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Helreið Brynhildar (Old Norse 'The Hel-ride of Brynhild') is a short Old Norse poem that is found in the Poetic Edda. Most of the poem (except stanza 6) is also quoted in Norna-Gests þáttr.

Henry Adams Bellows says in his commentaries that the poem is a masterpiece with an "extraordinary degree of dramatic unity" and that it is one of the "most vivid and powerful" poems in the Poetic Edda. It has, however, been argued that some parts originally belonged to Sigrdrífumál, and the two poems are anyway very close in content. The material is mostly Scandinavian and there are few elements that connect it with the corresponding German tradition found in the Nibelungenlied.

Synopsis
The poem deals with how the dead Sigurd and Brynhildr are burnt on two pyres. First they burn Sigurd and then they burn Brynhildr who is lying on a richly clad wagon. This wagon takes Brynhildr on her journey to the afterlife. During her journey, she passes a house where a giantess (gýgr) lived.

The giantess accuses Brynhildr of having caused the deaths of heroes and of having wanted another woman's husband (Sigurd). The giantess further accuses Brynhildr of having caused the fall of the house of Nibelungs (Gjúki's sons). Brynhildr responds that she will tell her the truth and how the sons of Gjúki made her an unhappy oath-breaker.

Formerly, she used to be called Hildr the helmed and she lived in a dwelling of valkyries called Hlymdalir. Then a monarch (presumably Agnarr) captured Brynhildr and her seven sisters' by taking their swan-robes that he found under an oak. She was only twelve winters old when she married the young king.

Against the will of Odin, she then made the aged Hjalmgunnar, the king of the Goths, die and instead she gave victory to Auða's young brother (Agnarr). The angry Odin imprisoned her in Skatalund within red and white overlapping shields, and cursed her to sleep until a man without fear would set her free. In order to make it even harder to liberate her, Odin also created a circle of fire around her resting place.

Sigurd then arrived on Grani and brought her Fafnir's gold. The hero shared her bed during eight nights without them touching each other. Still, Gudrun would reproach her for having slept in Sigurd's arms, and then admit to her that they had tricked her out of her relationship with Sigurd and made her take another man instead (Gunnar).

Brynhildr finishes the poem by stating that men and women live in this world to suffer, but that she and Sigurd would never part again:

References

Bibliography

Further reading

 Brynhild's Hell-Ride, Henry Adams Bellows' translation and commentary
 Brynhild´s Hel-ride, Benjamin Thorpe's translation
 Brynhild's Hel Ride, Translated by W. H. Auden and P. B. Taylor
 Helreið Brynhildar, Sophus Bugge's edition of the manuscript text
 Helreið Brynhildar, Guðni Jónsson's edition with normalized spelling

Eddic poetry
Sources of Norse mythology
Nibelung tradition
Swan maidens
Brunhild

redpajama_set_name: RedPajamaWikipedia


text:
the Weblog of Nancye Blair Black
Engaging Education
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In addition to increasing engagement and depth of learning,
it gives students dignity, confidence and identity...
Willard Wigan has dyslexia. He can't read. Can't write. When he remembers being in school, he remembers feeling like nothing. A nobody. Yet, he is definitely a somebody in the art world. Nevertheless, Wigan's life's work exists on a scale that most of us cannot even comprehend, possibly even imagine. How many times do you think he was told it couldn't be done? How many times do you think he was told to stop building houses for ants and "make something of himself?" Yet, Wigan didn't listen. He found his own voice, his own dream…
And now, he believes he is Something, Somebody.
Everyday in classrooms around the world, there are students who feel like nothing. Students who feel like they have no control over the direction of their formal education, who feel bored with rote memorization, who feel trapped by the restrictions of traditional assignments and rubrics. Their education is meaningless to them.
Yet, when we put the power of learning, the power of creating, into the students' hands and see the reaches they can achieve, something surprising happens. They don't see the limits that we as adults assume are there. They don't know what is too big or too small to achieve. Anything is possible. And in the face of creating these unseen possibilities, our students discover that they have more potential and worth that they had imagined.
They become Something.
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text:
È di origine iraniana.

Carriera
Nel 2010 ha coscritto e coprodotto il brano Miss Me di Mohombi. Nel 2011 è autore e produttore di molti brani dell'album Alive di Linda Pritchard. Inoltre scrive e/o produce brani per Eric Saade (in Saade Vol. 2) e The Lonely Island (nell'album Turtleneck & Chain).

Nel periodo 2012-2013 collabora tra gli altri, in diversi ruoli, con Fifth Harmony (Me & My Girls), Cher Lloyd (I Wish), David Lindgren (Get Started), Anton Ewald e Amanda Fondell.

Nel 2014 coscrive e/o coproduce molte hit internazionali, tra cui Problem e One Last Time di Ariana Grande, First Love di Jennifer Lopez e Bang Bang di Jessie J (featuring Ariana Grande e Nicki Minaj). Inoltre, collabora per Comeback di Ella Eyre e alcuni brani dell'album Universe di Mohombi.

L'anno seguente, ossia il 2015, continua ad essere al lavoro con molti tra gli artisti principali della scena mainstream globale: Ariana Grande (Focus), Taylor Swift (Bad Blood), Ellie Goulding (Love Me like You Do, On My Mind, Codes), Demi Lovato (Confident), Adam Lambert (Things I Didn't Say), Tori Kelly (City Dove), Prince Royce (Back It Up), Sage the Gemini (Good Thing), Natalie La Rose (Around the World), Hilary Duff (One in a Million) e altri.

Nel 2016 è quasi interamente produttore del terzo disco di Ariana Grande, Dangerous Woman, co-scrivendo e producendo i singoli di grande successo internazionale  Into You e Side to Side.

Nel 2018 continua a lavorare con Ariana Grande, co-scrivendo insieme all'interprete moltissime delle canzoni del suo quarto album in studio, Sweetener, tra cui le hit God is a woman e Breathin. Prosegue nel 2019 producendo maggior parte delle tracce del quinto album della Grande, Thank U, Next, oltre a collaborare con la stessa aiutando nella composizione di alcuni testi delle canzoni contenute nel disco, tra cui il singolo di fama internazionale Break Up with Your Girlfriend, I'm Bored.

Collegamenti esterni


LuLu Financial Group, the leading financial services and payments solution brand, started its operations in Hong Kong with the inauguration of their head office at Hankow Centre in Kowloon.
Adeeb Ahamed, MD, LuLu Financial Group along with Surendran Amittathody, VP-APAC, LuLu Financial Group, Priscilla Law, Head of Financial Services, Invest Hong Kong, Rajiv Raipancholla, CEO, Orient Exchange and officials from the Philippines Consulate General, Hong Kong during the opening of the LuLu Financial Group's Hong Kong head office at Hankow Centre in Kowloon (Photo: AETOSWire).
LuLu Financial Group is an ISO 9001:2015 certified global financial services enterprise that serves banking institutions, business houses, local and international corporations as well as individuals. The group's services are designed to facilitate secure and instant financial transactions through digitized state-of-the-art systems that deliver flexibility, reliability, and transparency.


GLAS is proud to announce their sponsorship of Global ABS, Europe's most significant securitisation event.
After an extremely successful Global ABS in Barcelona last week our delegates are back in the office. The GLAS sponsored conference was very well attended with close to 4,000 structured finance professionals and the mood was one of optimism.
GLAS welcomed delegates to our stand where the team enjoyed meeting clients, contacts and old friends and discussing GLAS' services and market updates.
On Wednesday afternoon GLAS CEO and Founder, Mia Drennan, was a panel speaker and participated in a lively discussion around "Hot Spots for Performing and Re-Performing Portfolio Disposals in 2018".
The panel were in agreement that bank deleveraging continues to be a driver of European loan portfolio sales, and that securitisation continues to play a key role in the refinancing of these portfolio acquisitions. GLAS has recently witnessed this first hand, acting as Note Trustee, Security Agent and Registrar on the securitisation of an NPL portfolio of Spanish real estate assets.
Other key themes which emerged across the week included the development of a broader range of transactions with more focus on esoteric asset classes; the re-emergence of CMBS; and the continuing proliferation of innovative marketplace lending platforms and use of fintech in the structured finance industry.
There was also much discussion around the role of the trustee in structured finance transactions, which was centred on key considerations in relation to indemnities, dispute resolution and exercising discretion.
GLAS is getting ready to head to Barcelona next week for #GlobalABS We have some exciting giveaways to share with you and information on new products and services. Come find us on the floor, we look forward to seeing you. Don't forget the suncream!
Please feel free to stop by our booth to meet the team and discuss our services!
For more information please visit https://www.imn.org/ or contact media@glas.agency.
GLAS are proud to be an Associate Sponsor of the 22nd Annual Global ABS taking place on 5-7 June 2018, in Barcelona, Spain.
The event run by AFME and IMN is expected to attract over 3,500 leaders in the global ABS market, making it the largest annual European structured finance gathering.
Past keynote speakers have included Members of the European Parliament, senior leaders at the European Central Bank and European Banking Authority, ESMA, and other important regulatory and political figures.


What precautions should be taken after a hernia surgery?
Home » Frequently asked Questions on Health » What precautions should be taken after a hernia surgery?
Q: What measures should be taken after a hernia surgery?
A:Take precautions for 12 weeks. Avoid lifting heavy weights for 12 weeks. Also, avoid very strenuous exercise. Walking permitted early. Running permitted after two to three weeks usually (ask your doctor). Driving a car permitted after two to three weeks. Motorcycle riding, pillion, permitted after three weeks, but kicking and driving only after four to six weeks. Guard against constipation and cough - These can cause hernia recurrence. Wound - This needs very little maintenance. Wash it with soap and water after four or five days. No dressing is needed after this.


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text:
CGBets: Betting Bitcoin on Games of 'Skills, Not Luck'
Bitcoinist | Oct 18, 2016 | 21:57
CGBets is a new gambling platform that allows users to wager bitcoin against other gamers as they go head-to-head in skill and logic-based multiplayer games.
Disclaimer: This article is sponsored by Bitcoin PR Buzz.
CGBets Offers Games of Skill
On the platform, players compete against each other in flash-based games. According to a press release, the following games are currently available:
Basketball game – A game for two or more players where they are required to shoot the ball into the hoop to gain as many points as possible.
Go game – A two player logical board game whose invention can be traced back to a Chinese emperor's son. The game, not yet solved by any algorithm can be played only by live participants.
Chess – A familiar two player game on a chequered board with 64 squares arranged in an 8×8 grid.
The company told press that it would soon add "Duplicate Poker," a game it says "is a variant of the Poker card game based on Texas Hold'em Rules. It is more of a strategy game with no luck factor involved."
CGBets says its model sets itself apart from other bitcoin gambling platforms because it lets players bet on their own skills rather than luck.
Boasting high quality service, a company representative told press, "We provide high-quality games written in flash technology. We ensure optimum functionality of our gaming platform, guarantee secure, easy settlement and the withdrawal of winnings."
The company also claims to have a large degree of fairness on its platform because players always compete against real humans and not AI. "This way," the team said in a press release, "it is not the house but the best player who always wins."
An Apparent Demand for Blockchain-Based Gaming Platforms
Other cryptocurrency-based platforms have offered the same premise to people competing in console or PC games, such as Call of Duty or League of Legends.
Gamerholic, for example, provides a casual competition platform, letting users make bitcoin bets for online matches.
FirstBlood, an Ethereum-based gaming platform, caters to the highly competitive eSports market, employing smart contracts and cryptocurrency to decentralize the matchmaking and judgement mechanisms common in eSports platforms.
Showcasing the apparent demand for blockchain gaming platforms, FirstBlood's ICO sold out in minutes, raising $5.5 million USD.
What do you think about CGBets? Let us know in the comments below.
Images courtesy of CGBets.
Tags: Bitcoin betting, Bitcoin Wagers, CGBets, FirstBlood, Gamerholic


This is a placeholder page for Michelle Billaris, which means this person is not currently on this site. We do suggest using the tools below to find Michelle Billaris.
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text:
Melting Gold With Lasers May Hold the Key to Surviving the Surface of Venus
Scientists at Stanford think gold can do a lot more than line space helmets.
Matthew Phelan
Gold has a lot of pretty cool industrial applications. NASA uses it to protect astronauts from cosmic radiation by lining the visors of their space helmets. Commercial electronics also use gold to plate contact points to prevent static and corrosion. But this may only be the beginning, says a group of researchers at Stanford who are battering gold with laser beams to understand the full extent of what the shiny metal can really do.
"We can now actually see what is happening on the atomic scale," plasma physicist Siegfried Glenzer, director of the High-Energy-Density division at SLAC, tells Inverse. "That's quite significant."
Visualizing gold at the atomic scale required a number of technological breakthroughs, but that's exactly what the National Accelerator Laboratory at the Stanford Linear Accelerator Center (SLAC) did recently, a feat which required developing a device that could watch what was happening to those individual atoms of gold at a timescale down near 100 femtoseconds (meaning 100 millionths of a billionth of a second).
"Previously," Glenzer says, "we've had microscopes and we've had more and more improved tools, but this is really now the first time that we can see what atoms are doing, where the atoms are sitting, and then measuring how the atoms are moving around — where the atoms go as we excite the material."
"Excite," here, is a polite term for blasting gold with a pulsing ultraviolet beam until it reaches temperatures approaching those deep within Earth's mantle, near its molten outer core. (The gold gets to about 3500K±500 K — or between about 4900 to 6700 degrees Fahrenheit. Gold's melting point is 1948 degrees Fahrenheit.)
To actually capture what was happening with the gold as it melted, they basically had to manufacture a precise, "slow-motion camera" of sorts. What that means at the atomic scale is that the team at SLAC bounced a lot of incredibly fast-moving electrons off of the melting gold and then measured how those electrons behaved, a process called ultrafast electron diffraction (UED).
According to Glenzer, "You fire a laser beam on copper, you extract electrons, you catch those electrons in an electromagnetic field, and so on. Then you accelerate those."
Glenzer's group actually borrowed the free electron laser they needed from Stanford's Linac Coherent Light Source (LCLS) facility.
"They had, like, a spare gun, and we were allowed to use that spare gun to build UED."
A laser pulse melts solid gold (the dotted pattern) to a liquid (the ring pattern), as seen by SLAC's ultrafast electron camera. Mianzhen Mo / SLAC National Accelerator Laboratory
What We Can Learn by Melting Gold
So, how does gold melt when you torch it with an ultraviolet laser? What the group discovered was that the regions of gold with consistently spaced atoms in a well-organized crystalline latticework melted last, after all the more disorganized regions in between those homogenous areas melted first. It's a little bit like ice cubes, if you've ever seen tiny bits of ice melt faster than large blocks of ice.
Understanding how these crystal lattice fault-lines in gold first fracture and then melt — and just generally react to energy bombardment — should help scientists and engineers design better protective gold materials for space travel, as well as for future fusion reactor experiments.
"In outer space, the environment is pretty harsh," says Mianzhen Mo, a postdoctoral researcher at Stanford who has been focusing on the molecular geometry of "warm dense gold" and who played a pivotal role in this gold-melting research. "There's super-energetic particles, ions, and protons. So, those particles are going to, like, hit your spacecraft — and those interactions, the bombardment, can actually change the material properties."
Mo told Inverse he expects UED observational methods will also be used with other specialty materials designed for space and other extreme conditions. As an example, he mentioned silicon-carbide semiconductors that Stanford alumn Samira Motiwala has been investigating with NASA for use in a probe capable of surviving on the 864 degrees Fahrenheit surface of Venus.
"Previously," Glenzer says, "they sent a device to Venus. I think it was a Russian probe. It survived for two minutes and then it was over."
"And, actually, the conditions on Venus are still fairly okay compared to fusion reactors. Fusion reactors would be much more extreme."
This is a gold-plated hohlraum mock-up from the National Ignition Facility, a laser-based inertial confinement fusion (ICF) experimental unit, at Lawrence Livermore National Laboratory in California. Lawrence Livermore National Laboratory
High-tech materials are not the only area of scientific inquiry that might benefit from UED, however. Glenzer and Mo's research, conducted by Stanford on behalf of the US Department of Energy Office of Science, and published last Friday in Science, could also expand into other fields where observing the ultrafast (and very tiny) atomic activities during molecular reactions might come in handy.
"People have begun using UED also to study chemical reactions, study reactions that are important in biology," Glenzer says. "I think this is just the start."
Time-lapse shows shocking temperature changes between December and January
NASA ends Geotail mission and more: Understand the world through 7 images


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Home/Steering Committee/Alfred E. Smith, IV
Business advisor, investor, executive counselor, philanthropist — these are terms frequently used to describe Al Smith IV, founder and chief executive officer of A.E. Smith Associates. Barack Obama, Tony Blair, and leaders of corporations around the globe know Al Smith and call him friend.
After 35 successful years on Wall Street working as a specialist and member of the New York Stock Exchange, Al founded his own firm in 2009 while simultaneously sustaining a long list of corporate and philanthropic activities. As the great-grandson of the legendary Al Smith, four-time governor of New York, he served as the director, secretary, and dinner chairman for the Alfred E. Smith Memorial Foundation, as well as master of ceremonies at the annual Alfred E. Smith Foundation Dinner for 32 years. Guests of honor at the 2012 dinner included President Barack Obama and Governor Mitt Romney.
Al also serves on the board of the Global Tracheostomy Collaborative, Stamford Hospital Foundation and Mutual of America. He served as the chair for the Tony Blair Faith Foundation as well as a member of the Kroll Bond Rating Agency among many other civic and business endeavors.
Among the youngest members ever to join the New York Stock Exchange, Al began his Wall Street career as an independent floor broker, later relocating to Chicago to join Mitchell-Hutchins, where he served as vice president until 1979. Upon returning to New York, he was named partner of CMJ Partners. In 1997, he joined Bear Wagner as managing director, a position he held until 2006.
Al's work on behalf of charities in New York and Connecticut is extensive. He is the chairman of Hackers for Hope, an organization he founded in 1988 to raise money for cancer research and treatment. Since its inception, Hackers for Hope has donated over $17,000,000 to the Bennett Cancer Center, Saint Vincent Catholic Medical Centers Comprehensive Cancer Center, Memorial Sloan Kettering Cancer Center and other organizations committed to finding a cure for and treating cancer.
He also served as chairman of the Irish Chamber of Commerce, served as trustee of Calvary Hospital, past president of the Friendly Sons of St. Patrick and served as chairman of the board of St. Vincent's Hospital in Manhattan. Over the years, Al has received numerous honors and awards including:
Ellis Island Medal of Honor;
National Brotherhood Award, National Conference of Christians and Jews;
American Cancer Society's Gold Sword of Hope Award;
Terence Cardinal Cooke Humanitarian Award.
In 2013, Al was named grand marshal of the St. Patrick's Day Parade in New York City. He is married to Nan Moore Smith. They have two children and six grandchildren.


text:
Q: How to create an object with the name and frequency count from an object array with lodash I have an array like this:
const blogs = [
  {
    _id: "5a422a851b54a676234d17f7",
    title: "React patterns",
    author: "Michael Chan",
    url: "https://reactpatterns.com/",
    likes: 7,
    __v: 0
  },
  {
    _id: "5a422ba71b54a676234d17fb",
    title: "TDD harms architecture",
    author: "Robert C. Martin",
    url: "http://blog.cleancoder.com/uncle-bob/2017/03/03/TDD-Harms-Architecture.html",
    likes: 0,
    __v: 0
  },
  {
    _id: "5a422bc61b54a676234d17fc",
    title: "Type wars",
    author: "Robert C. Martin",
    url: "http://blog.cleancoder.com/uncle-bob/2016/05/01/TypeWars.html",
    likes: 2,
    __v: 0
  }
]

I want to have at least an object like this:
{
    "name":"Robert C. Martin",
    "blogs": 2,
}

I try with lodash but can't understand how I can count the number of blogs for one author.
_.maxBy(blogs, 'author') //gives me the author with the maximum of blogs
_.groupBy(blogs, 'author') // group all blogs in an array under the author name
// _.countBy(blogs,'entries') //that doesn't work

A: This is easy enough to do with plain JavaScript (see Array.prototype.reduce) if you didnt want to use lodash, for example:

const blogs = [{
    _id: "5a422a851b54a676234d17f7",
    title: "React patterns",
    author: "Michael Chan",
    url: "https://reactpatterns.com/",
    likes: 7,
    __v: 0
  },
  {
    _id: "5a422ba71b54a676234d17fb",
    title: "TDD harms architecture",
    author: "Robert C. Martin",
    url: "http://blog.cleancoder.com/uncle-bob/2017/03/03/TDD-Harms-Architecture.html",
    likes: 0,
    __v: 0
  },
  {
    _id: "5a422bc61b54a676234d17fc",
    title: "Type wars",
    author: "Robert C. Martin",
    url: "http://blog.cleancoder.com/uncle-bob/2016/05/01/TypeWars.html",
    likes: 2,
    __v: 0
  }
];

const blogAuthorCounter = blogs.reduce((obj, blog) => {
  obj[blog.author] = obj[blog.author] ? obj[blog.author] + 1 : 1;

  return obj;
}, {});

Object.entries(blogAuthorCounter).forEach(entry => {
  const [author, count] = entry;

  console.log(`${author} = ${count}`);
});

redpajama_set_name: RedPajamaStackExchange


text:
El Paso's Hilton Hotel debuts as city's tallest building with fastest elevators
Trish Long
The newly renovated Plaza Hotel Pioneer Park that opened June 17 got its start in 1930 as the Hilton Hotel, the tallest building in El Paso at the time.
The hotel, built by Conrad Hilton, debuted Nov. 6, 1930, with the fastest elevators, radio speakers in the chandeliers and custom furniture.
In 1950, actress Elizabeth Taylor married Hilton's son, Conrad "Nicky" Hilton Jr.
In March 1950, Taylor stayed at the hotel, where she made wedding plans. After the couple married, they again stayed at the hotel while visiting Hilton's mother, Mrs. Mack Saxon. They were married for 205 days before finalizing their divorce in 1951.
In 1963, the hotel was bought by the Plaza Motor Hotel Corp. and became the Plaza Motor Hotel and later just the Plaza Hotel.
More:Great Depression's El Paso Hilton reborn as Plaza Hotel Pioneer Park in great pandemic
From the Nov. 5, 1930, Hilton Hotel Section of the El Paso Times:
20-story hotel to be on display from basement to flagpole
Open house to the people of El Paso and the Southwest will be held by the new $1,000,000 350-room Hilton hotel, beginning at 10 a.m. and lasting all day tomorrow.
Everybody in El Paso and surrounding territory is invited by President C.N. Hilton to inspect the building on opening day, and to participate in the opening festivities. ...
"This hotel, built from basement to flag mast as much as possible of El Paso materials by El Paso artisans and contractors, is an El Paso institution," said President Hilton, "and we want the people of this city and section to feel right at home in the hotel on opening day."
Chandeliers conceal radio speakers
Music from the chandeliers! That's a new wrinkle employed in the rooms in the Hilton hotel. Every one of the 350 rooms is equipped for radio.
Four set programs are provided. The guest may plug in for any of these. Immediately a loud speaker concealed in the chandelier starts delivering. The music cannot be heard from one room to another — which is important if musical preferences of guests in adjoining rooms happen to differ.
Elevators go 700 feet a minute
The swiftest elevators in El Paso are in the Hilton hotel. They travel 750 feet a minute, and have automatic leveling and automatic stop devices. Stops are made gradually ... and each cab stops exactly even with the floor, making unnecessary the customary warning, "Watch your step."
The cabs of the three elevators are beautifully furnished in walnut and are enclosed, so that passengers are not aware of the swift movement. The unusual quietness and smoothness of operation of the doors reduces the noise of operation
More:Garry Owen, champion cavalry horse, brought fame to Fort Bliss
Three private dining rooms
The finest place for a private dinner party, a small bridge party or a business conference is one of the private dining rooms of the Hilton hotel.
There are three of these private rooms, each designed, furnished and equipped in distinctive manner
One is paneled to the ceiling in walnut. The sideboard, which is built-in, is of the same wood, beautifully grained. The heavy carpet is in a harmonious green tone, and appropriate drapes hang from the windows. The furniture is heavy, massive oak in the Early English manner. This room is particularly equipped and adapted for "stag" parties, having a chummy, cozy, yet convenient, arrangement.
Another room is more effeminate in tone, being done in the modernistic manner, with furniture, drapes and carpets to conform. Daintiness is its keynote.
The third is done in the French and Italian renaissance manner. It is the largest of the three private dining rooms, and will accommodate 50 persons easily. It is especially designed for large private dinners and bridge parties. A distinctive feature, among many others, in this room is a black and gold mantel, handsomely carved.
More:Here are the benefits of an El Paso Times subscription
Iced air used in dining rooms
Iced air, a new method of cooling the atmosphere during hot weather, will be a feature in the new Hilton hotel dining rooms. The system is different from those in which air is cooled by being "washed" through water. Humidity is kept at a minimum.
Another dining room and coffee shop feature will be the smoothness and noiselessness of operation. The ceiling in both rooms is of gypsum blocks, acoustically treated to absorb the clatter of dishes, rattle of silverware and other noises usually common in eating places.
Trish Long may be reached at tlong@elpasotimes.com or 915-546-6179.


A snow-day journey with Grandma highlights all of the beauty, magic, and fun of winter.
With sparkling flakes calling from outside, this sister and brother bundle up for an outdoor adventure with Grandma. In the hushed woods, they see and hear wildlife thriving under a new blanket of snow. In the bustle of town, they help their grateful Grandpa dig out. Then, it's time to get sledding!
Snowy scenes capture the beauty of freshly fallen snow, and the lyrical verse delights in the magic of playing in the snow and the warm comfort of family.


text:
https://www.barrons.com/articles/support-for-compromise-stimulus-grows-but-deal-still-far-from-done-51607088243
Support for Compromise Stimulus Grows But Deal Still Far From Done
Ben Walsh
Dec. 4, 2020 8:24 am ET
More Republican senators have thrown their support behind a bipartisan coronavirus stimulus plan rolled out earlier this week. Senate Majority Leader Mitch McConnell (R., Ky.) has yet to signal his support for the package, leaving a deal still effectively as far off as it has been for months.
At least 11 Republican senators support the compromise plan as of Thursday, including Joni Ernst (Iowa), John Cornyn (Tex.), Chuck Grassley (Iowa) and Marco Rubio (Fla.). Cornyn told the Washington Post that Democrats' support for the...
More Republican senators have thrown their support behind a bipartisan coronavirus stimulus plan rolled out earlier this week.


text:
Is There a Trick to Making Halloween a Treat?
Our columnist takes a nostalgic look at our most kid-centric holiday and why it has so many of today's parents crying "boo."
Kate Tuttle Oct 21, 2014
This article was made possible because of the generous support of DAME members. Will you contribute just $5 a month to support our journalism?
Halloween is upon us once again, holiday of candy and costumes, pumpkins and (mock) mayhem. As I do every year, I find myself both looking forward to the fun my son will have trick-or-treating (one sweet measure of his growing up is that each fall he roams a little farther, hitting more houses) and looking back at what the holiday meant to me as a kid.
In my old neighborhood, kids went out without any adult supervision at an early age. We lived in a subdivision nowhere near any real traffic, and we travelled in a pack. A few families on our block hosted homemade haunted-house setups—one would invite us in to feel the cold spaghetti they pretended was a bucket full of guts, another ended with the opportunity to bob for apples. Once we got a little older, around 10, we'd wander one neighborhood over and knock on the doors of richer families, who handed out full-size candy bars, coupons for tacos, and—memorably, one year—dollar bills.
(Because my hometown was also home to a producer of educational films for schoolchildren, there's a 1977 movie about Halloween safety starring many of my classmates.)
Holidays always change with the times, even while proclaiming themselves to be immutable touchstones. Christmas, which once dominated a few days, has become a month-long season (one Thanksgiving increasingly focuses on shopping for), and Easter has gone nuts (have your kids asked when they're getting for Easter yet? Mine have. When did this become an occasion for gifts?).
Similarly, Halloween has ballooned. "I don't understand the creep of all the pre-Halloween festivities," said Jennifer, a mom of three in the Boston suburbs. "I feel like it used to be a one-night-only affair and now there are parties pretty much every weekend in October. Not only is it hard to manage three times the level of candy, but I think it takes away from the glory of the main event itself!"
And then there's the arms race of house decorating, crafting, and homemade-costume creation. Think one or two hand-carved pumpkins is enough? I do (although I do believe they MUST be hand-carved), but there are plenty of Halloween-iacs who doll up their places with skeletons, spider webs, gravestones, ghouls, and goblins. Some sport lightshows that rival any Christmas display. At least a few are kind of funny. This one has a soundtrack.
On the other end of the spectrum, some don't mess with Halloween at all. Mostly these objectors refuse on religious grounds. "When I was about 8, our rabbi devoted his pre-Halloween sermon to insisting that Jews shouldn't participate, since in some countries the holiday was an excuse for pogroms," says Brooklyn mom Debbie. "I didn't trick or treat again until college, and I will hate my parents forever for banning Halloween."
Halloween is rejected by people of many different faiths. There are many opinions about Halloween among Jews. Some Christian denominations, especially those on the fundamentalist end, warn against the holiday's pagan roots. Some pagans hate it, too. "My son's preschool discouraged costumes," says Cecilia, a mother from Baltimore, "because they said that Wiccan families felt the typical iconography (witches with pointed hats, broomsticks, etc.) mocked their neo-pagan religious beliefs."
There is agreement on one matter. When I asked a diverse group of parents what they hate about Halloween, one answer dominated: candy. It makes sense; we're all trying to eat better these days, and as parents most of us are far more concerned than our parents were about keeping our kids' bodies more or less junk-free. That said, there's a strong opposing viewpoint, voiced by many, that going nuts about candy one day of the year is a perfectly okay safety valve. If we have made candy a forbidden fruit, doesn't that make Halloween even more truly transgressive and fun for the kids?
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On the other hand, what does it say about how safe we've made our kids' lives that candy is the most dangerous thing we can expose them to?
What I love about Halloween is its focus on magic, creativity, and neighborhood, its openness to allowing kids to explore those liminal spaces of fear and danger, its tension between sweetness (candy) and bitterness (death). At its best, Halloween can make a kid feel like she's temporarily inhabiting a fairy tale—and not a sanitized Disney one, either. When my mother was little, Halloween was actually scary—the older boys in her neighborhood would hide in trees and throw rotten pumpkins down upon the younger kids as they ran (unsupervised) through the woods. I can only imagine the thrill, the racing heartbeats of those kids.
Now, some parents think even supervised trick-or-treating is too dangerous for their kids. Towns increasingly sponsor "trick or trunk" events, daytime affairs where kids walk through parking lots picking up candy from the backs of Subarus. I guess they're spooked by those old urban legends of poisoned or weaponized candy, or the newfangled version in which Colorado parents freaked out about possible weed-laced goodies in their kids' treat bags.
None of these are real dangers.
The only truly awful aspects of Halloween, it seems to me, are those that reflect larger problems in our society: competitive parenting (in the form of extreme crafting and stay-up-all-night handsewn costumes), commercialization (the push to buy more candy and decorations and deploy them all month long), and those twin pillars of evil, racism and sexism.
Parents, if you do anything this Halloween season, do this: resist the urge to buy costumes that sexualize or overly gender your young child. Not because a girl is going to be targeted by pedophiles, but because it affects how she sees herself. And – not coincidentally—the sexy little girl costumes are skimpy and cold, less comfortable and less realistic than those made for boys. Do real female firefighters wear miniskirts as part of their uniforms? No.
Finally, enough with racist costumes. Enough, enough, enough. What is a racist costume, you ask? I am glad you asked, because it's been very nicely explained already, here, here, and here.
Now go forth and get candy!
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Halloween Kids Nostalgia Parental Advisory Parenting
President of the National Book Critics Circle, Kate Tuttle writes about books for the Boston Globe. Her reviews have also appeared in the Los Angeles Times, Salon, the Washington Post, and Newsday. Her essays on raising children, race and politics, and coming to terms with her own 1970s childhood, have appeared in Dame, The Rumpus, The Atlantic, and elsewhere. Follow her @katekilla
More by Kate Tuttle
Revisiting the Terrifying Prophecies of "The Day After"
White Parents' Message to Brown and Black Kids: You Are Not Ours
Robin DiAngelo Wants White People to Confront Their Racism
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text:
\section{Introduction}\label{intro}
There are many factors that cause high-energy particle acceleration, precipitation, and short-term,
 sharp increases in particle count rates in radiation belts, including the influence of
  ground-based VLF electromagentic (EM) transmitters, lightning and thunderstorms,
   and ground nuclear testing. The primary mechanism of ground-based VLF EM transmission is
    that the emitted EM wave is transmitted across the atmosphere, expands into the ionosphere,
    and interacts with the energetic particles in the radiation belt.
    This interaction accelerates the particles by changing their momentum or scattering their pitch angle,
     which causes them to enter the bounce or drift loss cones $LC_{drift}$.
      As a result, a mass of energetic particles accumulates within a certain L-shell and
       yields particle-flux enhancement, which can be observed by the onboard particle detectors of
        satellites\cite{Reeves1998,Li1997,Su2014,Horne2005,Su2011,Thorne2010}.

Numerous experimental observations and theoretical interpretations of the electron-flux enhancement
 induced in the inner radiation belt by VLF ground-based transmitters have been
 reported.

For example, Kimura {\it et al.} have found strong correlations
between the $0.3$--$6.9$-keV electron fluxes observed by the
EXOS-B satellite and the $0.3$--$9$-kHz VLF wave emitted by the
ground-based transmitter at SIPLE\cite{Kimura1983}. The observed
instantaneous correlation between the VLF signal and the electron
fluxes has been studied\cite{Imhof1983} and interpreted using
wave-particle interaction theory\cite{Inan1985}, which was applied
to a test-particle model of a gyroresonant wave-particle
interaction in order to calculate the precipitation
characteristics of the particle flux induced by a VLF transmitter.
Hence, it was found that the particle precipitation is controlled
by the $\alpha$ distribution near the edge of the loss cone.

The Lualualei (NPM) VLF transmitter has been studied by Inan {\it
et al.}\cite{Inan2007}, who have suggested that the energetic
electrons induced by this transmitter, which are scattered at the
NPM longitude, continue to precipitate into the atmosphere as they
drift toward the South Atlantic Anomaly. Further, Graf {\it et
al.} have compared the precipitating fluxes with predictions based
on ray-tracing analysis of the wave propagation and test-particle
modeling of the wave-particle interaction\cite{Graf2009}. Their
results indicate that the precipitated flux of the $>$100-keV
electrons induced by the NPM transmitter peak at $L\simeq 1.9$.
They have also indicated that the detection rate is related to the
orientation of the Detection of Electro-Magnetic Emissions
Transmitted from Earthquake Regions
(DEMETER)\cite{Parrot2006,Sauvaud2006} particle detector,
obtaining agreement between their observations and theory.

Several studies of the electron-precipitation belts induced by the
North West Cape (NWC) VLF ground-based transmitter have also been
conducted, and the events related to this transmitter are the
focus of this paper. Based on readings from the DEMETER satellite,
Sauvaud {\it et al.} have observed NWC-transmitter-induced
enhancements in the ~100--600-keV $LC_{drift}$ electron fluxes at
$L$ values of 1.4--1.7\cite{Sauvaud2008}. These researchers have
calculated the variation in the energy of the enhanced electron
fluxes in response to changes in $L$ using the first-order
cyclotron resonance theory of wave-particle interaction; hence,
they have obtained results consistent with observation.Further, Li
{\it et al.} have analyzed the energy spectra of the NWC electron
belts precisely using an on-off method, and explained the $\alpha$
range by considering the quasi-linear diffusion equation of
wave-particle theory\cite{Li2012}. Independently of the DEMETER
detection of the NWC-transmitter-induced electron enhancement of
$LC_{drift}$, Gamble {\it et al.} have also examined the data for
$>$100-keV quasi-trapped electron fluxes and reported similar
enhanced electron counts from the $90^{\circ}$ electron telescopes
on the National Oceanic and Atmospheric Administration (NOAA) 15,
16, 17, and 18 Polar-orbiting Operational Environmental Satellite
(POES), for the time period in which the NWC transmitter was
broadcasting\cite{Gamble2008}.

In the early work by Kennel {\it et al.} on the pitch angle scattering of radiation-belt particles,
 the gyroresonant wave-particle interactions were thought to play a crucial role in the
  magnetosphere physics\cite{Kernel1966}. Further, scattering by chorus waves was studied as the dominant cause
   of diffuse auroral precipitation\cite{Thorne2010}. One of the theoretical models for numerically
    calculating the precession of waves inducing energetic particle precipitation is
     the quasi-linear diffusion equation. In particular, Summers {\it et al.} have developed
      a precise formula of quasi-linear diffusion coefficient corresponding to R- or L-mode EM waves
      which have a Gaussian spectral density and propagate in a hydrogen plasma\cite{Summers2005}.
       These researchers have expanded the collisionless Vlasov equation for the particle-flux
        differential function to the second-order perturbation and obtained the diffusion equation form.
         In the inner radiation belt, the particle velocities are generally significantly larger than
          the typical phase velocities of the waves; therefore, pitch angle diffusion plays a dominant
           role in the wave-particle interaction.

In addition, many electron-belt effects induced by man-made VLF
ground-based transmitters can be described using the theoretical
model of wave-particle interaction. For example, Horne {\it et
al.} have studied the mechanism behind the wave-induced electron
acceleration in the outer radiation belt\cite{Horne2005}. Those
researchers have shown that the electrons can be accelerated by EM
waves at frequencies of a few kHz, which can also increase the
electron flux by more than three orders of magnitude over an
observation timescale of 1--2 d.

However, all the previous analyses of the NWC-transmitter-induced
particle precipitation have focused on particles with energies
above 100 keV only. In this paper, we present a more comprehensive
survey of energetic particles for a wider energy spectrum,
including particles with energies below 100 keV. And then we
simulate the wave-particle interaction process for NWC-induced
electron precipitation using quasi-linear diffusion theory, which
considers the $\alpha$ scattering and energy diffusion for
different $L$ values. We compare the simulation
results to the observations from the DEMETER and NOAA satellites.
Finally, we discuss the
limitations of the theory.

\section{Observation}
The NWC ground station is located in the northwest corner of Australia with geographical coordinates of $(21.82^{\circ}S$, $114.15^{\circ}E)$, and geomagnetic coordinates of $(-31.96^{\circ}$, $186.4^{\circ})$, which emits electromagnetic wave with frequency 19.8 kHz, a very narrow bandwidth and a large emission power of 1 MW\cite{Li2012}.

The DEMETER satellite was launched in June 2004 and is a low-altitude
    satellite with onboard detectors to measure local electric and magnetic
     fields and energetic particle populations\cite{Parrot2006,Sauvaud2006}. This satellite,
     having a quasi-Sun-synchronous orbit, travels downward (from north to south)
     during local daytime and upward (from south to north) during local nighttime.
      The orbital period is 102.86 min.

Data on the NWC-induced electron belts have been obtained using
DEMETER and analyzed\cite{Li2012}. These data indicate the
presence of obvious wisp structures, which correspond to a
spectrogram of NWC electrons distributed in five different
$L$-value regions (see Fig. 10 in Ref. [9] for details). Thus, it
has been confirmed that the electron precipitation belts are
caused by EM waves emitted from the NWC transmitter. The $L$
values for the NWC electron belts range from 1.5 to 2.2. The local pitch angle
$\alpha$ for the NWC electron belts measured by the DEMETER
detector is approximately $60$--$110^{\circ}$, which corresponds
to an equatorial pitch angle $\alpha_{eq}$ of $23.5$--$25^{\circ}$
at a latitude of $37^{\circ}$ in the southern hemisphere.

The NOAA satellites are positioned in a polar orbit (inclination
angle: $~99^{\circ}$) at altitudes of 807--854 km. The constituent
particle detectors (Space Environment Monitor; SEM-2), which
monitor the proton and electron fluxes at the satellite altitudes,
consist of total energy detectors (TEDs) and medium energy proton
and electron detector (MEPEDs). An MEPED is composed of eight
solid-state detectors.

In addition to the wisp structure of the NWC-induced electron
precipitation observed by the DEMETER satellite, we have
investigated the observed data for the inner-radiation-belt
electrons using data recorded in 2007 by NOAA satellites.
Following the approach described in Ref.\cite{Gamble2008}, we also
present NWC-induced electron belts obtained from NOAA data in
Fig.\ref{1}. This image shows the significant distributions of the
$30$--$100$- and $100$--$300$-keV electron counts for the
geographic position of the subsatellite point, for signals
obtained in the operating period of 1 January to 31 May 2007. The
background obtained during the non-operational period of 1 August
to 31 December 2007 has been subtracted from these signal data. The
ratios of the subtraction and background electron counts are also
shown in the figure.

Note that waves from the NWC propagate through the ionosphere
primarily at night\cite{Starks2008}. Thus, we combined all the
16-s electron integral flux observations provided by the NOAA
National Geophysical Data Center by summing the observation data
obtained by the NOAA 15,16, 17, and 18 POES at night
(2200--0600UT).

\begin{figure}
\centering
\includegraphics[width=38pc]{NWC-elec-NOAA-standard.eps}
  \caption{\small Effects of NWC transmission for
  $30$--$100$ and $100$--$300$-keV electron observation data from NOAA satellites.
  (top) Electron counts for 1 January to 31 May 2007 with those for 1 August to 31 December 2007 subtracted.
   The data in each period are the sum of all $30$--$100$- or $100$--$300$-keV electron counts
   from the medium energy proton and electron detectors (MEPEDs) in the $90^{\circ}$ telescopes
    for the given periods. (bottom) Ratio of subtracted data shown above to background electron counts
     for 1 August to 31 December 2007. The NWC was operating normally from 1 January to 31 May 2007. }
  \label{1}
 \end{figure}

Different to Ref.\cite{Gamble2008}, we exhibit the NWC electron
belts in the lower-energy region ($30$--$100$ keV) in the left two
plots of Fig.\ref{1}. These images indicate that the NWC transmitter
induces not only electrons of $>100$ keV, but also those with
energy $<100$ keV. Note that this is the first time that
NWC-induced electron precipitation belts in the lower-energy range
of $30$--$100$ keV have been reported. In Fig.\ref{2}, we also
present the effect of NWC transmission projected into the L-shell
for electron observations in the two energy ranges of $30$--$100$
and $100$--$300$ keV, based on data from the NOAA satellites. The
L-shell values are directly linked to the dynamic mechanism of the
wave-particle interaction, and the L-shell distribution of the NWC
electrons demonstrates that the $30$--$100$-keV electrons are most
likely induced by the NWC transmission in the $1.8$--$2.0$
L-shell, whereas the $100$-$300$-keV electrons are at
$1.7$--$1.9$. This result indicates that lower-energy electrons
can be influenced by NWC EM waves in higher L-shells in the
ionosphere. In addition, Fig.\ref{2} also indicates that the the NWC
electrons drift eastward above the Earth's surface, in accordance
with the basic three-motion theory for charged particles in the
ionosphere, where those motions are gyration, bounce, and drift.
Furthermore, the $30$--$100$- and $100$--$300$-keV NWC electrons
drift from $110^{\circ}$--$160^{\circ}$ and
$110^{\circ}$--$240^{\circ}$ longitude, respectively. This
behavior is likely caused by the different electron velocities.
Note that, the higher the electron velocity, the farther eastward
in the ionosphere the electrons can travel.

\begin{figure}
\centering
\includegraphics[width=38pc]{noaa-distribution-L-standard.eps}
  \caption{\small Effect of NWC transmission projected in L-shell
  as indicated by $30$--$100$- and $100$--$300$-keV electron observations from NOAA satellites.
   (top) Electrons for 1 January to 31 May 2007, with those for 1 August to 31 December 2007 subtracted.
    The data in each period are the sum of all $30$--$100$- or $100$--$300$-keV electron counts
     from the $90^{\circ}$ MEPEDs for the given periods. (bottom) Ratio of subtracted data shown
      above to background for 1 August to 31 December 2007. The NWC was operating normally
       from 1 January to 31 May 2007. }
  \label{2}
 \end{figure}

Examples of NWC wisp structures observed by the DEMETER satellite
are exhibited in Fig.\ref{3}, which displays various NWC electron precipitation belts
 obtained during NWC transmitter operation.
  Note that the background data when the NWC transmitter was deactivated
   are subtracted from these results.

\begin{figure}
\centering
\includegraphics[width=38pc]{six_NL4_page44_48_50_51_53_57.eps}
  \caption{\small Examples of NWC electron precipitation wisp structures
  after background effect is extracted from signal data obtained from IDP on board the DEMETER satellite. Six examples of absolute flux measurements
    are given in units of electrons  cm$^{-2}$s$^{-1}$sr$^{-1}$keV$^{-1}$ during wisp events.
     The signal is adopted from data recorded in April 2007, when the NWC transmitter was operating,
      whereas the background data were obtained in July 2007, when the NWC transmitter was deactivated.
  For example, the first plot is the effect of the signal data in the NWC electron precipitation
   area on April 14th. Thus, the background data recorded in the same area on July 14th have been subtracted. }
  \label{3}
 \end{figure}

\section{Verification of Quasi-linear Diffusion Equation in Wave-Particle Interaction Theory}

\subsection{Quasi-linear Models}
Originating from the Fokker-Planck equation, the quasi-linear
diffusion equation has been developed as a practical and
convenient form\cite{Schulz1974,Tao2008,Subbotin2009,Shprits2009b,Su2010}. Similar to
the dipole field case, the diffusion equation used in this paper,
 which includes both pitch angle and momentum diffusion, is expressed as

\begin{eqnarray}
\frac{\partial f}{\partial t}&=&
\frac{1}{T(\alpha)}\frac{\partial}{\partial\alpha}[T(\alpha)(<D_{\alpha\alpha}>\frac{\partial
f}{\partial\alpha}+<D_{\alpha p}>\frac{\partial f}{\partial p})]
\\
&&+\frac{1}{p^2}\frac{\partial}{\partial
p}[p^2(<D_{p\alpha}>\frac{\partial
f}{\partial\alpha}+<D_{pp}>\frac{\partial f}{\partial p})]-\frac{f}{\tau},
\end{eqnarray}
where
\begin{equation}
T(\alpha)=S(\alpha)\sin2\alpha.
\end{equation}
Here, $S(\alpha)$ is a function corresponding to the bounce
frequency obtained from the bounce-averaged performance, which is
estimated in a dipole field\cite{Lenchek1961} such that
\begin{equation}
S(\alpha)=1.38-0.32(\sin\alpha+\sqrt{\sin\alpha}).
\end{equation}
$\tau$ is the electron lifetime, which is generally set to be a quarter of the bouncing time in the
loss cone and $f/\tau$ is infinite outside the loss cone.
The $<D_{\alpha\alpha}>$, $<D_{pp}>$, and $<D_{p\alpha}>$ terms correspond to the bounce-averaged
 diffusion coefficients for the pitch angle diffusion, momentum diffusion, and their mixed term, respectively,
  having the following detailed formulae:

\begin{equation}
<D_{\alpha\alpha}>=\frac{1}{S(\alpha_{eq})}\int^{\lambda_m}_{0}d\lambda
D_{\alpha\alpha}\frac{\cos\alpha}{\cos^2\alpha_{eq}}\cos^7\lambda,
\end{equation}

\begin{equation}
<D_{\alpha
p}>=\frac{1}{S(\alpha_{eq})}\int^{\lambda_m}_{0}d\lambda D_{\alpha
p}\frac{(1+3\sin^2\lambda)^{\frac{1}{4}}}{\cos\alpha_{eq}}\cos^4\lambda,
\end{equation}

\begin{equation}
<D_{pp}>=\frac{1}{S(\alpha_{eq})}\int^{\lambda_m}_{0}d\lambda
D_{pp}\frac{(1+3\sin^2\lambda)^{\frac{1}{2}}}{\cos\alpha}\cos\lambda,
\end{equation}
where $\lambda_m$ denotes the latitude of the bounced-particle mirror point.
 Therefore, the phase space density is regarded as a function of equatorial pitch angle $\alpha_{eq}$, the kinetic energy $E$,
   and the L-shell with the expression $f(\alpha_{eq},E,L)$.

 The wave-frequency spectrum density is assumed to obey a Gaussian distribution. Assuming the field-aligned electromagnetic wave, the closed analytical form of the local pitch-angle diffusion coefficient of the wave-particle interaction is derived as follows (see Ref.\cite{Summers2005}, Eqs. (33)--(35)):
\begin{eqnarray}
D_{\alpha\alpha} & =&
\frac{\pi}{2}\frac{1}{\nu}\frac{\Omega^2_{\sigma}}{|\Omega_e|}\frac{1}{(E+1)^2}\sum_s\sum_j\frac{R(1-\frac{x\cos\alpha}{y\beta})^2|F(x,y)|}{\delta
x|\beta \cos\alpha-F(x,y)|} \nonumber\\
&& \cdot  e^{-(\frac{x-x_m}{\delta x})^2},
\end{eqnarray}
\begin{eqnarray}
\frac{D_{\alpha p}}{p} & =&
\frac{\pi}{2}\frac{1}{\nu}\frac{\Omega^2_{\sigma}}{|\Omega_e|}\frac{\sin\alpha}{\beta(E+1)^2}\sum_s\sum_j\frac{R(\frac{x}{y})(1-\frac{x\cos\alpha}{y\beta})|F(x,y)|}{\delta
x|\beta \cos\alpha-F(x,y)|} \nonumber\\
&& \cdot  e^{-(\frac{x-x_m}{\delta x})^2},
\end{eqnarray}
\begin{eqnarray}
\frac{D_{pp}}{p^2} & =&
\frac{\pi}{2}\frac{1}{\nu}\frac{\Omega^2_{\sigma}}{|\Omega_e|}\frac{\sin^2\alpha}{\beta^2(E+1)^2}\sum_s\sum_j\frac{R(\frac{x}{y})^2|F(x,y)|}{\delta
x|\beta \cos\alpha-F(x,y)|} \nonumber\\
&& \cdot  e^{-(\frac{x-x_m}{\delta x})^2},
\end{eqnarray}
where $E$ is the dimensionless particle kinetic energy given by
$E=E_k/(m_{\sigma}c^2)=\gamma-1$,
$\beta=\nu/c=[E(E+2)]^{1/2}/(E+1)$, $R=|\delta B_s|^2/B^2_{0}$ is the ratio of the energy density of the turbulent magnetic field to that of the background field, and $B_0$ is the Earth's magnetic field. Further, $x_m=\omega_m/|\Omega_e|$, $\delta x=\delta
\omega/|\Omega_e|$, and $s=1$ for the R-mode wave, while $s=-1$ for the L-mode wave. $j=1,2,\cdots,N $ is the root number satisfying the resonance
condition. We have
\begin{equation}
\omega_j-\nu \cos\alpha
k_j=-s\frac{q}{|q|}\frac{|\Omega_{\sigma}|}{\gamma}.
\end{equation}
$F(x,y)=dx/dy$ ($x=\omega/|\Omega_e|, y=ck_i/|\Omega_e|$) is
determined from the dispersion equation of the electrons or protons as
follows:
\begin{equation}
(\frac{ck}{\omega})^2=1-\frac{(1+\epsilon)/\alpha^{\ast}}{(\omega/|\Omega_e|-s)(\omega/|\Omega_e|+s\epsilon)},
\end{equation}
where
\begin{equation}
\alpha^{\ast}=\Omega^2_e/\omega^2_{pe},
\end{equation}
is an important cold-plasma parameter; $\epsilon$ is the rest mass
ratio of an electron and proton; $|\Omega_e|=e|B|/(m_ec)$ denotes
the electron gyrofrequency, and $\omega_{pe}=(4\pi
N e^2/m_e)^{1/2}$ is the plasma frequency, where $N$ denotes
the particle number density in the ionosphere and is determined by formula $N=N_0 \times (2/L)^4 cm^{-3}$,
        according to Refs.\cite{Angerami1964,Inan1984}.
\subsection{Numerical Method, Initial and Boundary Conditions}

We solve the bounce-averaged Fokker-Planck equation numerically on ($\alpha_{eq}$, $p$) plane at different $L$.
The domain of our simulation corresponds to $[0, \frac{\pi}{2}]$ in $\alpha_{eq}$, $[0~\text{MeV}, 1.5~\text{MeV}]$ in $E_{k}$, and $[1, 3]$ in $L$.
The grid points are chosen to be $200 \times 200 \times 100$ for equaiorial pitch angle, momentum, and $L$-shell, respectively.
And these grid points are distributed uniformly in our simulation domain.
Our time step in this simulation is 100~s.

Since mixed partial derivatives appear in our diffusion equation, we choose fully implicit finite difference
 method to keep our simulation stable (similar to \cite{Subbotin2009}).
Schematically, our equation takes the form
\begin{equation}
    \frac{\partial f}{\partial t} = \boldsymbol{F} f
\end{equation}
where $\boldsymbol{F}$ represents the differential operator on the right-hand-side.
The implicit finite difference method can be written as
\begin{equation}
    \frac{f^{n + 1} - f^{n}}{\Delta t} = \boldsymbol{F} f^{n + 1}
\end{equation}
where $n$ is the time index.
By solving the linear equation
\begin{equation}
    (\boldsymbol{I} - \Delta t \boldsymbol{F}) f^{n + 1} = f^{n}
\end{equation}
at each step, we can obtain numerical solution of $f$ at arbitrary time.
To reduce solving time at each step, we apply LU decomposition to the discretized equation before simulation starts.

In order to resolve the wave particle interaction equations with mixed derivative term, many numerical simulation methods are introduced (\cite{tHout2010,Su2010}). Here our simulation time is only several hours, with the time step 100 s, so a conventional fully implicit finite difference method is enough in this work.

In the numerical simulation of the quasi-linear diffusion to the NWC electron belts, the initial diffusion function $f_{0}$ satisfies the empirical formula
\begin{equation}
f_0=\sin\alpha_{eq}\cdot e^{-\frac{E-0.1}{0.2}}
\end{equation}

In our simulation, we apply Dirichlet boundary condition at $E_{k} = 0~\text{MeV}$,
and Neumann boundary condition on other boundaries.
For $\alpha_{eq}$
\begin{equation}
    \left. \frac{\partial f}{\partial \alpha_{eq}} \right|_{\alpha_{eq} = 0} = 0 ,
    \qquad
    \left. \frac{\partial f}{\partial \alpha_{eq}} \right|_{\alpha_{eq} = \frac{\pi}{2}} = 0
\end{equation}
and for $E_{k}$
\begin{equation}
    \left. f \right|_{E_{k} = 0~\text{MeV}} = \left. f_{0} \right|_{E_{k} = 0~\text{MeV}} ,
    \qquad
    \left. \frac{\partial f}{\partial E_{k}} \right|_{E_{k} = 1.5~\text{MeV}} = 0
\end{equation}

\subsection{Simulation Results}
In order to simulate the NWC electron belts induced by whistler
waves in the ionosphere, the following parameters are chosen for use
 in the quasi-linear wave-particle coupling model: a Gaussian wave
  spectrum center frequency $\omega/(2\pi)=19.8$ kHz; a wave amplitude $\delta b= 200$ pT,
   which is consistent with the calculated result obtained via the NWC EM wave
    propagation described by full-wave model analysis \cite{Lehtinen2009,Zhao2015}, a semi-bandwidth of 500 Hz,
    which is approximately consistent with the observed values obtained from the electric-field
     instruments on board the DEMETER satellite, and an equatorial magnetic field
      $B=3.11\times 10^{-5}/L^3 $ T, which is determined by a dipole model.

We still consider the effect of the bounce loss cone and
drift loss cone in the
numerical simulation on the NWC electron precipitation belts.
 The bounce loss cone $LC_{bounce}$ depends on the L-shell
according to the expression
\begin{equation}
LC_{bounce}=\arcsin{\sqrt{\frac{(\frac{6470}{6370L})^3}{\sqrt{4-3(\frac{6470}{6370L})}}}}.
\end{equation}
In theory, drift loss cone $LC_{drift}$ varies with longitude; however, it is actually affected by many factors, such as the season or certain magnetic storms. In the local area above the NWC transmitter position, we will exhibit the effect of $LC_{drift}$ value at approximately $5^{\circ}$, $10^{\circ}$ and $15^{\circ}$, respectively. The electron lifetime $\tau$ is generally set to be a quarter of the bouncing time in the loss cone and infinite outside the loss cone. But in inner radiation belt, the bounce loss cone is larger and the observed electrons by satellite come from precipitated electrons in loss cone. $\tau$ with too small value will induce too weak effect of electron precipitation in certain time. So here we set $\tau$ value to be 60 s.

  The bounce-averaged Diffusion coefficients are exhibited in Fig.\ref{4}. We can see that
  the pitch angle diffusion is dominant and larger by about two orders of magnitude than momentum and mixed diffusion terms. And pitch angle diffusion for electrons in L = 1.4 -- 2.0 plays a strongest role in energy range of 0.05 -- 0.25 MeV.

Following the above numerical simulation method in section 3.2,
simulated results for 4-h evolution were obtained and are
presented in Fig.\ref{5}. These results indicate the relatively good
agreement with the satellite observation for the electron flux
distribution, which is shown as a function of energy and L-shell (see Fig.\ref{3}).
Identical parameters to those listed above were used in the
simulation. Eqs. (1) and (2) were solved in the radial distance
range from 1--3 earth radii ($R_E$) and for equatorial pitch angle
$\alpha_{eq}$ = 0 -- $\pi/2$. The energy range does not vary
with radial distance and was set to 0.05--1 MeV. As in the inner
radiation belt, the radial diffusion scattering plays a small role
in the total particle diffusion behavior. Note that all the plots
in this figure correspond to $\alpha_{eq} = 17$--$25^{\circ}$
(that is 0.3 to 0.44 radian), which is consistent with detection
range of the DEMETER satellite\cite{Li2012}. In the results shown
in Fig.\ref{5}, the particle distribution depends on the
$\sin\alpha_{eq}$; this is similar to the flat distribution inside
the loss cone adopted in Ref.\cite{Kennel1969}. We still
consider both the bounce and drift loss cone effects with $LC_{drift}$ set to be:
(a) $5^{\circ}$, (b) $10^{\circ}$, and (c) $15^{\circ}$.  The bounce loss cone is
determined by Eq. (14). From Figure 4, it can be seen that electron
precipitation also takes place for the ~50--100-keV range at higher L shell; this
result is in agreement with the observations of the NOAA
satellites.

\begin{figure}
\centering
\includegraphics[width=38pc]{D1-Dlc10-N3000-fw500.eps}
  \caption{\small Diffusion coefficient distributions with parameters: wave frequency $\omega/(2\pi)=19.8$ kHz, wave amplitude $\delta b=200$ pT, semiband width 500 Hz, and $N_0=3000$ counts/s. L-shell  in (a) (b) (c): L = 1.4--2.0, L-shell in (d) (e) (f): L= 2. Five colorful lines denotes the diffusion coefficient for electrons with 50 keV, 100 keV, 200 keV, 500 keV and 800 keV. }
  \label{4}
 \end{figure}

\begin{figure}
\centering
\includegraphics[width=38pc]{Flux2dim-Dlc5-10-15-N1000-fw500.eps}
  \caption{\small Simulated NWC electron precipitation structures
  after subtraction of initial flux distribution from final flux distribution.
   Parameters used in simulation: frequency $\omega/(2\pi)=19.8$ kHz; wave amplitude $\delta b=200$ pT; semiband width 500 Hz;
   and $N_0=1000$ counts/s. The equatorial pitch angles $\alpha_{eq}$
    used in the simulation ranged from 0.3 to 0.44, corresponding to the observation range by the DEMETER and NOAA satellites.
      The loss cones were set to:
   $LC_{drift} =$ (a) $5^{\circ}$; (b) $10^{\circ}$; (c) $15^{\circ}$, all of which were with a bounce loss cone. }
  \label{5}
 \end{figure}

Fig.\ref{6} is the flux distribution of initial( black ) and final ( red ) states during wave particle interaction, corresponding to electrons with energy 0.05--0.6 MeV and L shell value 1.4--2.0. We can see that the satellite-observed electrons locate inside of loss cone when the electrons are scattered into loss cone mainly by pitch angle diffusion mechanism.

\begin{figure}
\centering
\includegraphics[width=22pc]{Flux-Dlc10-N3000-fw500.eps}
  \caption{\small Flux distribution of initial and final states during wave particle interaction, corresponding to electrons with energy 0.05 -- 0.6 MeV and L shell value 1.4--2.0. Other parameter values: wave frequency $\omega/(2\pi)=19.8$ kHz, wave amplitude $\delta b = 200$ pT, semiband width 500 Hz, and $N_0=3000$ counts/s. The DEMETER and NOAA satellite observation ranges from 0.3 to 0.44 radian. }
  \label{6}
 \end{figure}

Fig.\ref{7} is the simulated NWC electron precipitation for different equatorial pitch angle $\alpha_{eq}$ values of $0.1$--$0.2$, $0.2$--$0.3$, $0.3$--$0.4$, $0.4$--$0.5$, and $0.5$--$0.6$ radian. It is apparent that the electron precipitation induced by the wave-particle interaction differs in different $\alpha_{eq}$ ranges. The simulation result obtained for an $\alpha_{eq}$ of $0.3$--$0.4$ is located inside the IDP observation range on board the DEMETER satellite. Note that, at a higher $\alpha_{eq}$ range, it is easier for higher energy electrons to interact with VLF waves in the ionosphere. However, due to the pitch angle observation limitations of high-energy particle detectors and the lower density distribution of higher-energy electrons in space, it is possible that the electron precipitation induced by VLF waves is not observed by satellites to some extent.

\begin{figure}
\centering
\includegraphics[width=40pc]{Flux2dim-diffPitchangle.eps}
  \caption{\small Simulated electron precipitation structures after subtracting initial flux distribution
   from final flux distribution. Simulation parameters: Electromagnetic wave
  frequency $\omega/(2\pi)=19.8$ kHz; wave amplitude $\delta b=200$ pT; semi-band width 500 Hz;
  $N_0=1000$ counts/s; and equatorial pitch angles $\alpha_{eq} =$ 0.1--0.6 radian. }
  \label{7}
 \end{figure}

\section{Asymmetric Distribution of the NWC Electric Field}
The NWC electric field power distribution for the entirety of
January 2007, as detected by the DEMETER satellite,
is shown in Fig.\ref{9}. This figure shows that, at the altitude of
the DEMETER satellite orbit, the L-shell of the NWC electric-field
power covers $1.3$--$1.5$ and $1.5$--$1.8$ in the southern and northern
hemispheres, respectively. This phenomenon of asymmetrical
distribution of the NWC electric field in space is obvious.

\begin{figure}
\centering
\includegraphics[width=40pc]{NWC-ICE.eps}
  \caption{\small NWC electric-field power distributions measured
 by DEMETER satellite in January 2007. }
  \label{9}
 \end{figure}

In order to explain this phenomenon, we use ray tracing model in a cold plasma in dipole magnetic field\cite{Horne1989,Chen2009, Chen2013,Xiao2007}, to simulate the NWC wave propagation path in magnetosphere.
Electromagnetic waves with 19.8 kHz are launched at L=1.35 close to NWC site on southern hemisphere, over a cone of 5 degree with respect to the vertical direction of earth's surface. The launch position is at geographic coordinate ($21.82^o$ S, $114.15^o$ E) and geomagnetic coordinate ($-31.96^o$, $186.4^o$).
Fig.\ref{10} shows the simulated ray propagation pathes. We can see that the L-shell values of NWC waves on north hemisphere at the conjugate latitude is higher. This asymmetry nature of NWC wave in southern and northern hemispheres is caused by the refraction effect of wave propagation in the inhomogeneous magnetosphere.

\begin{figure}
\centering
\includegraphics[width=22pc]{raytracing.eps}
  \caption{\small Simulated NWC transmission path by ray tracing model. Electromagnetic wave with 19.8 kHz is launched over a transmission cone of 5 deg with respect to vertical direction. }
  \label{10}
 \end{figure}

\section{Discussion and Summary}

In this work, in addition to the previously reported electron precipitation with 100--600-keV energy
 detected by the DEMETER satellite, we have still reported enhancement of the 30--100-keV electron flux
  observed by the NOAA satellites at night, when the powerful NWC VLF transmitter is broadcasting.
   We then performed a validity check using a theoretical model, i.e., the quasi-linear diffusion equation,
    and demonstrated approximate agreement with the satellite observation results.

Many factors influence the simulation results obtained using the quasi-linear diffusion equation,
 including the adopted wave semi-bandwidth, electron density. In Fig.\ref{8}, we show the simulated electron precipitation
  structure obtained for wave semi-bandwidths of 300, 500 and 1000 Hz and different electron densities. It is apparent
   that the simulated wisp structure is wider for a greater wave width. The simulated wisp structure moves toward to the lower L value with the increasing electron density. Thus,
   the parameter uncertainty, including loss cone, wave width and electron density, may consist of the factors which cause the difference of simulated result with the real wisp shapes observed via satellite.

\begin{figure}
\centering
\includegraphics[width=40pc]{Flux2dim-Dlc10-1.eps}
  \caption{\small Simulated electron precipitation structures after subtracting initial flux distribution
  from final flux distribution. Simulation parameters: Electromagnetic wave
  frequency $\omega/(2\pi)=19.8$ kHz; wave amplitude $\delta b=200$ pT.
    The equatorial pitch angles $\alpha_{eq}$ range from 0.3 to 0.44, which is consistent with the DEMETER observation. }
  \label{8}
 \end{figure}

Thus, these results indicate that the quasi-linear wave particle interaction model can describe
 an NWC electron precipitation wisp structure approximately, and can also explain the coupling
  characteristics of wave-particle interaction in a general sense. In particular,
   below the 0.1-MeV electron energy, the theoretical simulation results demonstrate
    agreement with the NOAA satellite observations shown in Fig.\ref{2}.

Electron precipitation or accumulation in the ionosphere may also be
caused by both energy diffusion and radial diffusion in the
L-shell\cite{Falthammar1965,Su2015}. However, in the inner
 radiation belt, the effect of radial diffusion on the L-shell can be omitted, especially
  at the satellite altitudes of hundreds of kilometers. The radial diffusion plays a large role in the wave-particle interaction only in the outer radiation belt \cite{Su2011}. In addition, when the theoretical simulation time is sufficiently long, e.g., having a duration of
   approximately 1 yr\cite{Selesnick2013}, the radial diffusion in the L-shell evolution
 must be considered in the wave-particle interaction analysis in the inner radiation belt.
 Thus, significant attention is not paid to the effect of
    radial diffusion on the NWC electron belts in the analysis of the wave-particle interaction
    simulation conducted in this study.

However, we must note that the quasi-linear theory is thought to
describe interactions between charged particles and
small-amplitude broadband waves\cite{Kennel1966}. When the wave
amplitude increases or the band becomes narrower, nonlinear
effects such as phase trapping and bunching are more likely to
become dominant, calling the use of quasi-linear theory into
question\cite{Bortnik2008}. Inan {\it et al.} have studied the
nonlinear pitch angle scattering of energetic electrons by
coherent VLF waves in the magnetosphere and compared their
observations with linear theory\cite{Inan1978}. They have also
defined a quantity $\rho$, the ratio of the maximum absolute
values of the wave and inhomogeneity terms, so as to differentiate
between the linear and nonlinear interactions. Furthermore, Tao
{\it et al.} have reported that the nonlinear interactions may be
important near the equatorial plane, even for a moderate wave
amplitude, and have shown that phase trapping is likely to occur
when the wave-induced motion dominates the adiabatic
motion\cite{Tao2010}. Those researchers subsequently used a
test-particle code to confirm that the effect of the amplitude
modulations should be considered in the quantitative treatment of
nonlinear interactions between electrons and chorus
waves\cite{Tao2012,Tao2013}. There are other related works about
dynamics of high-energy electrons interacting with whistler mode
chorus emissions studied by test particle
simulations\cite{Hikishima2009,Omura2006}. Su {\it et al.} pointed
out that the nonlinear physical processes, including boundary
reflection effect, phase bunching and phase trapping, start to
occur as the amplitude increases by studying the interaction
between electrons and parallel-propogating monochromatic EMIC
waves\cite{Su2012}. And then he further presented that the
nonlinear processes depend on the electron initial latitude and
decrease or increase the loss rate predicted by the quasi-linear
theory\cite{Su2013}.
In addition, the azimuthal advection may play an important role in the radiation belt electron dynamics\cite{Su2010}, in the next work, we'll study this effect and attempt to incorporate it in theory model for research of ground-based induced electron precipitation belts.

Therefore, in our next work, we will attempt to adopt a non-linear
theory model to further study this wave-particle interaction
event, focusing on the quantitative calculation.

Also considering the real NWC electric-field power distributions in the L-shell for the south and north hemispheres observed by the DEMETER satellite, shown in Fig.\ref{9}, the wave-particle interaction is simulated numerically
    using the quasi-linear diffusion equations described above. The simulation results are shown in Fig.\ref{11}.

\begin{figure}
\centering
\includegraphics[width=22pc]{Flux-Dl10-N1000-fw500-PowerChangeWithL.eps}
  \caption{\small Simulated NWC electron precipitation structure
  following subtraction of initial flux distribution from final flux distribution.
   The NWC electric-field power distributions in the L-shell in the south
    and north hemispheres are considered in the simulation process.
     Simulation parameters: Electromagnetic wave frequency $\omega/(2\pi)=19.8$ kHz;
      wave amplitude $\delta b=200$ pT; semi-bandwidth 500 Hz; $N_0=1000$ counts/s.
       The equatorial pitch angles $\alpha$ used in the simulations range from 0.3 to 0.4,
        which is consistent with the value of the NWC electron precipitation wisp structures
         observed by the DEMETER and NOAA satellites. The bounce loss cone and $LC_{drift} = 5^{\circ}$
          are set in the simulation. }
  \label{11}
 \end{figure}

From the simulation results shown in Fig.\ref{8}, the distribution trend of the NWC electron
 precipitation in the L-shell and the energy dimensions remain consistent with the observed
  wisp structure, although the simulated result is less accurate. This deviation
   from the observation results may be caused by a number of factors,
   including the influence of the wave bandwidth and cold plasma density.
 Additionally, the wave propagation effect in the ionosphere must be further studied in the next research stage.
  A comprehensive theoretical model that incorporates the wave propagation effect (such as the ray tracing model)
   and wave-particle interaction will facilitate a more complete and accurate approach to describing
    the electron precipitation in the radiation belt induced by the ground-based NWC transmitter.

In addition, we believe that analysis of the effects of the NWC
VLF wave propagation and electron precipitation, along with
development of a comprehensive theoretical model, will facilitate
the study of ground-based waves propagating into the ionosphere
and interacting with high-energy particles in radiation belts.
Based on wave particle interaction theory, investigation of the EM disturbance in the ionosphere induced by
seismic electromagnetic signals will be particularly useful, supposing that it is possible for seismic electromagnetic
 signals to propagate into ionosphere. As regarding to the influence of the EM waves emitted
by seismic activities in wider space, a large number of works have
also been published on this topic, including studies based on
satellite observation\cite{Zhang2012} and theoretical
exploration research\cite{Zhang2014a,Zhang2014b}.

\vspace*{2mm}

\section{Acknowledgement}
The authors are grateful to Tao Xin, Zong Qiugang, Wang Yongfu for useful discussions.

redpajama_set_name: RedPajamaArXiv


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About Rachel Remen M.D.
Rachel Naomi Remen, M.D., is Clinical Professor of Family and Community Medicine at UCSF School of Medicine and Founder and Director of the Institute for the Study of Health and Illness at Commonweal. She is one of the best-known of the early pioneers of Holistic and Integrative Medicine. As a medical educator, therapist, and teacher, Rachel has enabled many thousands of physicians and other health professionals to work from the heart, and thousands of patients to remember their power to heal. Her groundbreaking curriculum for medical students, The Healer's Art, is taught in ninety of America's medical schools and medical schools in seven countries abroad. This master storyteller and observer of life has published two bestselling books, Kitchen Table Wisdom and My Grandfather's Blessings, which have sold more than a million copies and are translated into twenty-three languages. Rachel has had Crohn's disease for more than sixty years, and her work is a unique blend of the wisdom, strength, and experience of both doctor and patient.
Kitchen Table Wisdom: Stories that Heal
"I recommend this book highly to everyone."… Deepak Chopra, M.D.
The The New York Times bestseller addresses the spiritual issues that make cancer survivors ponder: suffering, meaning, love, faith, and miracles.
"Despite the awesome powers of technology, many of us still do not live very well," says Dr. Rachel Remen. "We may need to listen to one another's stories again." Dr. Remen, whose unique perspective on healing comes from her background as a physician, a professor of medicine, a therapist, and a long-term survivor of chronic illness, invites us to listen from the soul.
My Grandfather's Blessings: Stories of Strength, Refuge, and Belonging
Rachel Naomi Remen, a cancer physician and master storyteller, uses her luminous stories to remind us of the power of our kindness and the joy of being alive.
Dr. Remen's grandfather, an orthodox rabbi and scholar of the Kabbalah, saw life as a web of connection and knew that everyone belonged to him and that he belonged to everyone. He taught her that blessing one another is what fills our emptiness, heals our loneliness, and connects us more deeply to life.
Life has given us many more blessings than we have allowed ourselves to receive. My Grandfather's Blessings is about how we can recognize and receive our blessings and bless the life in others. Serving others heals us. Through our service, we will discover our own wholeness—and the way to restore hidden wholeness in the world.
The Will to Live and Other Mysteries
"Life is best defined not by science, but by mystery," teaches Dr. Rachel Naomi Remen. The beloved healer of the heart probes the universal experience of the unknown that can come in times of crisis. Join this master storyteller as she shares compelling front-line stories of people who opened to mystery and found healing. Complete with step-by-step exercises that Dr. Remen recommends to her own patients.
Rachel Naomi Remen, M.D.
Remembering the Heart of Medicine
November 17, 2017 Filed Under: Stories of Hope Tagged With: Rachel Remen M.D.


text:
Butelka – polski zespół metalowy pochodzący z Torunia.

Historia

1996-2003
Zespół powstał w 1996 roku, z inicjatywy McButelki, który zaprosił do współpracy kolegów z zespołów Kobranocka (Dr. Frankensteina i Pięknego Lolo) oraz OK'Laski (HipHłop). Pierwsze nagranie – "Potrzebni" – powstało w studiu w Dworze Artusa w Toruniu. Wkrótce Butelka rozpoczęła regularne próby w toruńskiej "Zębowni".

Pierwsza płyta pod prostym tytułem "Butelka" została nagrana w latach 1997-1998 – również w Dworze Artusa. W utworze "10 grudnia" na basie zagrał Klasztor (Kobranocka, Atrakcyjny Kazimierz). W 1999 roku materiał wydała niezależna wytwórnia Black Bottle Records, należąca do McButelki.
Na tym etapie istnienia zespół zagrał kilka znaczących koncertów, m.in. przed Katem i Heyem, a także na festiwalu Rap'n'Roll, na którym spotkał się na scenie z hiphopowymi Kalibrem44 i Wzgórzem Ya-Pa 3.

Z tego okresu pochodzi utwór "To mnie wkurwia", do dziś grany przez Butelkę na koncertach (a rozpoznawalny dzięki popularnemu w internecie teledyskowi).

2003-2007
Zespół w tym składzie został rozwiązany w 2003 roku – jednak już po kilku miesiącach ustabilizował się nowy skład. Do McButelki dołączyli inż.MBL, Martinus (członkowie Deuther X), Kot, Dyboś i Vitusz (grający wówczas w zespole Czaqu). Prace nad kolejną płytą zaczęły się w 2004 roku. W tym czasie od zespołu odeszli Martinus i Dyboś. Nowy album "Radio dla Polaków" (MTJ 2005) charakteryzował się bardziej metalowym brzmieniem od poprzedniego. Zespół w swoich tekstach (autorstwa McButelki) postawił sobie za zadanie obśmiewanie i piętnowanie hipokryzji - także tej występującej w Kościele katolickim, przez co wielu przypięło do zespołu łatkę antyklerykalizmu. Z tej płyty pochodzą m.in. utwory "Radio dla Polaków" (z wsamplowanymi wypowiedziami wprost z anteny Radia Maryja), "LPR" i "CHWD(P)" (poświęcone policji). Do poszczególnych utworów powstawały odważne teledyski, dostępne przede wszystkim w sieci.

W tym czasie Butelka w dalszym ciągu gra wiele koncertów, z których należy wymienić przede wszystkim WOŚP, Festiwal "Hunter Fest" - Szczytno 2005 i 2006 oraz Jarocin 2006 (wyróżnienie Jury). Butelka grała również na pierwszym i drugim koncercie pamięci Grzegorza Ciechowskiego w toruńskiej Od Nowie. Na koncertach grupa szokuje scenicznym imagem - członkowie zespołu noszą sutanny. Stosują też oryginalne dekoracje, efekty pirotechniczne, a wokalista zazwyczaj występuje z kilkoma krzyżami.

W 2007 roku od zespołu odchodzi Vitusz – szybko zastąpiony przez Kviatora (Deathcaller).

2007-2008
W nowym składzie Butelka opracowuje materiał na kolejną płytę "DemonArchia", która ukazuje się nakładem wytwórni MTJ na początku 2008 roku. Największym hitem z tego albumu okazał się "Dekoder TV Trwam", do którego teledysk długo bił rekordy popularności na YouTube. Klipy zrealizowano także do utworów "W imieniu wiary" i "Katolicki tajny współpracownik" (poruszającego temat lustracji w Kościele).
Rok 2008 był dla zespołu rokiem dużej aktywności koncertowej. Butelka zagrała m.in. na festiwalu Gotyk na Dotyk – 2007 i 2008, Park Fest – 2007, Wacken Metal Battle 2007 (II miejsce), MECH DAY 2008, MuszlaFest 2008. Warto odnotować też wspólne koncerty z zespołami Chylińska, KAT z Romanem, TSA, Acid Drinkers, Hunter, Frontside, Totem, Chainsaw, Rootwater, Horrorscope, Mech, Killjoy, The NO-Mads, Dragon's Eye, Corruption.
W 2008 roku z Butelki odchodzą inż. MBL, Kot i Kviator.

2008-2010
Nowy skład zaczyna się stabilizować już kolejnego dnia. Do McButelki dołącza Sivy (Chainsaw), Jołek (Doktor C) i Professor Jerry (TrzyCzwarte, All My Life). Pierwszy koncert z nowymi muzykami odbywa się na toruńskim finale WOŚP 2009. Wkrótce nastąpują kolejne zmiany personalne i miejsce Professora Jerry'ego zajmuje Gorzky, a za bębnami zasiada Padre zastępując Sivego. Obecnie zespół pracuje nad kolejną płytą. Nowe utwory, które można już usłyszeć na koncertach – m.in. "Lider nabity w Butelkę" i "Szatan" – zapowiadają kolejny zwrot stylistyczny w historii zespołu.

2010
W marcu 2010 nastąpiła zmiana gitarzysty - Jołasa zastąpił Grisch (ex Enhiridion, Pandemic Genocide). Kolejna zmiana składu nastąpiła w czerwcu 2010 - na miejsce Padre za perkusją usiadł Grzała (ex Crystal Lake). W październiku 2012 została wydana płyta Diabeł z powyłamywanymi rogami.

Muzycy

Obecny skład zespołu
 Grzegorz "McButelka" Kopcewicz - śpiew, keyboard (1996 - obecnie)
 Radosław "Grisch" Irla - gitara (2010 - obecnie)
 Sebastian "Gorzky" Gorzka - gitara basowa (2008 - obecnie)
 Krzysztof "Grzała" Grzelak - perkusja (2010 - obecnie)

Byli członkowie zespołu
 dr Frankenstein - gitara, śpiew (1996 - 2003)
 Piękny Lolo - perkusja, śpiew (1996 - 2003)
 HipHłop - gitara basowa, śpiew (1996 - 1997)
 Klasztor - gitara basowa, śpiew (1997 - 2003)
 Marek "Vitusz" Wituszyński - perkusja (2003 - 2006)
 Martinus - gitara, śpiew (2003 - 2004)
 Michał "Dyboś" Dybowski - keyboard, śpiew (2003 - 2004)
 Paweł "Kot" Kociszewski - gitara basoa, śpiew (2003 - 2008)
 Kviator - perkusja (2006 - 2008)
 Marek "inż. MBL" Sysoł - gitara, śpiew (2003 - 2008)
 Professor Jerry - gitara basowa (2008)
 Sivy - perkusja (2008 - 2009)
 Padre - perkusja (2009 - 2010)
 Jołek - gitara (2008 - 2010)

Dyskografia
 Butelka (1998)
 Radio dla Polaków (2005)
 DemonArchia (2008)
 Diabeł z powyłamywanymi rogami (2012)
 Szpun 'N' Roll (2017)

Zobacz też
 Kultura w Toruniu

Przypisy

Linki zewnętrzne
 Oficjalna strona zespołu

Polskie zespoły heavymetalowe
Muzyka w Toruniu


I shake hands with the reception officer and leave Komotini Prison in northern Greece. After talking for over an hour with a French prisoner and discussing his situation with the prison warden, I must hurry as I have a meeting with the local association of French teachers. Considering that I have had to travel over 400 kilometres from Thessaloniki in half a day, I might as well make the most of this visit : I have already met the regional chief of police to discuss the fight against illegal immigration in a region which is targeted by illegal immigration rings.
Why meet with the French teachers ? Because, in addition to being Consul General, I also head the French Institute of Thessaloniki, an institution that is part of the French Secular Mission (MLF) for which promoting French teaching is a priority. The combination of these two occupations was decided in 2011 as part of the rationalization of our outreach policy.
The meeting with the French teachers takes place in a café where young veiled women are sitting at the tables next to ours : we are in Thrace, where there is a large Muslim community whose rights are guaranteed by the Treaty of Lausanne. An issue to keep a close eye on.
But it's time to be off again. In the car, I check my e-mail as I'm waiting for confirmation of a visit by a delegation from a big French company. I simply can't delay as I'm also giving a talk this evening on the French military presence in northern Greece during the First World War. The Centenary is an opportunity to evoke the little known Eastern Front and a series of events has been scheduled on this theme. I was recently in charge of approving the renovation work on the house of the keeper of the French military necropolis (8,000 graves), which is to house a museum on the Army of the Orient. In liaison with the French Defence Ministry, we are very busy with the significant renovation work started in recent years in the cemetery in order to pay a dignified tribute to those who fell for France.


At this point issue another press release, suggesting you are about to launch, and point users to a form to sign up. You should then announce the number of students (in 100,000s) you have "enrolled). With this statistic in hand, approach investors for another round of funding and then repeat using a higher enrollment number and the amount of money you already have borrowed ("an $x million pound disruptive edtech giant").


text:
The Pride Season Two Review
A superhero book with a difference, forging its own path in a world of repetition.
Zachary Whittaker
The first threat to The Pride is defeated. Where will the heroes go next now that they're in the public eye more than ever before?
With the core of The Pride in place, Wolf rolls out his plan to expand the team with members from around the world to show that The Pride stands for everyone. However, the team's newfound fame will throw a number of obstacles in their path — with regular attacks on a pop star's audience and members of the team suffering personal attacks from the media, will the core team be spread too thin?
Although it may seem obvious, The Pride is a series that excellently examines modern perceptions of gender and sexuality, and every moment is handled fabulously. Every character feels carefully considered, with even the most perfect among heroes shown to make mistakes, and perhaps more importantly working past those mistakes. Aside from the themes you may expect from The Pride, this second season does examine other important real world issues, including identity and body image, which are also approached masterfully. The Pride constantly shows that even the most fantastic of characters have the same human flaws and concerns as everyone else.
The Pride is more than just its themes, though — it's also a great superhero story. There's an immediate comparison to be made with more mainstream superhero teams, which is understandable; any new superhero group will always borrow something from what's come beforehand and while that's true here, I do think The Pride feels noticeably different — a superhero book with a difference, forging its own path in a world of repetition. Every member of the team remains interesting and feels like they bring something different to the team, something that can often get lost within the confines of a team book, and most of all each member feels like more than just a set of ideals.
In a departure from the first installment of The Pride, Season Two features a consistent artist throughout the arc, Cem Iroz. He's not an artist I'm overly familiar with, but through these six issues I've definitely grown to be a fan. In the first issue Iroz gives the members of The Pride a makeover, and I must admit every character looks better than ever. With these strong character designs in place, dramatic action sequences and great attention to detail in the more emotional moments, Cem Iroz brings The Pride to life brilliantly.
Joe Glass has returned to The Pride in triumphant fashion. Where the first volume presented a cast of heroes who work wonders for representation, this continuation moves forward in exactly the way the series needed to, in keeping with the modern world and showing that it's entirely possible for everyone to see themselves within the superhero genre.
The Pride Season Two
The Pride boasts a truly unique cast of characters. It's almost certain you'll see a little something of yourself within the series. This is a series with an unwavering message of equality, celebrating the merits of representation and diversity at every turn.
An excellent continuation of Season One.
Cem Iroz brings great artwork and character designs throughout.
A well-crafted superhero tale with an entirely positive message.
Great variety of characters, that all feel like real individuals.
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