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Theater Review: "Fade"
Jean Lowerison - SDGLN Theater critic
Quasi Studios
Tanya Saracho's fascinating hot-button play about ethnicity, class and prejudice.
Lucia, a young novelist-turned-TV writer, moves into an office for her new job. When the bookshelf collapses under the weight of what she's put on it, the building's janitor Abel puts it back up.
In casual conversation, Lucia (Sofia Sassone) – a Mexican-born transplant to the U.S. – complains to Abel about a waitress who gave her not only English but attitude when Lucia tried to make her feel more comfortable by ordering in Spanish.
"It was obvious she spoke Spanish," she says.
"What was obvious about it?" counters Abel (Javier Guerrero), a self-described Mexican, born and still living in the El Sereno area of East Los Angeles.
This is the tipoff that playwright Tanya Saracho will take us into contentious hot-button territory like ethnicity, class and prejudice in her fascinating one-act, two-person play "Fade."
We see Lucia ("not pronounced Loo-sha") and Abel ("not pronounced able") only after hours in the studio, while he cleans up and she tries to adjust to her new, presumably collaborative job after living the lonely life of a novelist.
Actually, though, she's not even sure she belongs here. "I thought I'd be writing," she wails. "But there's zero writing involved. There's just been sitting and talking."
It gets worse when her boss calls her in to ask her to explain to his Spanish-speaking maid just how he wants his magazines laid out in the morning, and when he wants his coffee.
The fact that Lucia has published a book doesn't give her any advantages here. In fact, she's soon fuming from a colleague's comment that "you know you're the diversity hire, right?"
(Let it be said for the record that Saracho is no newcomer to TV writing: she's written for HBO's "Girls" and "Looking.")
But Lucia will suffer the indignities of the newbie even worse because she's the Latina newbie.
She and Abel have a lot in common in that regard: he's Latino as well, and even lower on the work pecking order. Stereotypes abound here, but are played with such honesty that you'll see them as real.
Lucia perseveres and finally gets a chance to write a script, or at least a treatment for one. By this time she's learned some interesting things about Abel. He was a Marine and a fireman, for one. She thinks those things might make an interesting character, and Abel gives her permission to use them.
Saracho's engaging way with words – and the actors' obvious but unintrusive commitment – keep the action riveting when it could easily come off as preachy.
Director Maria Patrice Amon keeps the pace snappy and sound designer Lily Voon chimes in with well-placed tunes as well.
Scene changes are defined as much by Mextly Almeda's fine lighting as anything else, and Kristen Flores contributes a basic office set of office and hall that make clear the class distinctions.
Moxie (which specializes in theater by and about women) has staged "Fade" in collaboration with TuYo Theatre, a brand new Latinx company of which Amon is co-founder.
They've given us the San Diego premiere of a fine new play. Let's hope more such collaborations are in the future.
"Fade" plays through November 11, 2018, at Moxie Theatre, 6663 El Cajon Boulevard.
Thursday at 7:30 pm; Friday and Saturday at 8 p.m.; Sunday at 2 pm
Tickets: (858) 598-7620 or www.moxietheatre.com
Tags: Jean Lowerison
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To deliver an online training course in E-Working over an agreed period as per course objectives and syllabus.
To provide a response to e-mail or Web site enquiries within 24 hours. This may from time-to-time involve sending a holding reply or acknowledgement, and the query will be dealt with as soon as possible.
To provide all training resources required for the programme.
To provide telephone support in case of emergencies.
To review all CVs submitted in advance by the required deadline, and provide individual feedback on each individual CV.
To ensure confidentiality when dealing with any issues that might arise within the programme.
What we expect from participants…..


The Very Rev Albert Bogle urges congregations to give permission to change.
WE'VE just had another General Assembly of the Church of Scotland. So many words spoken, plans and programmes reported upon, questions asked, motions debated and instructions given and received. If you didn't know better you'd think, judging by our organisational ability, that we were a thriving church.


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Ann Lindsay Aymer1
F, #30431, b. 1924, d. 5 October 2019
Ann Lindsay Aymer was born in 1924.2 She was the daughter of Alexander Lindsay Aymer and Mary Rose.1,3 She married, firstly, Major Robert Lee Bullard III before 1949.1 She married, secondly, Charles Melville McLaren, 3rd Baron Aberconway, son of Henry Duncan McLaren, 2nd Baron Aberconway and Christabel Mary Melville Macnaghten, on 15 October 1949.1 She died on 5 October 2019.2
From before 1949, her married name became Bullard.1 Her married name became McLaren. After her marriage, Ann Lindsay Aymer was styled as Baroness Aberconway on 23 May 1953.
Child of Ann Lindsay Aymer and Major Robert Lee Bullard III
Robin Lindsay Bullard+4
Child of Ann Lindsay Aymer and Charles Melville McLaren, 3rd Baron Aberconway
Hon. Michael Duncan McLaren+1 b. 29 Nov 1958
[S8] BP1999 volume 1, page 2. See link for full details for this source. Hereinafter cited as. [S8]
[S9243] Justin Downes, "re: Lindsay Family," e-mail message to Darryl Roger LUNDY (101053), 13 Jan 2021. Hereinafter cited as "re: Lindsay Family."
Katherine Mildred Marshall1
F, #30432, b. October 1849, d. January 1911
Katherine Mildred Marshall was born in October 1849 at 16 Gloucester Square, Paddington, London, England.1 She was the daughter of George Marshall and Elizabeth Helen Gore.1 She died in January 1911 at age 61 at Boston, Lincolnshire, England.1
[S3706] David Barttelot, "re: Crosland Family," e-mail message to Darryl Roger LUNDY (101053), 7 April 2009. Hereinafter cited as "re: Crosland Family."
Hon. Michael Duncan McLaren1
Hon. Michael Duncan McLaren was born on 29 November 1958.1 He is the son of Charles Melville McLaren, 3rd Baron Aberconway and Ann Lindsay Aymer.1 He married Caroline Jane Stacey, daughter of Air Chief Marshal Sir John Stacey and Frances Jean Faucett, on 25 May 1985.1
He was educated at Eton College, Windsor, Berkshire, EnglandG.1 He graduated from Cambridge University, Cambridge, Cambridgeshire, EnglandG, in 1980 with a Bachelor of Arts (B.A.)1 He was admitted to Middle Temple in 1981 entitled to practise as a Barrister-at-Law.1 He lived in 1999 at 27 Phillimore Gardens, London, EnglandG.1
Children of Hon. Michael Duncan McLaren and Caroline Jane Stacey
Angus John Melville McLaren1 b. 21 Oct 1987
Iona Ann Mariel McLaren1 b. 20 Feb 1991
Hamish Charles Duncan McLaren1 b. 23 Nov 1993
Hon. Julia Harriet McLaren1
F, #30434, b. 22 September 1942
Hon. Julia Harriet McLaren was born on 22 September 1942.1 She is the daughter of Charles Melville McLaren, 3rd Baron Aberconway and Deirdre Knewstub.1 She married Captain Charles Walter Hayes Ridley in 1969.1
She was educated at University of Grenoble, Grenoble, FranceG.1 From 1969, her married name became Hon. Ridley.1 She lived in 1999 at Rome, ItalyG.1
Children of Hon. Julia Harriet McLaren and Captain Charles Walter Hayes Ridley
Emma Jane Ridley1 b. 1970
Harriet Deidre Ridley1 b. 1971
Casper Charles Ridley1 b. 1977
Dr. Hon. Caroline Mary McLaren1
F, #30435, b. 24 October 1944
Dr. Hon. Caroline Mary McLaren was born on 24 October 1944.1 She is the daughter of Charles Melville McLaren, 3rd Baron Aberconway and Deirdre Knewstub.1 She married, firstly, Raimund Guernsey Sargent, son of Winthrop Sargent, III, on 8 February 1962.1 She and Raimund Guernsey Sargent were divorced after 1965.1 She married, secondly, Dr. Graham Charles Steele in 1978.1 She and Dr. Graham Charles Steele were divorced after 1978.1 She married, thirdly, William Howard between 1979 and 1999.1
From 8 February 1962, her married name became Sargent.1 She graduated from Imperial College, London, EnglandG, with a Bachelor of Science (B.Sc.)1 She graduated from Imperial College, London, EnglandG, with a Diploma of the Imperial College.1 She graduated from Imperial College, London, EnglandG, with a Doctor of Philosophy (Ph.D.)1 She was appointed Fellow, Linnean Society of the Imperial College (F.L.S.)1 She was a botanist.1 From 1978, her married name became Steele.1 From between 1979 and 1999, her married name became Howard.1 She lived in 1999 at Forest House, Barbados Hill, Tintern, Monmouthshire, WalesG.1
Children of Dr. Hon. Caroline Mary McLaren and Raimund Guernsey Sargent
Dominic Fitzwilliam Sargent1 b. 30 Aug 1963
Orlando Gorham Sargent1 b. 4 Nov 1964
Sir Henry Foley Grey, 7th Bt.1
M, #30436, b. 21 January 1861, d. 17 December 1914
Sir Henry Foley Grey, 7th Bt. was born on 21 January 1861.2 He was the son of Sir Henry Edward Francis Lambert, 6th Bt. and Eliza Catherine Hervey.2 He married Catherine Sarah Payne, daughter of Reverend Alfred Payne, on 14 June 1883.2 He died on 17 December 1914 at age 53.2
He was given the name of Henry Foley Lambert at birth.2 He succeeded as the 7th Baronet Lambert, of London [G.B., 1711] on 5 June 1872.1 He held the office of High Sheriff of Worcestershire in 1901.2 He gained the rank of Lieutenant-Colonel in the Worcester Yeomanry.2 He was awarded the Territorial Decoration (T.D.)2 On 27 July 1905 his name was legally changed to Henry Foley Grey by Royal Licence.2 He held the office of Deputy Lieutenant (D.L.) of Worcestershire.2 He held the office of Justice of the Peace (J.P.) for Staffordshire.2 He held the office of Justice of the Peace (J.P.) for Worcestershire.2 He held the office of Major of Stourbridge in 1914.2
Children of Sir Henry Foley Grey, 7th Bt. and Catherine Sarah Payne
Dorothy Catherine Grey3 b. 7 Sep 1884
Phyllis Kathleen Grey3 b. 14 Jun 1887
Joan Cecil Grey3 b. 18 May 1892, d. 4 Jun 1972
Sir John Foley Grey, 8th Bt.+2 b. 8 Jul 1893, d. 17 Mar 1938
Geraldine Ida Grey1 b. 13 Jun 1898, d. 11 Oct 1940
Mary Alice Grey+3 b. 8 Sep 1899
[S2] Peter W. Hammond, editor, The Complete Peerage or a History of the House of Lords and All its Members From the Earliest Times, Volume XIV: Addenda & Corrigenda (Stroud, Gloucestershire, U.K.: Sutton Publishing, 1998), page 44. Hereinafter cited as The Complete Peerage, Volume XIV.
Hamilton Beckett1
M, #30437, b. 15 October 1829, d. 1883
Hamilton Beckett was born on 15 October 1829.2 He was the son of Henry Beckett and Mary Lyle.3 He married Hon. Sophia Clarence Copley, daughter of John Singleton Copley, 1st Baron Lyndhurst and Sarah Garay Brunsden, on 14 December 1854.2 He died in 1883.2
Children of Hamilton Beckett and Hon. Sophia Clarence Copley
Constance Mary Beckett+1 d. 8 Feb 1932
Henry Lyndhurst Beckett3 b. 8 Apr 1857, d. 1896
[S6] G.E. Cokayne; with Vicary Gibbs, H.A. Doubleday, Geoffrey H. White, Duncan Warrand and Lord Howard de Walden, editors, The Complete Peerage of England, Scotland, Ireland, Great Britain and the United Kingdom, Extant, Extinct or Dormant, new ed., 13 volumes in 14 (1910-1959; reprint in 6 volumes, Gloucester, U.K.: Alan Sutton Publishing, 2000), volume I, page 14. Hereinafter cited as The Complete Peerage.
Hon. Sophia Clarence Copley1
F, #30438, d. 25 December 1911
Hon. Sophia Clarence Copley was the daughter of John Singleton Copley, 1st Baron Lyndhurst and Sarah Garay Brunsden.1 She married Hamilton Beckett, son of Henry Beckett and Mary Lyle, on 14 December 1854.2 She died on 25 December 1911.2
From 14 December 1854, her married name became Beckett.
Children of Hon. Sophia Clarence Copley and Hamilton Beckett
Elizabeth Cecile Sophia Norman1
F, #30439, d. 4 August 1921
Elizabeth Cecile Sophia Norman was the daughter of Reverend Frederick John Norman and Lady Adeliza Elizabeth Gertrude Manners.1 She married George James Drummond, son of George Drummond and Marianne Portman, on 6 July 1876.1 She died on 4 August 1921.1
Her married name became Drummond.
Children of Elizabeth Cecile Sophia Norman and George James Drummond
Cécile Elizabeth Drummond+1 b. 7 Aug 1878, d. 17 Sep 1948
Adeliza Beatrix Drummond+1 b. 20 Jun 1879, d. 1 Jun 1959
Ida Mary Drummond+1 b. 26 Jun 1880, d. 11 Dec 1966
Euphemia Mabel Drummond+1 b. 30 Jun 1881, d. 13 Sep 1964
George Henry de Vere Drummond+1 b. 3 Mar 1883, d. 12 Oct 1963
Lieutenant David Robert Drummond+1 b. 30 Oct 1884, d. 3 Nov 1914
Captain Alexander Victor Drummond+1 b. 20 Oct 1888, d. 29 Apr 1937
Walter Drummond, Master of Drummond1
M, #30440, d. 1518
Walter Drummond, Master of Drummond was the son of William Drummond, Master of Drummond and Lady Isabel Campbell.2 He married Lady Elizabeth Graham, daughter of William Graham, 1st Earl of Montrose and Janet Edmonstone, in February 1513/14.1 He died in 1518.1
He was styled as Master of Drummond between 1490 and 1518.1
Child of Walter Drummond, Master of Drummond and Lady Elizabeth Graham
David Drummond, 2nd Lord Drummond+2 b. bt 1515 - 1517, d. 1571
[S6] G.E. Cokayne; with Vicary Gibbs, H.A. Doubleday, Geoffrey H. White, Duncan Warrand and Lord Howard de Walden, editors, The Complete Peerage of England, Scotland, Ireland, Great Britain and the United Kingdom, Extant, Extinct or Dormant, new ed., 13 volumes in 14 (1910-1959; reprint in 6 volumes, Gloucester, U.K.: Alan Sutton Publishing, 2000), volume IV, page 470. Hereinafter cited as The Complete Peerage.

redpajama_set_name: RedPajamaCommonCrawl


Home » Manufacturer » Sensortech Systems, Inc.
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Sensortech's success is due to our leading edge manufacturing processes, comprehensive testing and quality control standards, a diverse range of applications, and superior customer support. We are a full design, development and manufacturing facility specializing in Near Infrared Reflectance (NIR) and Radio Frequency (RF) technology. Through our expertise in both disciplines of moisture measurement technologies we apply the correct instrumentation for your manufacturing process and desired moisture measurement outcome.
Sensortech's instruments have the reputation for being maintenance free and typically require minimal servicing for at least a decade after installation. Their operation is user friendly and and delivered with instrument pre-calibrated and ready to install as a turn-key package.


It's one of those transparently ridiculous perks. Like how free sodas in the office are an amazing perk. Or how long meetings are fun if there's "free" pizza.
Obviously, the vacation is not unlimited. So why say that it is?
There are certainly companies out there that have the best intentions for their employees. But stating that you have an unlimited vacation policy and leaving it at that is frankly irresponsible.
It's a means of weaponising ambiguity into guilt. Everyone knows it's not unlimited, because you can't take 3 months off. But because there's no boundary, the real limit has to be found by stressfully, riskily probing it.
I think a much better policy is a minimum vacation policy, with unlimited discretionary days on top.
We require a minimum of [high number] vacation days are taken by each employee, and we allow unlimited additional vacation days beyond that.
Now that is a true perk.


The Nasdaq last week finally hit an all-time high, surpassing the 5,000 level achieved 15 years ago in March 2000. It took much longer for the Nasdaq to hit record highs than the Dow or the S&P 500 due to the dot-com frenzy in 2000 that sent the technology-heavy Nasdaq soaring.
The Nasdaq record set off another round of predictions by the doomsayers of another "imminent crash." In the past few months, we've seen dire forecasts, including one from Congressman Ron Paul. Many of the warnings are aimed at seniors who are vulnerable to irresponsible scare tactics.
In addition, the Nasdaq has nearly quadrupled in six years – at a time when the Cassandras were warning of another collapse. How wrong they were!
There's a big difference between the Nasdaq of 2000 and today. Back then, the high-tech stock index was selling at 175 times earnings. Today, it is selling for 30 times earnings.
Are stocks too expensive? They are certainly fully priced, and today's market is vulnerable. We haven't had a serious correction in years.
Yesterday, the first-quarter real Gross Domestic Product (GDP) growth rate came in at an anemic 0.2%, confirming my view that the economy has slowed to a crawl.
Last week, the quarterly Gross Output (GO) and B2B (business-to-business spending) data that I have been championing were released by the federal government. Real GO, which measures spending at all stages of production, rose only 2.6% on an annualized basis, and B2B climbed only 2.5%, much slower than past quarters.
It is not enough to cause a recession, but it's enough to worry Fed Chair Janet Yellen and her colleagues at the U.S. central bank to extend its easy-money policies. In short, the Fed won't raise rates any time soon and, in fact, will engage in printing more money.
Last weekend, I talked to Robert Kuttner, former chief economist at BusinessWeek, who told me that the Fed's low interest rate policy has been good for the economy on net balance. He will be the defending attorney when we put "The Fed on Trial" at FreedomFest on July 10 (see our newly designed website: www.FreedomFest.com).
Certainly, low rates have been good for the stock market and our portfolio. And I think that trend will continue, especially for dividend-paying stocks in Forecasts & Strategies. It is the golden age of income investment.
Remember, the stock market is always looking forward. With a weak economy, the Fed is unlikely to raise rates any time soon and will continue to pump new money into the system. Much of that new money is likely to go into the stock market.


Weak Response For Mr. Majnu @ Advance Bookings!
A film's pre release buzz cannot be gauged by the posts across social media platforms or views for its promos on YouTube.
Advance booking trends will give the clear picture of how much the ticket paying public is interested in catching the earliest show of an upcoming release.
Going by the advance bookings trends on online ticketing portals, Akhil Akkineni's upcoming Friday release Mr. Majnu has been receiving lukewarm response all over.
Looks like it is the effect of Akhil's previous failures. Mr. Majnu will need a good word of mouth to set the cash registers ringing.
Thankfully, Mr. Majnu has the advantage of solo release, but it will have to withstand the F2 blitz, which is showing no signs of slowing down.
F2 will continue to rake in moolah at least for another weekend. Mr. Majnu has a job on hands to pull audiences to the theaters in big numbers.


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La nazionale di beach soccer della Bielorussia rappresenta la Bielorussia nelle competizioni internazionali di beach soccer.

Collegamenti esterni
Team profile on Beach Soccer Russia
Squad

Bielorussia
Beach soccer

redpajama_set_name: RedPajamaWikipedia


BT have reneged on their commitment to Loyal Broadband customers having access to BT Sports for FREE.
They now send you a letter regarding the demand for payment less than 9 WORKING days prior including day of delivery] to increasing your bill [DD] during the summer period to ensure they ensnare as many as possible who may not be able to respond in time!
They even have the cheek [if you check your bill] to state "BT Sport discount for BROADBAND LOYALTY" !
Let's be honest they prove that BT is in it for the greed and abuse their monopoly position [Openreach/BT] to basically demand and force residential customers, especially where they have made it difficult for other providers to supply through their exchanges!
VIRGIN please come to Margate!!


"Scholars and thinkers wake up early in the morning and contemplate. Also, those who desire wealth wake up early and get to work".
Due to the fact that there's no universal rule for "Ideal sleeping habit" to follow, generally, people follow the habits of successful people or Entrepreneurs. Successful Entrepreneurs never underestimate the significance of sound sleep. They wish to be focused, emotionally balanced, and quick-witted in all areas of their business. In this article, I have tried to explore about sleep, its importance for an Entrepreneur and have suggested a few important tips for having a sound solid deep sleep which is very important for staying calm and focus at their work.
Should sleeping hours be deducted for being productive?
Like all people in the world, Entrepreneurs do have to take care of things besides their routine work. So balancing both their official obligations and their business, project, etc. make them a very busy personality. This pattern is found common in Entrepreneur or any professional in today's fast-moving world where the sleeping habits and patterns of quantity and quality are affected by a variety of cultural, behavioral, social, pathophysiological, psychological, and environmental influences.
According to a new study, those who are early birds (early sleepers and risers) are less prone to develop stress, heart disease, kidney disease, high blood pressure, diabetes, Obesity, and stroke. Early birds are biologically programmed, Stable Circadian rhythms controlled by body's biological clocks, to be less susceptible to depression and schizophrenia and might just be happier than night owls (late sleepers and late risers).
Our ancestors used to follow a fixed pattern to have quality sleep and probably this was the key for their healthy physical and mental well-being. An inspirational quote of Benjamin Franklin, (1706-1790), one of the famous figures of American History quotes about the value of early rising and health "Early to Bed and Early to Rise Makes a man Healthy, Wealthy and wise".
Sun is the ultimate source of energy. Recent studies have pointed out that the exposure to sunlight or bright indoor lights during the morning hour's helps in having sleep better at night. The later you wake-up after sunrise the slothful and lethargic you will be. The closer you wake up to sunrise, preferably before sunrise it will make you active and zestful. It can be observed in the dynamism of animals, birds, and most of the elders in the family as they all wake up either at the stroke of sunrise or earlier than that.
Sleep is a complex and dynamic process which is the major part of our daily routine. We spend about one-third of the day in sleep. Quality sleep and getting a sufficient amount of it at the right times is as essential to survival as food and water. Without sleep, the pathways in our brain are not formed or maintained which allow us to learn and create new memories, and it's tougher to concentrate and respond swiftly.
Sleep is of paramount importance to a number of brain functions, like how nerve cells (neurons) communicate with each other. In fact, our brain and body remain substantially active while we sleep properly. Recent findings suggest that sleep plays a housekeeping role that eliminates toxins in our brain that is build up while we are awake.
Everybody requires sleep, but its biological purpose remains a mystery. Sleep affects altogether every type of human body tissue and system right from the brain, heart, stomach, and lungs to the central nervous system, immune system, respiratory system, digestive system, cardiovascular system, and Endocrine system.
Getting sufficient sleep is good for health. Infants generally require about 16-18 hours a day, while teenagers (13-18 years old) require about 9 hours on average. For most adults(above 18 years old), 7 to 8 hours a night appears to be the substantial amount of sleep, although some people may require as few as 5 hours or as long as 10 hours of sleep each day. The Prime Minister of India, Mr. Narendra Modi, a brilliant statesman has gained the ability to have a sound deep sleep but only for 3.5 hours.
It's very important to Set a schedule and go to bed and wake up at the same time each day.
Before going to bed nearly a few hours before, Exercise about 20 to 30 minutes a day.
Try a warm bath, reading, or another relaxing routine before going to bed.
Avoid bright lights and loud sounds, keep the room at a comfortable temperature and don't watch Television or have a computer in your bedroom to create a room for sound sleep.
If you are unable to go for sleep, do something else, like reading or listening to music, until you feel tired. Avoid lying in bed awake.
Visit a clinician for any problem in sleeping or for unusual tiredness feeling during the day. Most sleep disorders are effectively curable.
Sound sleep is one of the pillars of our health system along with good nutrition and regular physical exercise. Relaxation techniques like Meditation, yoga, and music have all proved effective for stress and sleep disorders. Successful entrepreneurs make it a priority to get sufficient sleep every night for self-control and being focused at their work.


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In the study of the human mind, intellect refers to, describes, and identifies the ability of the human mind to reach correct conclusions about what is true and what is false in reality; and how to solve problems. Derived from the Ancient Greek philosophy term nous, intellect derived from the Latin intelligere ("to understand"), from which derives the term intelligence in the French and English languages. The discussion of intellect is in two areas of knowledge that concern the relation between intelligence and intellect.

 In classical philosophy and in medieval philosophy the intellect (nous) is the subject of the question: How do people know things? In Late Antiquity and in the Middle Ages, the intellect was the conceptual means of reconciling the religious faith of monotheism with the facts of philosophy and science about Nature, a reconciliation that would make the intellect the conduit between the human soul, and the divine intellect of the cosmos. In the Late Middle Ages, philosophers developed the distinction that intelligence is in two modes passive intellect and active intellect.

 In psychology and in neuroscience, the controversial Theory of Multiple Intelligences applies the terms intelligence (emotion) and intellect (mind) to describe how people understand the world and reality.

Intellect and intelligence
As a branch of intelligence, intellect concerns the logical and the rational functions of the human mind, and usually is limited to facts and knowledge. Additional to the functions of linear logic and the patterns of formal logic the intellect also processes the non-linear functions of fuzzy logic and dialectical logic.

Intellect and intelligence are contrasted by etymology; derived from the Latin present active participle intelligere, the term intelligence denotes "to gather in between", whereas the term intellect, derived from the past participle of intelligere, denotes "what has been gathered". Therefore, intelligence relates to the creation of new categories of understanding, based upon similarities and differences, while intellect relates to understanding existing categories.

Development of intellect

A person's intellectual understanding of reality derives from a conceptual model of reality based upon the perception and the cognition of the material world of reality. The conceptual model of mind is composed of the mental and emotional processes by which a person seeks, finds, and applies logical solutions to the problems of life. The full potential of the intellect is achieved when a person acquires a factually accurate understanding of the real world, which is mirrored in the mind. The mature intellect is identified by the person's possessing the capability of emotional self-management, wherein he and she can encounter, face, and resolve problems of life without being overwhelmed by emotion.

Real-world experience is necessary to and for the development of a person's intellect, because, in resolving the problems of life, a person can intellectually comprehend a social circumstance (a time and a place) and so adjust their social behavior in order to act appropriately in the society of other people. Intellect develops when a person seeks an emotionally satisfactory solution to a problem; mental development occurs from the person's search for satisfactory solutions to the problems of life. Only experience of the real world can provide understanding of reality, which contributes to the person's intellectual development.

Structure of intellect
In 1955, the psychologist Joy Paul Guilford (1897–1987) proposed a Structural Intellect (SI) model in three dimensions: (i) Operations, (ii) Contents, and (iii) Products. Each parameter contains specific, discrete elements that are individually measured as autonomous units of the human mind. Intellectual operations are represented by cognition and memory, production (by divergent thinking and convergent thinking), and evaluation. Contents are figurative and symbolic, semantic and behavioral. Products are in units, classes, and relations, systems, transformations, and implications.

Intellect in psychotherapy
Intellectualization is a psychotherapeutic method based of intense intellectual focus in order to avoid dealing with a problem that occupies the attention of a person. In psychological praxis, intellectualization is a defense mechanism that blocks feelings in order to prevent anxiety and stress from acting upon and interfering with the psyche of the person, which otherwise would interfere with their normal functioning in real life. As psychotherapy, intellectualization is a rational, dispassionate, and scientific approach towards dealing with and resolving mental problems, which psychologically disturb the person.

The functions of intellectualization involve the Id, ego, and super-ego. The Ego is the conscious aspect of human personality; the Id is the unconscious, animal-instinct aspect; and the super-ego is the control mechanism that mediates and adjusts a person's thoughts and actions and behavior in accordance with the social norms of society. The purpose of intellectualization is to isolate the Id from the real world, and so make the conscious aspects of a person's life the only object of reflection and consideration. Therefore, intellectualization defends and protects the Ego from the Id, the unconscious aspect of human personality that usually is impossible to control.

Socially, intellectualization uses technical jargon and complex scientific terminology instead of plain language; e.g. a physician uses the word carcinoma instead of cancer to lessen the negative impact of a diagnosis of terminal disease — by directing the patient's attention away from the bad news. The different registers of language, scientific (carcinoma) and plain language (cancer), facilitate the patient's acceptance of medical fact and medical treatment, by avoiding an outburst of negative emotions that would interfere with the successful treatment of the disease.

Moreover, the defense mechanism of intellectualization is criticized because it separates and isolates the person from the painful emotions caused by the psychological problem. As such, the defense mechanism subsequently leads to the denial of intuition, which sometimes contributes to the processes of decision-making; a negative consequence of the absence of emotional stimuli can deprive the person of motivation, and lead to a mood of dissatisfaction, such as melancholy; such "emotional constipation" threatens their creativity, by replacing such capabilities with factual solutions.

See also
 Human intelligence
 Intellectualism

References

External links

Concepts in the philosophy of mind
Concepts in epistemology
Intellectualism
Intelligence
Mental content
Mental processes
Metaphysics of mind
Philosophy of psychology
Rational choice theory
Sources of knowledge
Thought


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FOOTBALL | ROD LIDDLE
Forget the Premier League – if you want real drama, look to Championship
Sunday May 31 2020, 12.01am, The Sunday Times
Championship players have been back in training for a week and the season is set to resume on June 20, assuming an absence of those irritating things, events. It will have been almost four months since a ball was kicked in anger: the last game was played on March 8.
The authorities have taken heart from the return of the top two divisions in Germany, Bundesligas 1 and 2, the first major football leagues in the world to have decided that an unpleasant virus is no reason to forsake that most important of all things, kicking a ball around.
The decision to restart did not meet with universal acclaim in Germany, with half of the population opposed. And you have to say, the strictures placed


Join Mel Homer weekdays on Mix. Mel gets you through the day playing all the Greatest Hits from artists like David Bowie, Queen, Dire Straits, Prince, Bon Jovi, Police, Eurythmics, Madonna, Tom Petty, Talking Heads, Crowded House and U2 alongside other bangers that we guarantee you won't have heard on the radio for a very long time. Mel will also keep you up to date with the latest music and sports news, interviews, technology and movie reviews.


Click to enlarge The Frangipanis in Pink Invitation has a fuschia pink backing card with a white insert. The frangipanis trace has a pink centreand wraps around the invitation. It is held together with a pink ribbon. Lovely and Bright. The size is 21cmx9.9cm.


The importance of evidence-based decision-making has become a mantra among those in the research and innovation community who wish to influence public policy. But science and policy don't always make easy companions.
Zhao pointed to recent research suggesting that a modest carbon tax may actually drive up emissions. If the cost is too small, people could actually embrace behaviours that produce GHGs even more, unconsciously believing they've earned the right to do so. "People may be perfectly happy to pay the small fee and feel justified to consume more gas, so the deterrence effect may backfire," Zhao explained. According to this theory, only a hefty tax will motivate citizens and companies to take more carbon-neutral actions.
Of course, research into the effectiveness of the carbon tax is ongoing, but surely no one wants to hear that it should cost even more. Even if the outcomes of research don't conform to convenient narratives, however, science needs to be part of the conversation when policy is being made.
Events like Science Meets Parliament affirm a strategy to make evidence-informed decision-making a stronger reality for Canadian politics: small talk. Informal, low-stakes conversations about research and policy may open doors that then stay open when the stakes are higher.


I cannot count how many Passport reviews I've read lately... mostly from non-blackberry users... in which the writer mentions a "learning curve" in using the keyboard. It's almost like the Passport's keyboard and the words "learning curve" have become the go-to buzz words for anyone writing a review of the phone. I seriously don't get it. What the heck is so hard about using the keyboard? I've had my Passport for only a few days and I find the keyboard to be very intuitive and quite easy to use. I cranked out my first email with no problem. I was too busy thinking about the content of my email to even realize I was flying away on the keyboard.
Sure, sure... I agree... it will take some time to learn all of the "tricks" of the keyboard, but most of these bloggers act like it takes 17 days in order to type an normal email. I swear, someone reading a review could easily walk away with the impression that it's nearly impossible to type an email on the Passport... when the truth is... it's incredibly easy to use it for exactly what it is - a freaking keyboard!!! You want an 'a'? Then press the 'a'. You want a period? Then press the period. I mean.. come on! Really??? This is arguably the best keyboard I've ever used on any phone!
Blackerthanblack, Gatmyer, tfitzpat03 and 1 others like this.
I would agree it could take up to 17 days for the muscle memory to develop to the point you can really fly on it.
But yes it's a bloody keyboard lol. Not exactly rocket science.
Blackerthanblack and kbz1960 like this.
I think there is a learning curve. To type with any type of decent speed you have to get used to reaching for the keys. They are spread out in such a way that it makes it difficult to reach them if you have been accustomed to using a smaller keyboard or a touchscreen keyboard.
In Kevin's initial review of the Passport he stated that there is a learning curve with the Passport keyboard and I think he's used a few Blackberry's in his time.
I admit I had to get used to the punctuation, but it's become second nature now. I believe people are way too choosy and most of the negative reviews come from the "other side" (iOS, Android users) who have become accustomed to burying BlackBerry since the legendary downfall. Plus, if you have been active on the forums, it's so easy to spot that the complaints from cb members came after using the device for a few hour/days, without bothering to read as much as possible on how to use it. I think that the three row design is much better than the old one and combined with the touch capability it's astounding.
Yes for some of use it feels natural at first hand. I was typing away when I first played with the demo at a store. It was a no brainer and the deciding point to buy the Passport for me.
I'm back to blackberry because I needed a good keyboard . But cmon guys this should not be be an issue to talk about. Some take longer then other to learn to type. Not everyone is a fast learner.
Just came from an iPhone 6 + and yes there you need some time to get used to the keyboard that the passport has.
It took me roughly a week to "I get it" and I'm still learning new tricks etc.
What I really love is that the keyboard is touch for scrolling. That is clutch when your editing a document or message and scrolling a webpage or excel sheet etc.
Either you love it or hate it but don't drop it that fast. Give it some more time.
My guess is that, for those who have never used a physical keyboard (or at least haven't used one in awhile), there is a learning curve involved because the keys actually have to be pressed, rather than just touched. Seems like an insignificant detail, but it really isn't.
I came from a Q5 and my only issue with the keyboard is the placment of zxcvbnm. They are all to far to each side of the keyboard, it's not like any other keyboard I've used. So I have to think about what I'm doing.
I know what you mean op. The first time I try the Passport in store the keyboard felt natural that I didn't have to look down on the keys. I don't understand why a lot of old time BlackBerry users would say it's a learning curve.
I never had a physical keyboard phone as a personal phone (had a 9900 for work). I understand that people who are used to the 9900 or other traditional BB's might find it a bit different, but it's really quick to learn. I actually prefer the larger keys on the passport, and the touch layer is just magical.
The only problem was the b and v keys especially B but in time you'll get used to it!
I asked her to write on my Q10 she was like WTF!
Well my blackberry device history is the first torch, the bb 9900, the z10, and now the passport. My favorite keyboard that I used is on the 9900, but I must say each day that I use the passport it is becoming closer and closer to being my favorite.
People complain about the 3 row keyboard. I can understand it if a person were to come from a torch or a 9900 or even a classic because that is what they are used to. They would have to train themselves to use this 3 row style keyboard. Other than that I don't see what's not to like about this keyboard.
I came from a z10 before the passport. They only thing I didn't like about the keyboard was that it was so tight at first which is understandable since I bought it brand new. Now that it is broke in I can say that it is a joy to type on. Blackberry is genius with this keyboard in my opinion.
The thing I like about it the most is the width. I used to have problems of my thumbs running into each other on the torch and 9900. Not a problem on my passport. I like the idea of putting the symbols and numbers on the touchscreen. I am almost as fast as I was on the 9900 but I am more accurate on the passport than any other device.
I am a student and I have typed papers on my passport. You can't type papers on a phone without being able to enjoy the keyboard so I am fine with it. I do kind of wish that it had full trackpad support. But for what it does I still appreciate it. Good job blackberry. If they come out with a passport 2 I will definitely get it.
It's natural for you. But it could be quite a challenge for many others. My son learned the push bike in about 30 minutes, some other kids had to go through different training bikes before they could ride without a third or fourth wheel. Not every one is born a genius.
As the OP mentioned review of 'non blackberry users', their message re. learning curve could be interpreted that they are convincing others, including non blackberry users, to give themselves some time to get used to it. And I see it as a positive thing and worth a thread to applaud and encourage them, rather than this.
I'm amazed by how much can be done from the keyboard. Since I've returned to BlackBerry, the keyboard's been the best part. No problems here, no learning curve. It's almost intuitive.
When I phone a person I hear him but they don't hear me, what could the problem be?
Z10. I love it now..!


text:
\section{Introduction}
A neutron star (NS) \cite{Baym:2005de, Prakash:2014tva} with a typical radius of 10-12 km and generally having a mass range of 1-2 solar mass ($\rm{{M}}_{\odot}$) is formed as an aftermath of a massive supernova explosion. A neutron star can be cooled principally by the emission of photons and neutrinos. It is also conjectured that the emission of axion from a neutron star may contribute to its cooling process in addition to photon and neutrino emissions. Axions \cite{Wilczek:1977pj, Weinberg:1977ma} are pseudo Nambu-Goldstone bosons which are introduced to circumvent the strong CP problem \cite{Peccei:2006as} that refers to the presence of CP violation term in QCD Lagrangian \cite{tHooft:1976rip} arising from the non-Abelian nature of QCD gauge symmetry. The Peccei-Quinn (PQ) solution \cite{Peccei:2006as} of strong CP problem results in the prediction of new particle namely axion. The axion which is a Goldstone boson that arises out of the PQ solution where an anomalous chiral symmetry U(1)$_{\rm A}$ \cite{Peccei:1977hh} is introduced and is spontaneously broken at the PQ energy scale, is an interesting candidate in addressing several aspects of cosmology and particle physics such as dark matter in the Universe. Since the axion have tiny couplings with photons, nucleons and electrons, they can be produced inside a neutron star through the nucleon-nucleon axion bremsstrahlung process $ N + N \rightarrow N + N + a $, where $N$ is a nucleon (proton or neutron) and $``a"$ denotes axion. As mentioned earlier, while the energy loss is considered to be mostly due to photon and neutrino emission, the emission of axion from the late stages of the star such as the supernova or neutron star can also contribute in considerable measure to the process of their cooling. Here we have considered that neutron star is the source of the axions. But axions can be emitted from the other astrophysical sources like the sun, white dwarf, supernova, red giant, globular clusters etc. by the mechanisms such as Primakoff, electron bremsstrahlung, Compton processes etc. Axion mass is also constrained by the experimental \cite{Ringwald:2016}, astrophysical and cosmological limits. These limits indicate that axion have very low mass $m_{a}\lesssim 10 \hspace{1mm}\rm {meV}$ \cite{Hagmann:2010}. Cosmological data constrain the axion mass as $m_{a}< 0.4-1.0 \hspace{1mm}\rm {eV}$ at the $95\%$ statistical CL \cite{Melchiorri:2007}. Solar axions are produced mainly by the Primakoff process. The CAST experiment put an upper limit on the solar axion mass to be $m_{a}\lesssim 0.02 \hspace{1mm}\rm {eV}$ \cite{Zioutas:2005}. In case of globular-clusters, the limits on axion decay constant is given as $f_{a}> 2.3\times 10^{7} \hspace{1mm}\rm {GeV}$ ($m_{a}< 0.3\hspace{1mm}\rm {eV}$) when KSVZ model \cite{Cadamuro:2012rm, Leskinen:2016tfu} is considered while for DFSZ model \cite{Cadamuro:2012rm}-\cite{Berezhiani:1992rk} $f_{a}> 0.8\times 10^{7} \hspace{1mm}\rm {GeV}$ ($m_{a}< 0.7\hspace{1mm}\rm {eV}$) \cite{Hagmann:2010}. But for the case of white dwarf, the constraints on $f_{a}$ is given by $f_{a}> 1.3\times 10^{9}\hspace{1mm} \rm {GeV}\hspace{1mm} {\cos^2{\beta}} $ ($m_{a}< 4.5\hspace{1mm} \rm {meV}\hspace{1mm}/ {\cos^2{\beta}} $) \cite{Hagmann:2010} where $\tan {\beta}$ is the ratio of two Higgs vacuum expectation values. These parameters are useful for explaining the white dwarf cooling by the axion emission \cite{Raffelt:2006cw}. The constraint on axion mass limit for the red giant case is given as (\cite{Raffelt:1995}) $f_{a}\gtrsim 6.6\times 10^{8} \hspace{1mm}\rm {GeV}\hspace{1mm} {\cos^2{\beta}} $ ($m_{a}< 0.009\hspace{1mm} \rm {eV}/\hspace{1mm} {\cos^2{\beta}} $) in the DFSZ model. Raffelt \cite{Raffelt:2006cw} also derived similar constraints from the measured duration of the neutrino signal of the Supernova SN 1987A $f_{a}\gtrsim 4\times 10^{8} \hspace{1mm}\rm {GeV}$ ($m_{a}\lesssim 16\hspace{1mm}\rm {meV}$). Supernova energy loss arguments \cite{Raffelt:2006cw} can be explained by the aforementioned axion parameters. The astrophysical and cosmological axion mass limits are however summarised in Fig. 3 of Ref. \cite{Raffelt:2006cw}.

We consider the bremsstrahlung production of axion in the interior of the neutron star. The energy loss at the later stage of a star can be addressed for two conditions, namely degenerate and non-degenerate limits. While the degenerate condition is applied to only neutron stars, the non-degenerate one is for the accretion disc. In earlier works related to such energy loss through axion, Sedrakian \cite{Sedrakian:2015krq} and Umeda $\it{et}$ $\it{al}$ \cite{Umeda:1997da} considered only the degenerate scenario but in this work we consider both degenerate and non-degenerate cases. We performed a detailed study in this regard and obtain the energy loss of neutron star as a function of time as also the variation of temperature as a function of time for the case when axion emission contributes to the cooling in addition to neutrinos and photons. We then compare our results when axion is not included. We find that for the mass of emitted axions $\sim 10^{-5}\rm{eV}$ and higher, the contribution to the neutron star cooling rate differs considerably from that when no axion emission occurs.

The paper is organised as follows. In Section 2, we briefly describe
the formalism that includes the cooling process of neutron star and
axion production and emission from such a neutron star. The expressions for energy loss rate for both the degenerate and non-degenerate limits are also given in this section. Section 3 elaborates the calculations and results while we furnish some summary and discussions in Section 4.
\section{Formalism}
In this section we furnish a brief account of axion production and emission from the neutron star. We also furnish the cooling of the star when the effect of axion emission is included.

\subsection{Axion Emission via Nucleon Nucleon Axion Bremsstrahlung process}
Axions can be emitted from an NS via the nucleon-nucleon axion bremsstrahlung process $ N + N \rightarrow N + N + a $, where $N$ refers to a proton $p$ or a neutron $n$ and $``a"$ denotes axion. In this process nucleons are interacting via one-pion exchange (OPE) potential.
\subsubsection{Matrix Elements for the process $ N + N \rightarrow N + N + a $}
The interaction Hamiltonian for the interaction of axions with the nucleons can be written as \cite{Raffelt:1996wa}
\begin{equation} \label{eq:1}
\mathcal{H}_{int}=-\dfrac{C_{N}}{2f_{a}}\overline{\psi}_{N}\gamma_{\mu}\gamma_{5}\psi_{N}\partial^{\mu}a
\end{equation}
where $f_{a}$ is the PQ energy scale for axions, $C_{N}$ is a dimensionless model dependent coupling constant of order unity, the $\psi_{N}$ represents the nucleon Dirac fields and $``a"$ is the axion field.
The possible Feynman diagrams related to this process is given in Ref. \cite{Brinkmann:1988vi}. There are two kinds of diagrams. One (four of them) refers to the processes where the axion is attached to each nucleon line while the other four diagrams are for the exchange processes ($ N_{3} \leftrightarrow N_{4}$) where the axion is attached to each nucleon line and $N_{1}, N_{2}, N_{3}$ and $N_{4}$ denote the four nucleons which take part in bremsstrahlung process. For the processes, $nn \rightarrow nn + a$ and $ pp \rightarrow pp + a$ (``pure processes") the spin-summed squared matrix element is of the form \cite{Brinkmann:1988vi, Raffelt:1993ix}
\begin{equation} \label{eq:2}
\sum_{spins}{{\mid \mathcal{M} \mid}^2_{NN}}=\dfrac{16({4\pi})^{3}\alpha_{\pi}^{2}\alpha_{a}}{3{m_{N}}^{2}}\bigg[\bigg(\dfrac{\textbf{K}^{2}}{\textbf{K}^{2}+m_{\pi}^{2}}\bigg)^{2}+\bigg(\dfrac{\textbf{l}^{2}}{\textbf{l}^{2}+m_{\pi}^{2}}\bigg)^{2}+\dfrac{\textbf{K}^{2}\textbf{l}^{2}-3\bigg(\textbf{K}.\textbf{l}\bigg)^{2}}{(\textbf{K}^{2}+m_{\pi}^{2})(\textbf{l}^{2}+m_{\pi}^{2})}\bigg]
\end{equation}
where $m_{\pi}$ is the pion mass and $m_{N}$ is the nucleon mass. The axion-nucleon ``fine-structure constant" $\alpha_{a}\equiv(C_{N}m_{N}/f_{a})^{2}/4\pi=g_{aN}^{2}/4\pi$, where $g_{aN}=(C_{N}m_{N}/f_{a})$ is the axion-nucleon coupling constant. The quantity pion-nucleon ``fine structure constant" is given by $\alpha_{\pi}\equiv(f2m_{N}/m_{\pi})^{2}/4\pi\approx17$ where the pion-nucleon coupling $f\approx1.05$ and $\textbf{K}=\textbf{p}_{2}-\textbf{p}_{4}$ and  $\textbf{l}=\textbf{p}_{2}-\textbf{p}_{3}$
with $p_{i}$ ($i=1-4$) are the momenta of the nucleons $N_{i}$.
For the ``mixed" process $np \rightarrow np+a$, spin-summed squared matrix element can be written as \cite{Raffelt:1993ix}
\begin{equation} \label{eq:3}
\begin{aligned}
\sum_{spins}{{\mid \mathcal{M} \mid}^2_{np}}=\dfrac{256{\pi}^{2}\alpha_{\pi}^{2}}{3{m_{N}}^{2}}\dfrac{(g_{an}+g_{ap})^{2}}{4}\bigg[2\bigg(\dfrac{\textbf{l}^{2}}{\textbf{l}^{2}+m_{\pi}^{2}}\bigg)^{2}-\dfrac{4\bigg(\textbf{K}.\textbf{l}\bigg)^{2}}{(\textbf{K}^{2}+m_{\pi}^{2})(\textbf{l}^{2}+m_{\pi}^{2})}\bigg]\\
+\dfrac{256{\pi}^{2}\alpha_{\pi}^{2}}{3{m_{N}}^{2}}\dfrac{(g_{an}^{2}+g_{ap}^{2})}{2}\bigg[\bigg(\dfrac{\textbf{K}^{2}}{\textbf{K}^{2}+m_{\pi}^{2}}\bigg)^{2}+2\bigg(\dfrac{\textbf{l}^{2}}{\textbf{l}^{2}+m_{\pi}^{2}}\bigg)^{2}\\
+2\dfrac{\textbf{K}^{2}\textbf{l}^{2}-\bigg(\textbf{K}.\textbf{l}\bigg)^{2}}{(\textbf{K}^{2}+m_{\pi}^{2})(\textbf{l}^{2}+m_{\pi}^{2})}\bigg].
\end{aligned}
\end{equation}
\subsubsection{Energy Loss Rate Expression}
The axion energy-loss rate per unit volume is given by \cite{Raffelt:1996wa}
\begin{equation} \label{eq:4}
\begin{aligned}
Q_{a}=\int{\dfrac{d^{3}\textbf{K}_{a}}{2\omega_{a}(2\pi)^{3}}}\omega_{a}\int{\prod_{i=1}^{4}\dfrac{d^{3}\textbf{P}_{i}}{2E_{i}(2\pi)^{3}}}f_{1}f_{2}(1-f_{3})(1-f_{4})\\
\times(2\pi)^{4}\delta^{4}(P_{1}+P_{2}-P_{3}-P_{4}-K_{a})S\sum_{spins}{{\mid \mathcal{M} \mid}^2_{NN}}
\end{aligned}
\end{equation}
where $P_{1}$ and $P_{2}$ are the four-momenta of the initial-state nucleons, $P_{3}$ and $P_{4}$ are the four-momenta of the final states nucleons and $K_{a}$ is the four-momentum of the axion. A factor $S$ is introduced to accounts for the identical particles in the initial and final states and it takes the value $S = 1/4$ for pure processes and $S = 1$ for mixed processes. In Eq. \ref{eq:4} $f_{i}$'s are the occupation numbers for the nucleons $N_{i}$'s. In this case, it is assumed that the axions escape freely so that a Bose stimulation factor $(1+f_{a})$ as well as axion absorption factors are neglected.

In the following, we furnish the simplified expressions for energy loss rate $Q_{a}$ for both degenerate and non-degenerate limits.
\subsubsection{Non-degenerate Limit}
For simplicity, we first neglect the pion mass contribution in Eqs. \ref{eq:2} and \ref{eq:3}. With this approximation, the squared matrix element reduces to \cite{Greenberg:2000he}
\begin{equation} \label{eq:6}
\sum_{spins}{{\mid \mathcal{M} \mid}^2_{NN}}=\dfrac{256{\pi}^{2}\alpha_{\pi}^{2}}{3{m_{N}}^{2}}\tilde{g}_{NN}^{2}
\end{equation}
with $\tilde{g}_{NN}^{2} \equiv g_{an}^{2}(3-\beta)$ for $nn\rightarrow nn+a$ process, $\tilde{g}_{NN}^{2} \equiv g_{ap}^{2}(3-\beta)$ for $pp\rightarrow pp+a$ process, and \\$\tilde{g}_{NN}^{2} \equiv \left(\dfrac{g_{an}+g_{ap}}{2}\right)^{2}(2-4\beta/3)+\dfrac{g_{an}^{2}+g_{ap}^{2}}{2}(5-2\beta/3)$ for $np\rightarrow np+a$ process. The effective coupling $\tilde{g}_{NN}$ is given by $\tilde{C}_{N}m_{N}/f_{a}$ and $\beta \equiv 3\langle(\hat{\textbf{K}}.\hat{\textbf{l}})^{2}\rangle.$ In the non-degenerate limit the numerical value of $\beta$ is 1.3078 \cite{Raffelt:1993ix}. The axion-nucleon coupling $\mid\tilde{C}_{N}\mid$ can be found numerically as $\mid\tilde{C}_{N}\mid =0.013$ for $nn\rightarrow nn+a$ process,
$\mid\tilde{C}_{N}\mid =0.442$ for $pp\rightarrow pp+a$ process and
$\mid\tilde{C}_{N}\mid =0.495$ for $np\rightarrow np+a$ process \cite{Greenberg:2000he}.  Introducing a ``fudge factor" $\xi(T)$ to account for the pion mass effects and using Eq. \ref{eq:6} in Eq. \ref{eq:4} yields the total energy loss rate per unit volume as \cite{Greenberg:2000he}
\begin{equation} \label{eq:7}
\begin{aligned}
Q_{a}^{ND}=\dfrac{\xi(T)}{280}\dfrac{n_{B}^{2}T^{7/2}}{m_{N}^{5/2}\pi^{7/2}}\Big(Y_{n}^{2}\sum_{spins}{\mid \mathcal{M} \mid}^2_{nn}+Y_{p}^{2}\sum_{spins}{\mid \mathcal{M} \mid}^2_{pp}+Y_{n}Y_{p}\sum_{spins}{\mid \mathcal{M} \mid}^2_{np}\Big)\\
=\dfrac{32}{105}\xi(T)\dfrac{\alpha_{\pi}^{2}n_{B}^{2}T^{7/2}}{m_{N}^{9/2}\pi^{3/2}}\Big(Y_{n}^{2}\tilde{g}_{nn}^{2}+Y_{p}^{2}\tilde{g}_{pp}^{2}+4Y_{n}Y_{p}\tilde{g}_{np}^{2}\Big)\hspace{3.8cm}\\
=\dfrac{32}{105}\xi(T)\dfrac{\alpha_{\pi}^{2}n_{B}^{2}T^{7/2}}{m_{N}^{9/2}\pi^{3/2}}g_{ND}^{2}\hspace{8.3cm}
\end{aligned}
\end{equation}
where $g_{ND}$ is the total effective axion-nucleon coupling constant for the non-degenerate limit, $Y_{p}$ is the proton number fraction and $Y_{n}$ is the neutron number fraction. With $Y_{p} \approx 0.1$, $Y_{n} \approx 0.9$, $\xi(T)\approx 0.5$, and using the above $\mid\tilde{C}_{N}\mid $ values, $\tilde{g}_{NN}^{2}$ expressions and the relation $m_{a}=6\rm{\mu eV} \left(\frac{10^{12}\rm{GeV}}{f_{a}}\right)$ \cite{Berenji:2016jji}, the values of $g_{ND}$ and $C_{N}^{ND}$ can be found numerically as
\begin{equation} \label{eq:8}
g_{ND}=4.71\times 10^{-8}\hspace{1mm}\Big(\dfrac{m_{a}}{eV}\Big)\hspace{1cm} \rm{and} \hspace{1cm}C_{N}^{ND}=0.30.
\end{equation}
With the above expression for $g_{ND}$ the axion energy loss rate per unit volume (Eq. \ref{eq:7}) reduces to
\begin{equation} \label{eq:9}
Q_{a}^{ND}=2.90166\times 10^{31} \hspace{1mm}erg\hspace{1mm}cm^{-3}\hspace{1mm}yr^{-1}\hspace{1mm}T^{3.5}_{9}\hspace{1mm}\rho_{12}^{2}\hspace{1mm}m^{2}_{eV}
\end{equation}
where $m_{eV} \equiv m_{a}/eV $, $T_{9}\equiv T/10^{9} K$, and $\rho_{12} \equiv \dfrac{\rho}{10^{12} \rm{g/{cm}^{3}}}=n_{B}m_{N}$ where $n_{B}$ is the nucleon (baryon) density.
\subsubsection{Degenerate Limit}
In the degenerate limit, Eq. (\ref{eq:6}) simplies to \cite{Greenberg:2000he}
\begin{equation} \label{eq:11}
\sum_{spins}{{\mid \mathcal{M} \mid}^2_{NN}}=\dfrac{256{\pi}^{2}\alpha_{\pi}^{2}}{{m_{N}}^{2}}\tilde{g}_{NN}^{2}.
\end{equation}
Unlike the non-degenerate case, here the parameter $\beta$ is zero.
With $\tilde{g}_{NN}^{2}\equiv g_{an}^{2}$ for $nn\rightarrow nn+a$ process,
$\tilde{g}_{NN}^{2} \equiv g_{ap}^{2}$ for $pp\rightarrow pp+a$ process and
$\tilde{g}_{NN}^{2}\equiv \left({g_{an}^{2}+g_{ap}^{2}}+(g_{an}g_{ap})/3\right)$ for $np\rightarrow np+a$ process.
The numerical values of effective coupling are
$\mid\tilde{C}_{N}\mid=0.01$ for $nn\rightarrow nn+a$ process,
$\mid\tilde{C}_{N}\mid =0.34$ for $pp\rightarrow pp+a$ process and
$\mid\tilde{C}_{N}\mid=0.338$ for $np\rightarrow np+a$ process \cite{Greenberg:2000he}.
In this case the integration in Eq. \ref{eq:4} can be simplified analytically without neglecting the pion masses. Here the pionic contribution $F(u)$ is given by \cite{Raffelt:1996wa}
\begin{equation} \label{eq:12}
\begin{aligned}
F(u)=1-\frac{5u}{6}\hspace{1mm}\arctan(\frac{2}{u})+\frac{u^{2}}{3(u^{2}+4)}+\frac{u^{2}}{6\sqrt{2u^{2}+4}}\\
\times\arctan \Big(\frac{2\sqrt{2u^{2}+4}}{u^{2}}\Big)
\end{aligned}
\end{equation}
where $u=m_{\pi}/p_{F,N}$. {With $u\approx0.32Y_{N}^{-1/3}$ and consider $\rho_{B}\approx 2\rho_{nuc}$, {$F(u)$ can be replaced by $F(Y_{N})$ and the total emission rate is given as \cite{Raffelt:1996wa, Greenberg:2000he}
\begin{equation} \label{eq:13}
\begin{aligned}
Q_{a}^{D}=\dfrac{31}{967680}\Big(\dfrac{3n_{B}}{\pi}\Big)^{1/3}T^{6}\Big(Y_{n}^{1/3}F(Y_{n})\sum_{spins}{\mid \mathcal{M} \mid}^2_{nn}+Y_{p}^{1/3}F(Y_{p})\sum_{spins}{\mid \mathcal{M} \mid}^2_{pp}\\+4Y_{np}^{1/3}F(Y_{np})\sum_{spins}{\mid \mathcal{M} \mid}^2_{np}\Big)\\
=\dfrac{31\pi^{5/3}(3n_{B})^{1/3}\alpha_{\pi}^{2}T^{6}}{3780m_{N}^{2}}\Big(Y_{n}^{1/3}F(Y_{n})\tilde{g}_{an}^{2}+Y_{p}^{1/3}F(Y_{p})\tilde{g}_{ap}^{2}+Y_{np}^{1/3}F(Y_{np})\tilde{g}_{np}^{2}\Big)\hspace{-0.13cm}\\
=\dfrac{31\pi^{5/3}(3n_{B})^{1/3}\alpha_{\pi}^{2}T^{6}}{3780m_{N}^{2}}g_{D}^{2}\hspace{8.2cm},
\end{aligned}
\end{equation}
where $g_{D}$ is the total effective axion-nucleon coupling constant for the degenerate limit. The effective nucleon fraction $Y_{np}$ for the mixed processes are given by \cite{Brinkmann:1988vi}
\begin{equation} \label{eq:14}
Y_{np}^{1/3}=\dfrac{1}{2\sqrt{2}}(Y_{n}^{2/3}+Y_{p}^{2/3})^{1/2}\Big[2-\dfrac{\mid Y_{n}^{2/3}-Y_{p}^{2/3} \mid}{Y_{n}^{2/3}+Y_{p}^{2/3}}\Big].
\end{equation}
For the degenerate case, using the values of nucleon number fractions $Y_{p}=0.01$, $Y_{n}=0.99$ and $Y_{np}=0.06$, we can calculate $F(Y_{n})\approx 0.64, F(Y_{p})\approx 0.12 \hspace{2mm}$ and $F(Y_{np})\approx 0.31$ for the pure and mixed processes. Also using the above values one can attain the effective coupling constants $g_{D}$ and $C_{N}^{D}$ for the degenerate case as
\begin{equation} \label{eq:15}
g_{D}=2.04\times 10^{-8}\hspace{1mm}\Big(\dfrac{m_{a}}{eV}\Big)\hspace{1cm} \rm{and} \hspace{1cm}C_{N}^{D}=0.13.
\end{equation}
Using Eqs. \ref{eq:13} and \ref{eq:15} the axion emission rate per unit volume is obtained as
\begin{equation} \label{eq:16}
Q_{a}^{D}=4.84244\times 10^{30} \hspace{1mm}erg\hspace{1mm}cm^{-3}\hspace{1mm}yr^{-1}\hspace{1mm}T^{6}_{9}\hspace{1mm}m^{2}_{eV}\hspace{1mm}\Big(\dfrac{\rho_{NS}}{\rho_{nuc}}\Big)^{1/3}
\end{equation}
where $m_{eV} \equiv m_{a}/eV $, $T_{9}\equiv T/10^{9} K$, $\rho_{NS}$ is the density of the neutron star and $\rho_{nuc}$ is the nuclear density.
\subsection{Neutron star cooling}
In the last few years it has been observed that the surface temperature of the neutron star decreases with time. This is the only direct indication of cooling of a neutron star \cite{Pizzochero:2016ffp}.

In Newtonian formulation the energy balance equation for the neutron star is given by \cite{Sedrakian:2015krq}
\begin{equation} \label{eq:18}
\frac{dE_{\rm th}}{dt}=C_{v}\frac{dT}{dt}=
-L_{\nu}(T)-L_{a}(T)-L_{\gamma}(T_{e})+H(T),
\end{equation}
where $E_{\rm th}$ is the thermal energy content of the star,
$T$ is its internal temperature and $T_{e}$ is the effective
temperature. The quantities $L_{\nu}$ and $L_{a}$ are the neutrino and axion
luminosities respectively from the bulk of the star
and $L_{\gamma}$ is the luminosity of photons radiated from the
star surface. In Eq. \ref{eq:18} $C_{v}$ is the specific heat of the
core, and the source term $H$ contains all possible
``heating mechanisms" which, for example, convert magnetic or
rotational energy into heat energy. This could be significant in the
late time evolution of neutron stars. It is assumed here that
$H(T)=0$. The photon luminosity $L_{\gamma}$ is given by the Stefan-Boltzmann law \cite{Nscool:2010dpl}
\begin{equation} \label{eq:19}
L_{\gamma}=S\hspace{1mm}T^{2+4\alpha}=4\pi\hspace{1mm}\sigma\hspace{1mm}R^{2}\hspace{1mm}T_{e}^{4}
\hspace{2mm}.
\end{equation}
The above relation is obtained using $\hspace{2mm} T_{e}\propto T^{0.5+\alpha} \hspace{1mm}(\alpha\ll 1)$,
where $\sigma$ is the Stefan-Boltzmann constant, and $R$ is the radius of the star. In the present work we use the NSCool code \cite{Nscool:2010dp} for calculating the axion luminosity. Various neutrino processes are also
involved in the cooling of neutron stars \cite{Page:2005fq}. Dominant neutrino emitting processes are direct Urca processes and modified
Urca processes. The direct Urca processes are $n\rightarrow p+e^{-
}+\overline{\nu}_{e}$ (beta decay) and $p+e^{-}\rightarrow n+\nu_{e}$ (electron capture), which are only possible in neutron stars if the proton fraction exceeds a critical threshold. The above two neutrino emitting
processes are fast and the dependence of luminosity on temperature is given by the relation $L_{\nu}^{fast}\propto
T^{6}_{9}$. In case the proton fraction is below the threshold, the dominant neutrino emission process, a variant of the direct Urca process, namely the  modified Urca process, is a second-order process. The modified processes
are
\begin{eqnarray} \label{eq:20}
n+n\rightarrow n+p+e^{-}+\overline{\nu}_{e}, &&
n+p+e^{-}\rightarrow n+n+\nu_{e}\,\, \nonumber \\ \
{\rm neutron}\,\, {\rm branch} \nonumber \\
p+n\rightarrow p+p+e^{-}+\overline{\nu}_{e}, &&
p+p+e^{-}\rightarrow p+n+\nu_{e}\,\, \ \nonumber \\
{\rm proton}\,\, {\rm branch.}
\end{eqnarray}
These neutrino emitting processes are slow and the dependence of luminosity on temperature is given by the relation
$L_{\nu}^{slow}\propto T^{8}_{9}$.
The other neutrino emitting processes are electron-positron pair annihilation, plasmon decay, electron synchrotron, photoneutrino emission, electron-nucleus bremsstrahlung, cooper pairing of neutrons, neutron-neutron bremsstrahlung, neutron-nucleus bremsstrahlung \cite{Nscool:2010dpl}.

\section{Calculations and Results}
As mentioned earlier, we use NSCool numerical code \cite{Nscool:2010dp} and include axion  energy loss rate for both degenerate and non-degenerate cases. We adopt Akmal Pandharipande Ravenhall (APR) equation of state (EoS) for our work. This equation of state deals with nuclear degrees of freedom only by which the fast cooling processes are avoided. Moreover, APR does not include non-nucleonic degrees of freedom. In this EoS the two-nucleon interaction, namely Argonne $v_{18}$ \cite{Akmal:1998cf} has been incorporated and the boost corrections to the two-nucleon interaction are also considered. This ensures the relativistic effect in the EoS. In addition, three-nucleon interactions are also considered in the nuclear Hamiltonian. This enables an increase in mass limit of the neutron star to $\sim$ 2.2 ${M}_{\odot}$. For demonstrating the effect of axion emission in the cooling process of neutron star, we consider neutron stars of three different masses namely 1.0${M}_{\odot}$ (light), 1.4${M}_{\odot}$ (intermediate) and 1.8${M}_{\odot}$ (massive) and obtain the variation of their luminosities with surface temperature and time for the cases including axion emission in the cooling process and without axion emission. We also consider three axion masses ($m_{a}$) namely $m_{a}=10^{-5}\rm{eV}$, $10^{-3}\rm{eV}$ and $10^{-2}\rm{eV}$, in the calculation. The energy loss rate due to axion emission increases with the increase of axion mass because of $m_{a}^{2}$ factor in the energy loss rate formula (Eqs. \ref{eq:9}, \ref{eq:16}) which implies fast cooling of neutron star and fast cooling occurs for the increase of neutron star masses. In Figs. \ref{fig:3}$-$\ref{fig:5} we show how the neutron star luminosities vary with time due to neutron star cooling when axion cooling is included along with the cooling due to neutrino and gamma emission and compared with the case when axion emission is not considered for neutron star masses 1.0${M}_{\odot}$, 1.4${M}_{\odot}$ and 1.8${M}_{\odot}$ respectively. The left panel of Figs. \ref{fig:3}$-$\ref{fig:5} are for degenerate case while the right panels are for non-degenerate case. In Figs. \ref{fig:3}$-$\ref{fig:8} we include observational results for three pulsars, namely PSR B0656+14, Geminga and PSR B1055-52. The results are shown by points in all the figures.

It can be observed from Figs. \ref{fig:3}$-$\ref{fig:5} that heavier the axion masses further away are the luminosity-time plots from the observational data. For the degenerate category, the variation of luminosities with time almost coincide with the results when no axion mass is considered. This is true for all the three chosen masses of neutron stars. It can also be observed from the left panel of Fig. \ref{fig:5} that for the 1.8${M}_{\odot}$ neutron star, the observational data for the luminosities for the pulsars PSR B0656+14 and Geminga fairly agree with the case when axion mass is $10^{-5}\rm{eV}$. In addition, the luminosity with axion mass $10^{-3}\rm{eV}$ is within the error bar of the Geminga pulsar observational data. For the non-degenerate case however, the cooling due to axion emission appears to cause the depletion of both luminosities and temperatures more rapidly in comparison to degenerate cases, at the region of more advanced stages (higher time) of the neutron star. This trend becomes more prominent for lower neutron star mass. For example, neutron star mass of 1.8${M}_{\odot}$ the cooling curve (Fig. \ref{fig:5}, right panel) with axion emission for axion mass $10^{-5}\rm{eV}$ barely differs from that without axion emission after $t\sim 10^{5}$ years but this difference increases when neutron star mass is 1.4${M}_{\odot}$ or 1.0${M}_{\odot}$ (Fig. \ref{fig:3}, right panel and Fig. \ref{fig:4}, right panel). For the other two chosen axion masses ($10^{-3}\rm{eV}$,  $10^{-2}\rm{eV}$), the cooling curve however, shows much rapid decrease of luminosity. Similar trends are also observed for the temperature vs. time plots for non-degenerate cases but the temperature in this case falls off more rapidly for all the chosen axion masses (Figs. \ref{fig:6}$-$  \ref{fig:8}).

Calculations are also done to obtain the variations of neutron star temperature with time for the same set of three neutron star masses and axion masses as in the previous case (Figs. \ref{fig:3}$-$\ref{fig:5}). These are ploted in Figs. \ref{fig:6}$-$\ref{fig:8}. Here too the left panel of Figs. \ref{fig:6}$-$\ref{fig:8} are for the degenerate limit while the right panels of these Figures show the results for non-degenerate limit. Once again, one notices that for the degenerate case the results for axion mass $m_{a}=10^{-5}\rm{eV}$ almost coincide with that for the case when no axion cooling is considered. It is also to be noted that the neutron star temperature calculations are agree with the observational data for pulsars PSR B0656+14 and Geminga at least upto their error bars for all the three neutron star masses considered here. Similar trends are also obtained for non-degenerate case. These results and their comparison with the observational data of three pulsars can be indicative of the fact that the mass of the axion would be below $10^{-3}\rm{eV}$.

We also make a direct comparison between the degenerate case and the non-degenerate case in Figs. \ref{fig:9}$-$\ref{fig:12}. In Fig. \ref{fig:9}, the results for degenerate and non-degenerate limits are shown by calculating and ploting the variation of luminosities with time for both the limits when the axion mass is $10^{-5}\rm{eV}$. The results are shown for all the three neutron star masses, namely 1.0${M}_{\odot}$, 1.4${M}_{\odot}$ and 1.8${M}_{\odot}$ considered in this work. In Fig. \ref{fig:10} we show similar results but for axion mass $m_{a}=10^{-3}\rm{eV}$. In both Figs. \ref{fig:9} and \ref{fig:10} it can be seen that while at early times results for both the degenerate and non-degenerate limits appear to almost overlap, at later times this difference decreases with the increase in neutron star mass. Therefore for very low axion mass ($\sim10^{-5}\rm{eV}$) the degenerate and non-degenerate cases appears to be increasingly indistinguishable as the neutron star becomes more and more massive. In contrast, we observe from Fig. \ref{fig:10} that with the increase in axion mass (in this case $\sim10^{-3}\rm{eV}$) the difference in results for degenerate and non-degenerate cases, although decreases with increase of neutron star mass, does not tend to vanish at high neutron star mass. Similar plots as in Figs. \ref{fig:9} and \ref{fig:10} but for the variation of temperature and time are shown in Figs. \ref{fig:11} and \ref{fig:12}. While Fig. \ref{fig:11} is for axion mass $10^{-5}\rm{eV}$, in Fig. \ref{fig:12} we plot the result temperature vs. time when the axion mass is $10^{-3}\rm{eV}$. The results are shown all the three neutron star masses considered.
Similar trends regarding the variations of differences between the degenerate and non-degenerate cases are also noticed when temperature is varied with time.

\begin{figure}
\includegraphics[width=8.5cm,height=8.5cm]{dlvst10.png}
\includegraphics[width=8.5cm,height=8.5cm]{ndlvst10.png}
\caption{Luminosity ($L$) vs. time ($t$) graph for both degenerate (left panel) and non-degenerate (right panel) limits with $ \rm{M}=1.0\rm{M}_{\odot}$ and $m_{a}=0\rm{eV}, 10^{-5}\rm{eV}, 10^{-3}\rm{eV}, 10^{-2}\rm{eV}$ (from top to bottom). The observational data for three pulsars PSR B0656+14, Geminga and PSR B1055-52 are shown by dots with error bars from left to right.}
\label{fig:3}
\end{figure}
\begin{figure}
\includegraphics[width=8.5cm,height=8.5cm]{dlvst14.png}
\includegraphics[width=8.5cm,height=8.5cm]{ndlvst14.png}
\caption{Same as in Fig. \ref{fig:3} but for $ \rm{M}=1.4\rm{M}_{\odot}$}
\label{fig:4}
\end{figure}
\begin{figure}
\includegraphics[width=8.5cm,height=8.5cm]{dlvst18.png}
\includegraphics[width=8.5cm,height=8.5cm]{ndlvst18.png}
\caption{Same as in Fig. \ref{fig:3} but for $ \rm{M}=1.8\rm{M}_{\odot}$}
\label{fig:5}
\end{figure}
\begin{figure}
\includegraphics[width=8.5cm,height=8.5cm]{dtvst10.png}
\includegraphics[width=8.5cm,height=8.5cm]{ndtvst10.png}
\caption{Surface temperature ($T$) vs. time ($t$) graph for both degenerate (left panel) and non-degenerate (right panel) limits with $ \rm{M}=1.0\rm{M}_{\odot}$ and $m_{a}=0\rm{eV}, 10^{-5}\rm{eV}, 10^{-3}\rm{eV}, 10^{-2}\rm{eV}$ (from top to bottom).  The observational data for three pulsars PSR B0656+14, Geminga and PSR B1055-52 are shown by dots with error bars from left to right.}
\label{fig:6}
\end{figure}
\begin{figure}
\includegraphics[width=8.5cm,height=9cm]{dtvst14.png}
\includegraphics[width=8.5cm,height=9cm]{ndtvst14.png}
\caption{Same as in Fig. \ref{fig:6} but for $ \rm{M}=1.4\rm{M}_{\odot}$}
\label{fig:7}
\end{figure}
\begin{figure}
\includegraphics[width=8.5cm,height=9.5cm]{dtvst18.png}
\includegraphics[width=8.5cm,height=9.5cm]{ndtvst18.png}
\caption{Same as in Fig. \ref{fig:6} but for $ \rm{M}=1.8\rm{M}_{\odot}$}
\label{fig:8}
\end{figure}
\begin{figure}
\includegraphics[width=5.5cm,height=7cm]{dvsnd105l.png}
\includegraphics[width=5.5cm,height=7cm]{dvsnd145l.png}\includegraphics[width=5.5cm,height=7cm]{dvsnd185l.png}
\caption{Comparison between degenerate and non-degenerate limits for $L$ vs. $t$ plot with $m_{a}$=$10^{-5}\rm{eV}$ and $ \rm{M}=1.0\rm{M}_{\odot}$, $ \rm{M}=1.4\rm{M}_{\odot}$ and $ \rm{M}=1.8\rm{M}_{\odot}$ (from left to right).}
\label{fig:9}
\end{figure}
\begin{figure}
\includegraphics[width=5.5cm,height=7cm]{dvsnd103l.png}
\includegraphics[width=5.5cm,height=7cm]{dvsnd143l.png}\includegraphics[width=5.5cm,height=7cm]{dvsnd183l.png}
\caption{Same as in Fig. \ref{fig:9} but for $m_{a}$=$10^{-3}\rm{eV}$.}
\label{fig:10}
\end{figure}
\begin{figure}
\includegraphics[width=5.5cm,height=7cm]{dvsnd105t.png}
\includegraphics[width=5.5cm,height=7cm]{dvsnd145t.png}\includegraphics[width=5.5cm,height=7cm]{dvsnd185t.png}
\caption{Comparison between degenerate and non-degenerate limits for $T$ vs. $t$ plot with $m_{a}$=$10^{-5}\rm{eV}$ and $ \rm{M}=1.0\rm{M}_{\odot}$, $ \rm{M}=1.4\rm{M}_{\odot}$ and $ \rm{M}=1.8\rm{M}_{\odot}$ (from left to right).}
\label{fig:11}
\end{figure}
\begin{figure}
\includegraphics[width=5.5cm,height=7cm]{dvsnd103t.png}
\includegraphics[width=5.5cm,height=7cm]{dvsnd143t.png}\includegraphics[width=5.5cm,height=7cm]{dvsnd183t.png}
\caption{Same as in Fig. \ref{fig:11} but for $m_{a}$=$10^{-3}\rm{eV}$.}
\label{fig:12}
\end{figure}

\newpage
\section{Summary and Discussions}
In this work, we have explored the effect of axion emission on the cooling of neutron stars. For the axion emission we consider nucleon-nucleon axion bremsstrahlung process. We have made our analysis for the stars considering degenerate and non-degenerate limits. In earlier such works related to axion cooling of neutron stars, only degenerate process has been considered. For the present purpose, we adopt the APR equation of state. However, one can use other EoS available in the literature. From our analyses, we find that the axion emission effects the neutron star cooling through other estrablished processes such as gamma and neutrino emissions. We have demonstrated this by considering three axion masses, namely $10^{-5}\rm{eV}$, $10^{-3}\rm{eV}$ and $10^{-2}\rm{eV}$ and the neutron star masses of 1.0${M}_{\odot}$, 1.4${M}_{\odot}$ and 1.8${M}_{\odot}$. For comparison with observational results, we used luminosity and temperature of three pulsars namely PSR B0656+14, Geminga and PSR B1055-52. We demonstrate our results by calculating the variations luminosity and temperature of neutron stars with time. While for the neutron star masses 1.0${M}_{\odot}$, 1.4${M}_{\odot}$ the observational points barely agrees with these variations, for the neutron star mass of 1.8${M}_{\odot}$ this agreement appears to improve marginally. From these analyses, we derive a bound on axion masses $m_{a}\leq10^{-3}$ which implies that the decay constant $f_{a}\geq 0.6\times10^{10}\rm{GeV}$. We also find that the cooling patterns for degenerate and non-degenerate cases are different. This difference increases with the mass of the emitted axion. More elaborate studies involving other equation of states are required to obtain better insight of the effect of axion emission on neutron star cooling. This is for posterity.

redpajama_set_name: RedPajamaArXiv


text:
Semtech Releases Next-Generation LinkCharge® 20 Series Wireless Charging Platform
The new chipset provides increased flexibility with 83% efficiency at 20 W nominal power, supports latest fast charging protocols
CAMARILLO, Calif., May. 10, 2018 – Semtech Corporation (Nasdaq: SMTC), a leading supplier of high performance analog and mixed-signal semiconductors and advanced algorithms, announced the next-generation LinkCharge® 20 Series wireless charging platform. The new IC, a 20W mid-power (5W to 20W) wireless-charging transmitter chipset, is based on a simplified controller architecture, allowing for additional flexibility with 83% efficiency, supports present and future fast charging protocols, and reduces system cost.
The new LinkCharge 20 Series chipset, when in range and powered sufficiently, is able to announce its presence to the transmitter to begin a transaction. The transmitter also provides a small amount of power to the newly-discovered receiver, so that the receiver can tell the transmitter what the power requirements are for the receiver. This flexible architecture can be customized in order to wirelessly charge or continuously power devices through a physical layer, such as powering a surveillance camera through a window pane, or charging a phone through furniture. In addition, the firmware of the new wireless charging controller can be updated on transmitter modules that are already deployed in the field.
"Semtech continuously works on having the latest wireless charging platform available and the next-generation LinkCharge 20 Series supports the most recent smartphones fast charging protocols," said Francois Ricodeau, Power and High-Reliability Product Line Manager for Semtech's Wireless and Sensing Products Group. "The new wireless charging platform is a very efficient design with 83% efficiency at nominal power allowing minimal heat dissipation."
LinkCharge 20 Series is immediately available through Semtech and DigiKey. The order code is TSDMTX-19V3-EVM. The datasheet is available on www.semtech.com.
Next-Generation LinkCharge 20 Series Applications:
Smartphone charging pads
Modules for furniture integration
Wireless charging of IoT and connected objects, including LoRa®-based devices
Charging of portable consumer and medical devices
Wireless transfer of power through glass and wood
Aftermarket automotive phone charging docks
Learn more about Semtech Wireless Charging Technology.
Contact Semtech's support team for technical support or general product inquiries.
Follow Semtech on Twitter, LinkedIn, Facebook, YouTube, and Google+.
About Semtech's LinkCharge Platform
Semtech's LinkCharge wireless charging platform provides a range of solutions to enable wireless power in next-generation products for consumers, infrastructure and industrial applications. It includes the LinkCharge 40 Series, the LinkCharge 20 Series, the LinkCharge CT Series, and the LinkCharge LP. The LinkCharge platform is compatible with the major industry standards ensuring end products can quickly charge any wireless charging-equipped device even as the industry adoption continues to grow and evolve. More information about LinkCharge platform and the rest of Semtech's wireless charging solutions is available at www.semtech.com/wireless-charging.
About Semtech
Semtech Corporation is a leading supplier of high performance analog and mixed-signal semiconductors and advanced algorithms for high-end consumer, enterprise computing, communications, and industrial equipment. Products are designed to benefit the engineering community as well as the global community. The Company is dedicated to reducing the impact it, and its products, have on the environment. Internal green programs seek to reduce waste through material and manufacturing control, use of green technology and designing for resource reduction. Publicly traded since 1967, Semtech is listed on the Nasdaq Global Select Market under the symbol SMTC. For more information, visit www.semtech.com.
Forward-Looking and Cautionary Statements
All statements contained herein that are not statements of historical fact, including statements that use the words "can be," "designed to," or other similar words or expressions, that describe Semtech Corporation's or its management's future plans, objectives or goals are "forward-looking statements" and are made pursuant to the Safe-Harbor provisions of the Private Securities Litigation Reform Act of 1995, as amended. Such forward-looking statements involve known and unknown risks, uncertainties and other factors that could cause the actual results of Semtech Corporation to be materially different from the historical results and/or from any future results or outcomes expressed or implied by such forward-looking statements. Such factors are further addressed in Semtech Corporation's annual and quarterly reports, and in other documents or reports, filed with the Securities and Exchange Commission (www.sec.gov) including, without limitation, information under the captions "Management's Discussion and Analysis of Financial Condition and Results of Operations" and "Risk Factors." Semtech Corporation assumes no obligation to update any forward-looking statements in order to reflect events or circumstances that may arise after the date of this release, except as required by law.
Semtech, the Semtech logo, LinkCharge, and LoRaWAN are registered trademarks or service marks of Semtech Corporation or its affiliates.
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Show off your cherished moments, memories, friends and family members with this 5 x 7" Freestanding Twin Aperture Picture Frame from Nicola Spring; a beautifully sleek, sophisticated display.
Built from sturdy acrylic, the strong white lines created by these frames are sure to stand out in a variety of settings. The central hinged design enables you to bend and shape to perfectly suit your photo display needs.
A great housewarming gift, the twin aperture design of this frame also makes an ideal piece for weddings, anniversaries and more.


Musky Mania 10 was held on the Eagle River Chain with the awards held at the Chanticleer Inn. 11 fish were caught during this outing.
Dave Kuen wins Musky Mania 10 with a 35.5" caught on Catfish Lake. 2nd place is Musky Pete with a 31"er from Craneberry and 3rd went to Jim Jessup with a 30.5" Musky from the Eagle chain. Carl Brusky wins smallest Musky with a 25" fish.
Dave Kuen made the award for the smallest Musky, a very large white wooden bait to be passed on at each MM.
Lunch was held on Cranberry Island provided by Ray Bergen and wife, sandwiches and fruit. Musky Pete came into Cranberry Lake from Catfish Lake and notices 2 guys trolling. Trolling is illegal in Vilas county, so he goes over to tell them and guess what. It is two guys fishing Musky Mania, Ed Werner and Ken Enloe. I tell them it is illegal to troll and they say that they troll in Canada. Well you are not in Canada. I think they kept on trolling.
I go around the island on Cranberry and see a boat waving me over. It is Greg and Kevin Kelly. "Greg caught his first musky and wants you to take his picture". OK, where is it. They pull up a stringer with a 27" musky on it. "Hey you can't put an illegal fish on a stringer, you might get caught and fined". Well, Musky Pete take his photo and they release it.


text:
using System;
using System.Collections.Generic;
using System.Linq;
using System.Text;

namespace DataWings.Assertions.Conventions
{
    public enum DbTableNameConventionType
    {
        ClassNameEqualsTableName,

        Custom
    }

    [AttributeUsage(AttributeTargets.Method | AttributeTargets.Class, AllowMultiple = true)]
    public class DbTableNameConventionAttribute : Attribute
    {
        private DbTableNameConventionType conventionType;
        private string convention;

        public DbTableNameConventionAttribute(DbTableNameConventionType conventionType)
        {
            this.conventionType = conventionType;
        }

        /// <summary>
        /// Gets or sets the name of the entity. If this property
        /// returns null, the attribute is applicable for all
        /// entities that are not otherwise mentioned in some
        /// other attribute decoration
        /// </summary>
        /// <value>The name of the entity.</value>
        public Type EntityType { get; set; }

        /// <summary>
        /// Gets or sets the convention to be used. This
        /// </summary>
        /// <value>The convention.</value>
        public string Convention
        {
            get { return convention; }
            set
            {
                if (value == null)
                {
                    convention = null;
                }
                else
                {
                    if (!value.Contains("{0}"))
                        throw new ArgumentException("Convention for DbTableNameConvention must contain '{0}'");

                    convention = value;
                }
            }
        }

        public string GetTableName(Type entityType)
        {
            if (DbTableNameConventionType.ClassNameEqualsTableName == conventionType)
                return entityType.Name;

            if (Convention == null)
                throw new InvalidOperationException("Convention type is Custom, but convention is not set.");

            return string.Format(Convention, entityType.Name);
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
WB Games Announces 'LEGO Harry Potter Collection' for PS4
WB Games Announces 'LEGO Harry Potter Collection' for PS4
Motwera Thursday, September 8, 2016 GamingLeave a Comment
WB Games announced today that the rumored LEGO Harry Potter Collection is releasing this fall on the PS4. While other platforms aren't announced yet, its likely the title will be coming to the PS3, Xbox 360, Xbox One, and Wii U in the future. The full press release from WB Games UK can be found below, but this applies to NA as well.
Source: NeoGaf via WB Games UK Press Release
Warner Bros. Interactive Entertainment and TT Games today announced the LEGO® Harry Potter™ Collection, bringing LEGO® Harry Potter™: Years 1-4 and LEGO® Harry Potter™: Years 5-7 to the PlayStation®4 computer entertainment system for the first time with both top-selling videogames remastered on one disc.
Launching on 21st October 2016 in Europe, this compilation unites the creative prowess of LEGO ® and the expansive world of Harry Potter, with an exciting journey full of spell-casting, potion-making, puzzle-solving, lessons, dueling and much more for players young and old to enjoy. Gamers can experience the entire LEGO Harry Potter adventure featuring content from seven books and eight films, with enhanced graphics, environments, lighting and visual effects, along with two downloadable content (DLC) packs. Sure to delight fans of J.K. Rowling's ever-expanding Wizarding World, the LEGO Harry Potter Collection serves as a perfect gift for those eagerly anticipating the upcoming film, Fantastic Beasts and Where to Find Them.
· LEGO Harry Potter: Years 1-4 is based on the first four books and films—Harry Potter and the Philosophers stone ™, Harry Potter and the Chamber of Secrets ™, Harry Potter and the Prisoner of Azkaban ™ and Harry Potter and the Goblet of Fire ™—allowing fans to experience Harry's first four years at Hogwarts School of Witchcraft and Wizardry in full LEGO form.
· LEGO Harry Potter: Years 5-7 transports players through the final three books and final four films—Harry Potter and the Order of the Phoenix™, Harry Potter and the Half-Blood Prince™ and Harry Potter and the Deathly Hallows™—to experience Harry's last years at Hogwarts™ and his battle against Lord Voldemort™ in the ultimate fight between good and evil.
· Character Pack DLC included on disc featuring 10 characters—Godric Gryffindor, Harry (Yule Ball), Helga Hufflepuff, Lockhart (Straightjacket), Luna (Lion Head), Peeves, Hermione (Pink Dress), Ron Weasley (Ghoul), Rowena Ravenclaw and Salazar Slytherin.
· Spell Pack DLC included on disc featuring 5 spells—Cantis, Densaugeo, Ducklifors, Melofors and Tentaclifors.
· Available on 21st October, 2016 in Europe for a suggested retail price of £39.99.


text:
Secret EU budget vote is unacceptable
MEPs - have they forgotten who gave them their mandate? (Photo: europarl.europa.eu)
By Karl Sigfrid and Andreas Norlen
Brussels, 27. Feb 2013, 08:40
Earlier this month EU leaders agreed for the first time ever to a cut in the long term budget of the European Union.
At that meeting, hawkish countries such as the UK, Denmark and Sweden managed to achieve an agreement that will reduce the 2014-2020 budget from €977 to €960 billion.
But the budget drama is not over. New for this budget process is that the European Parliament gets to accept or reject the result of the summit.
Top MEPs have so far expressed mostly negative sentiments, with most of the parliament having backed the European Commission's original and far bigger budget proposal.
The European Parliament believes that the EU needs more money, not less. But when the resources are limited, a choice must be made and the heads of state and government chose austerity in times of economic crisis.
For our part, we feel certain that a great majority of Europeans would find it reasonable that the EU is now run on a smaller budget.
But we are less sure that the majority of euro-deputies will vote for the much-needed slimmed down proposal.
Some MEPs argue it is natural to support budget increases if you represent Europe as a whole.
These members have misunderstood their role. Unlike EU commissioners, who are appointed to represent the EU as such, MEPs have a mandate from their constituents at home.
Is it possible that MEPs realise they are not going to become popular at home by voting for increased spending?
EU parliament president, German Socialist Martin Schultz, has suggested there may be a secret ballot on the budget. This would make it impossible to see how each deputy voted. Schulz explained such a vote could mean that MEPs would not be put under pressure by their national governments or those they represent.
But If they go against the wishes of their constituents they could be voted out of office in the 2014 elections.
Secret ballots in this context are unacceptable. If you are elected by the people to a political assembly, then the people must be able to hold you accountable.
When former US leader Ronald Reagan felt unsure whether the Congress would support his tax reform in 1981 he coined a famous phrase: "When you can't make them see the light, make them feel the heat."
Reagan encouraged voters to call their members of Congress and give their opinion. The Congressmen were drowned in phone calls from citizens who wanted tax cuts and the proposal passed.
Now it is time for some of the members of the European Parliament to hear what their constituents think.
Should the EU budget be cut back in harsh times as is the case in member states, or should the trend of spending more than the previous round continue?
Should the vote on the budget be open and democratic, or should it be a secret procedure impossible to scrutinise?
We call on citizens to email their representative in the European Parliament to find out whether they want to reveal their position.
The writers are members of the Swedish parliament for the centre-right Moderate Party
The views expressed in this opinion piece are the author's, not those of EUobserver.
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Dr. Kisida is an Assistant Research Professor in the Department of Economics and the Truman School of Public Affairs at the University of Missouri. He has over a decade of experience in rigorous program evaluation and policy analysis. The dominant theme of his research focuses on identifying effective educational options and experiences for at-risk students that can close the achievement gap, the experience gap, and the attainment gap. His research has examined the educational benefits of cultural institutions, school-community partnerships, art and music education, teacher diversity, urban charter schools, and the cognitive and non-cognitive effects of means-tested school choice programs for at-risk students. His academic publications include articles in the Journal of Policy Analysis and Management, Sociology of Education, Educational Researcher, and the Journal of Research on Educational Effectiveness. His work has been cited in congressional testimony and has appeared in numerous media outlets, including The New York Times, USA Today, The Washington Post, The Wall Street Journal, and CNN. Reach him on Twitter at @briankisida.