artículo circularon por la ciudad, la reacción fue mayoritariamente hostil. Recibió amenazas de muerte y mensajes obscenos, y su propiedad fue objeto de vandalismo. El presidente del estado de Sul Ross desautorizó los puntos de vista de Sechrest, pero no pudo tomar ninguna acción formal contra él ya que Sechrest tenía  tenencia. Los estudiantes amenazaron con boicotear sus clases. El alcalde de la ciudad respondió declarando una "Semana de los Alpes Nos Encanta" con una manifestación y un desfile. La controversia finalmente disminuyó y Sechrest continuó enseñando en la universidad.

Sechrest publicó numerosos artículos en revistas revisadas por pares, incluido el Journal of Economics, el South African Journal of Economic and Management Sciences, el Review of Austrian Economics y Reason Papers. También escribió para medios no académicos como "Liberty", "The Freeman" y " Free Radical". Formó parte del consejo editorial de Quarterly Journal of Austrian Economics y del consejo asesor de The Journal of Ayn Rand Studies. Fue miembro de la Academia de Ciencias de Nueva York.

Vida personal
Sechrest nació el 12 de octubre de 1946 en Detroit. A la edad de 11 años se mudó con su familia a Arlington, Texas. Se graduó de Grand Prairie High School, y luego recibió una Licenciatura en Artes de la Universidad de Texas en Arlington en 1968. Trabajó durante muchos años en el negocio hotelero, pero finalmente regresó a la universidad para obtener su maestría en 1985 y su Doctorado 1990.

Sechrest murió de insuficiencia cardíaca el 30 de octubre de 2008. Le sobrevivieron su esposa y dos hijos de un matrimonio anterior.

Bibliografía seleccionada
 "White's Free Banking Thesis: A Case of Mistaken Identity". Review of Austrian Economics. November 1987, Vol. II, 247–57.
 "The Internal Paradigm of an Austrian Economist: Economics As If Reality Mattered". South African Journal of Economic and Management Sciences. November 1988, Vol. I, 1–13.
 "Free Banking vs. Central Banking: A Geometrical Analysis". South African Journal of Economic and Management Sciences. November 1989, Vol. II, 83–97.
 "Free Banking in Scotland: A Dissenting View". Cato Journal. Winter 1991, Vol. 10, No. 3, 799–808.
 "The Austrian Conception of Money: An Econometric Exercise". South African Journal of Economic and Management Sciences. Summer 1993, Vol. 11, 13–28.
 "Internal Marketing: The Key for External Marketing Success". Journal of Services Marketing. 1994, Vol. 8, No. 4, 5–13. Co-authored with Walter Greene and Gary Walls.
 "Delegating Pricing Authority in Mature Industries". Review of Business. Fall 1996, Vol. 18, No. 1, 19–24. Co-authored with Walter Greene and Gary Walls.
 "Purchasing Power Parity: An Alternative Approach". South African Journal of Economic and Management Sciences. Winter 1996, Vol. 19, 35–50.
 "Austrian and Monetarist Business Cycle Theories: Substitutes or Complements?". Advances in Austrian Economics. Fall 1997, Vol. 4, 7–31.
 "The Irrationality of the Extended Order: The Fatal Conceit of F. A. Hayek". Reason Papers. Fall 1998, No. 23, 38–65.
 Free Banking: Theory, History, and a Laissez-Faire Model. Westport, Connecticut: Quorum Books. 1993.
 "Jean-Baptiste Say: Neglected Champion of Laissez-Faire". In 15 Great Austrian Economists. Edited by Randall G. Holcombe. Auburn, Alabama: Ludwig von Mises Institute. 1999.
 "Rand, Anarchy, and Taxes". Journal of Ayn Rand Studies. Fall 1999, Vol. 1, No. 1, 87–105.
 "Taxation and Government Are Still Problematic". Journal of Ayn Rand Studies. Fall 2000, Vol. 2, No. 1, 163–87.
 "Capital, Credit, and the Medium Run". Quarterly Journal of Austrian Economics. Fall 2001, Vol. 4, No. 3, 63–77.
 "Privateering and National Defense: Naval Warfare for Private Profit". In The Myth of National Defense: Essays on the Theory and History of Security Production. Edited by Hans-Hermann Hoppe. Auburn, Alabama: Ludwig von Mises Institute. 2003.
 "Public Goods and Private Solutions in Maritime History". Quarterly Journal of Austrian Economics. Summer 2004, Vol. 7, No. 2, 3–27.
 "Private Provision of Public Goods: Theoretical Issues and Some Examples from Maritime History". ICFAI Journal of Public Finance. August 2004, Vol. II, No. 3, 45–73.
 "Praxeology, Economics, and Law: Issues and Implications". Quarterly Journal of Austrian Economics. Winter 2004, Vol. 7, No. 4, 19–40. Reprinted in Philosophers of Capitalism: Menger, Mises, Rand, and Beyond. Edited by Edward W. Younkins. Lanham, Maryland: Lexington Books. 2005.
 "Alan Greenspan: Rand, Republicans, and Austrian Critics". Journal of Ayn Rand Studies. Spring 2005, Vol. 6, No. 2, 271–97.
 "Ayn Rand Among the Austrians". Journal of Ayn Rand Studies. Spring 2005, Vol. 6, No. 2, 241–50. Co-authored with Chris Matthew Sciabarra.
 "Public Goods and the Non-Neutrality of Taxes". ICFAI Journal of Public Finance. May 2005, Vol. III, No. 2, 62–71.
 "Explaining Malinvestment and Overinvestment". Quarterly Journal of Austrian Economics. Winter 2006, Vol. 9, No. 4, 27–38.
 "Atlas, Ayn, and Anarchy: A is A is A". In Ayn Rand's Atlas Shrugged: A Philosophical and Literary Companion. Edited by Edward W. Younkins. Burlington, Vermont: Ashgate Publishing. 2007.
 "Privately Funded and Built U.S. Warships in the Quasi-War of 1797–1801". The Independent Review. Summer 2007, Vol. 12, No. 1: 101–113.

Referencias

Nacidos en 1946
Fallecidos en 2008
Economistas de la escuela austriaca
Nacidos en Detroit

redpajama_set_name: RedPajamaWikipedia


text:
Home / Afghanistan / US defense secretary Mattis asked to present long-term Afghan strategy
US defense secretary Mattis asked to present long-term Afghan strategy
Posted by: The Pashtun Times in Afghanistan, Latest News, US July 15, 2017 0 22 Views
WASHINGTON: The National Defense Authorization Act (NDAA) for 2018, as passed by the US House of Representatives on Friday, requires the defense secretary to provide an Afghan strategy beyond five years.
"It directs the secretary of defense to provide an Afghanistan strategy that will look beyond the next five years to describe the trajectory of US efforts in Afghanistan and assess the timeline and total resources necessary to achieve US objectives," the House Armed Services Committee said.
Passed by 344/81 votes, NDAA-2018 provides for a robust Afghan Security Forces Fund to support the Afghan allies who have suffered significant losses in the fight against the Taliban and terrorist organisations.
The fund provides for enhancements in the Afghan Air Force's fixed and rotary wing fleet and supports the expansion of the Afghanistan Special Security Forces. At the same time the bill provides to support for President Ghani's anti-corruption efforts.
It encourages the Office of the Secretary of Defense to develop strategies to modernize analog flight and crew advisory instruments in the UH–60A/L aircraft bound for Afghanistan Aviation Forces.
At the same time, the House continued with tough condition for US aid to Pakistan. It said of the total reimbursement and support for Pakistan from October 1, 2017 to December 31, 2018, $400.0 million would not be eligible for a waiver unless the secretary of defense certifies that Pakistan continues to conduct operations against the Haqqani Network in North Waziristan.
One of the legislative amendments proposes withholding reimbursements to Pakistan unless the secretary can certify the country is not providing military, financial, or logistical support to any individuals designated by the US as a terrorist operating in Pakistan or Afghanistan.
NDAA also requires that the Pentagon to assess Pakistan's support for known terrorists before handing over US dollars to Islamabad, Congressman Ted Poe said.
"It is well known that Pakistan is a Benedict Arnold ally who supports multiple terrorist organisations, including groups that target Americans working to stabilise Afghanistan. But current limitations on military reimbursement funding to Pakistan only apply to the Haqqani Network," Poe said.
Previous: Pashtun leader Mehmud Khan Achakzai warns Pakistan regarding persistent interference in Afghanistan
Next: No honour in killing: Remembering Qandeel Baloch on her first death anniversary


Download 10 Good Reasons To Mentor A Student Teacher Advantages For Supervising Mathematics Teachers And Their Classes or read 10 Good Reasons To Mentor A Student Teacher Advantages For Supervising Mathematics Teachers And Their Classes online books in PDF, EPUB and Mobi Format. Click Download or Read Online button to get 10 Good Reasons To Mentor A Student Teacher Advantages For Supervising Mathematics Teachers And Their Classes book now. This site is like a library, Use search box in the widget to get ebook that you want.
How to Download 10 Good Reasons To Mentor A Student Teacher Advantages For Supervising Mathematics Teachers And Their Classes : Press button "Download" or "Read Online" below and wait 20 seconds. This time is necessary for searching and sorting links. This site is like a library, you could find million book here by using search form widget.


← What's So Great About Hackathons?
On Saturday, December 20th, 2014 at approximately 1:30p.m. I would like to invite you to join me in toasting my 20th anniversary of cheating death.
I made this toast ten years ago in the year that I turned 30; this year we celebrate another decade attained.
This entry was posted in Life and tagged event, health, people. Bookmark the permalink.


text:
Senantes è un comune francese di 642 abitanti situato nel dipartimento dell'Eure-et-Loir nella regione del Centro-Valle della Loira.

Società

Evoluzione demografica

Note

Altri progetti

Senantes


An adenoidectomy is a quick operation to remove the adenoids. Adenoids are small lumps of tissue located at the back of the throat, above the tonsils.
Sometimes a child's adenoids can become swollen or enlarged. For most children, this will only cause mild discomfort and will not require any specific treatment.
An adenoidectomy is usually performed by an ear, nose and throat (ENT) surgeon. The operation is quick and carries very risks.
An adenoidectomy is a low-risk procedure that rarely causes any complications. It is a relatively common operation that is quick and easy to carry out.
Most children find their throat feels very sore after an adenoidectomy but this is perfectly normal. Your child will usually be given painkillers while in hospital to help ease discomfort.


text:
CharterUP stepping in to aid motorcoach industry
April 5, 2020 • by MET Staff
CharterUP is offering this program to bus operators for free for a duration of three months, ending June 30.
Charter bus reservation company CharterUP launched the Bus Provider Assistance Program, which aims to provide advice and assistance to bus companies in need during the coronavirus pandemic — free of charge.
Due to COVID-19 and its social distancing measures, motorcoach operators have seen a halt in business resulting in significant financial strain during what is typically a "busy season" for most bus businesses.
To help counteract this, Armir Harris, founder and CEO of CharterUP, has chosen to offer this Bus Provider Assistance Program free of charge. Having been in the bus business for 16 years himself, Harris feels an innate connection to bus providers and wants to see the industry succeed. The program will provide guidance to struggling bus companies from CharterUP's own in-house insurance and financial experts.
"Our company is fortunate to be in a financial position to weather the storm in the long run. Now, I want to make sure that all companies in this industry have that same chance," says Harris. "If we all pool our knowledge, we can come out ahead of this when it's all over."
Using CharterUP's own experience as a source, the company's experts are taking note of successful planning strategies that have helped the business remain strong in the wake of the COVID-19 pandemic. With this in mind, advice and services to motorcoach operators will include:
Assistance with SBA Disaster Relief Loans.
Assistance with SBA's Payroll Protection Program.
How to manage finances after the pandemic assistance with business continuity insurance.
To get in touch with a CharterUP expert or inquire about the program's details call 855-920-2287 or email info@charterup.com.
Read more about CharterUP COVID-19 financial issues motorcoach safety SBA loans


text:
Lady Gaga's LP won't be 'deluxe'
Lady Gaga will not release a ''deluxe'' version of 'Born This Way' because she hates the word, although she has previously sold a bonus edition of her second album 'The Fame Monster'.
by : Elle Canada- Apr 13th, 2011
Lady Gaga will not release a "deluxe" version of new album 'Born This Way'.
Despite releasing a bonus edition of her second album 'The Fame Monster', the pop star now claims to hate the word and has insisted she won't have it on any of her future works.
Discussing her new LP she told a colleague: "I don't want to use the word deluxe on the album I hate that word."
When her companion added, "It infers that the other one is of lesser value," Gaga agreed, saying "right".
The 25-year-old pop star revealed she has finally finished her eagerly awaited third album after putting in a marathon 72-hour final stint at it and couldn't wait to celebrate by cuddling with her "beautiful mother".
She revealed in her Gagavision video: "I have been up for 72 hours finishing this album and I finally finished the record. I love it so much and I now have a show and then I'm going to take two days off in NYC to cuddle in bed with my beautiful mother. I may get drunk with my friends too."
Gaga is getting ready to release her second single 'Judas' from the LP and says she did all the artwork herself.
She explained: "I graphic designed the 'Judas' single cover myself, in Word, and photographed the image with my cellphone for texture."


Shanan Estreicher is a composer, songwriter, and educator living in New York City. He studied music at the Manhattan School of Music, Mannes College, and The Aaron Copland School of Music at Queens College.
He has composed chamber music, art songs, as well as music for theater, TV, and film. His compositions have been featured on NBC, Lifetime, and Fox. As a songwriter he released five albums as a solo artist and with the alt-country group The Brown Trousers. His musical Once 'Round the Circle is currently in development and was recently workshopped in New York City as part of the Emerging Artists Theatre's New Work Series. Shanan has collaborated extensively with Grammy Award-winning producer Brian Forbes.
This 2018 - 2019 season will include premieres of his Songs of Emily Dickinson for Sarah Shafer (Metropolitan Opera, San Francisco Opera) and Chamber Orchestra of New York at Carnegie Hall, and two pieces commissioned by the Composers Concordance.
One of Shanan's greatest joys is sharing his passion for music with children. For twelve years he has taught music at a public school in Queens, NY. The documentary Rise Up and Sing—The Movie chronicles his work with the P.S./I.S. 127 Chorus. He is also the founder and director of the Queens County Choral Festival for elementary and middle school students.
As a founding board member of Chamber Orchestra of New York, Shanan has helped to lead the ensemble to international success and acclaim. He served as Co-Artistic Producer for the orchestra's Naxos recordings of Respighi's "The Birds" and Ralph Vaughan Williams's "The Lark Ascending," as well as upcoming Naxos releases of Respighi's "Ancient Airs and Dances" and Salvatore Di Vittorio's symphonic poems. Shanan has also begun an educational outreach program Maestro Juniors for the orchestra which brings live classical music performances to title-one schools in New York City.