text:
Does the Science of Music Confirm the Clichés?
art-and-science health neuroscience scientific discovery
Humans have been making music since the beginning of time. Although this sounds like a platitude, there is evidence to back this claim.
Consider the 40,000-year-old bone flute that was left in a Central European cave around the dawn of human settlement in Europe. Going back even further, fossils of the Neanderthal's ancestor Homo heidelbergensis show that they had similar vocal physiology to modern humans, so they might have been able to sing. Discover suggests that it's scientifically possible that music has a 500-millennium history.
The science of music can help us better understand how humans are influenced by song, and how music and emotions are intertwined.
Music Can Enhance Intelligence and Creativity
Many studies have demonstrated the benefits of music, but can it really boost your intelligence?
A Harvard study discovered that musicians' brains have more bundles of nerves connecting the left and right hemispheres. A study published on PLOS One found that "musicians learned response sequences more easily than non-musicians as their responses were faster and more accurate."
Listening to music engages practically every part of the brain:
Cochlear nuclei
The brain stem
The cerebellum
Auditory cortices on both sides of the brain
Memory centers of the brain (hippocampus, the lowest parts of the frontal lobe)
Additionally, tapping along with music involves your cerebellum; composing music fires up the visual cortex; and song lyrics utilize the language centers in the temporal and frontal lobes.
Therapeutic Benefits of Music
The science of music makes it an excellent tool for treating neurological conditions such as Parkinson's disease, Alzheimer's disease, stroke, brain injury, anxiety and depression. For example, Parkinson's patients have used music to improve their balance and movement. According to Harvard Health, patients who listened to music in the operating room experienced less pain.
Mic cites several other positive medicinal effects of music, such as a study where listening to Mozart decreased epilepsy in patients, even when the patients were in comas. Music therapy isn't just a new aged holistic approach. Plato suggested using music to treat anxiety, Aristotle considered music a therapeutic tool, and in ancient Greece, Apollo ruled both music and healing.
Music Changes Your Mood
Music and emotions are connected. Different types of melodies and rhythms evoke various emotional responses; even ambient noise can boost creativity, according to Mic. While a slow ballad can give you the chills, a peppy pop song could make you dance.
There are chemical and biological explanations for why music evokes such strong feelings. Mic notes that music increases libido, and listening to music can elevate serotonin levels in a person's body. A French study found that listening to romantic music increased the odds of single women giving out their phone numbers.
Athletes often train with music, and several studies have shown that music can improve endurance and help us use energy more efficiently during exercise. In a 2012 study, cyclists who peddled along to music used 7% less oxygen than the control group, says Mic.
A study published on Scientific Reports details that music can evoke "deeply personal, often unsolicited and emotionally-laden, thoughts and memories." The National Association of Music Merchants (NAAM) Foundation mentions a study that found people who actively engaged with classical music, rather than passively listening to it, had a happier, more emotional response. The NAAM Foundation also cites a study that says people who are more open to experiences "are likely to feel the most chills while listening to music."
We feel music on such a deep emotional level that it's hard to quantify its impact. Ultimately, scientific studies have confirmed that the cliches about music are true. It is the ultimate universal language, with the power to change the way you feel.
From Music to Missile Defense: The Very Interesting Life of Jeff Baxter
Jeff Baxter: Rock 'n' rock guitarist, innovator — counterterrorism expert? The very interesting life of the...
Art Innovates Life: The Brandon Balasbas Story
Northrop Grumman's corporate graffiti artist and aerospace photographer shares his career path story and his inspiration...
Behind the Scenes: Multipurpose Movie Magic
Movie magic: The real-world applications of behind the scenes tech advancements.


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fernando alvarez - chief executive officer
falvarez@siglasul.com.br
Mini-curriculum
With a degree in engineering from the National University of Buenos Aires, with master's degrees in energy economics and administration, Fernando Alvarez is an expert on economic regulation and planning in the electricity and sanitation markets.
Between 1994 and 2002 his professional activities were focused on Argentina and other countries of Latin America where he developed and guided important regulatory assistance projects and business evaluations for major economic groups in the region. Since 2002, as a founding partner and CEO of Siglasul, his professional performance focused on Brazil developing regulatory and institutional studies, and business evaluations for the electricity and sanitation sectors.
leonardo campos - project director
lcampos@siglasul.com.br
Leonardo is an economist graduated (BSc) from the Federal University of Rio de Janeiro. He holds a MSc (1992) and a PhD (1998) in economics from the London School of Economics. Leonardo is an specialist in economic regulation for network utilities.
His professional career started in academia, where he undertook research and teaching activities related to regulation of energy markets. He worked for the ANP (national oil and gas regulator) (1998-2000) and was a Competitive Intelligence Manager in Embratel (a large telecom utility). Between 2002 and 2007, he worked as Associate Consultant in a Rio based energy consulting business (CBIE) where Leonardo was responsible for managing and developing consulting projects related to oil, gas and electricity markets.
Since 2007, he has been working as Manager in Siglasul undertaking projects and developing businesses associated to gas, electricity and water sectors in Brazil. In 2010, Leonardo was appointed Project Director.
sebastián butto - project director
sebabutto@siglasul.com.br
Sebastian graduated as an Economist from the National University of Cordoba, UNC (1997), with a Magister in Finance from the CEMA University (1999). He is a specialist in economic regulation of public services.
He has 12 years of experience advising regulatory agencies, industry associations and large electricity and water utilities (EDF, AES, EDP, SABESP) on issues related to economic regulation, defining business strategies, evaluation of investment projects, benchmarking studies, analysis of EVA, Research & Development (R&D) projects, and written experts reports on technical, tariff and regulatory matters. He has participated in more than 20 tariff review processes in Latin America countries (Brazil, Argentina, Panama, Guatemala, Bolivia and Peru). Previously, he was a trainee in the Regional Energy Integration Commission, CIER (1999) and worked as a researcher in the Roela Bank (1996-1998). On the academic side, Sebastian was professor of Monetary Economics and Microeconomics at the UNC.
Within SIGLA, Sebastian has held several positions, from head of the Economics Area (Sigla 2000-2002), Project Manager (Siglasul 2002-2006) to project Director in 2006 (Siglasul).

redpajama_set_name: RedPajamaCommonCrawl


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'Ghost Songs of the Conscientious Objectors' collaboration with Rideout resource now available
Posted on January 30, 2020 by ittsoundingout in Music in Prisons, News // 0 Comments
'Ghost Songs of the Conscientious Objectors' collaboration with Rideout resource available
We were delighted to be invited by Rideout (Creative Arts for Rehabilitation) to be involved in their Staging Time programme, for the Ghost Songs of the Conscientious Objectors project at HMP Stafford.
The resulting text and music is now available for others to use (see note below on Performing Rights): Ghost Songs of the Conscientious Objectors Book
'Not Quite the Ritz' is an example of the music created on the project:
Ghost Songs of the Conscientious Objectors was originally devised and performed by men at HMP Stafford. It was the third in a trilogy of performing arts projects produced by Rideout (Creative Arts for Rehabilitation) as part of Staging Time – an exploration of the history of 19th and early 20th century prison with serving prisoners. This was a programme of activity arising from a partnership with the Wellcome Trust funded research programme, Prisoners, Medical Care and Entitlement to Health in England and Ireland 1850 – 2000, led by Professor Hilary Marland (University of Warwick) and Associate Professor Catherine Cox (University College Dublin).
Ghost Songs of the Conscientious Objectors explores the experiences of World War I conscientious objectors, and particularly those who were sent to prison for their beliefs. Furthermore, it celebrates the role the objectors played in the prison reforms of the early part of the 20th century.
Ghost Songs of the Conscientious Objectors was co-facilitated by professional artists from Rideout and the Irene Taylor Trust who worked with a group of 20 prisoners for two weeks to devise and rehearse the work. The final performance, conceived as a 'secular service', was performed to an invited audience at HMP Stafford on 14 November 2019.
We had always intended to make the songs available for others to perform, but a number of audience members lamented the fact that a performance about such an important part of prison history was only seen by a small number of people. As a result we made the decision to make the whole piece available, text and songs (here).
Performing Rights
Rideout (Creative Arts for Rehabilitation) and Irene Taylor Trust grant a non exclusive license to amateur choirs and/or groups to perform this work free of charge, on the condition that you inform them of your intention to do so. This right is solely for amateur choir and/or groups. For all other performances, a fee will be payable.
In both instances contact admin@rideout.org.uk for further information.
Ghost Songs of the Conscientious Objectors was commissioned by the University of Warwick and funded by the Wellcome Trust as part of Prisoners, Medical Care and Entitlement to Health in England and Ireland 1850-2000, with additional funding from Arts Council England, HMP Stafford, the University of Warwick, the W.E.D Trust, the Edward Cadbury Charitable Trust and Thomas Deane Trust.
Rideout


After picking up a mattress, we always have a plan for how we're going to dispose of it. Our company will either donate the full mattress or recycle it depending on what condition it's in. We also do full bed removals as well. Mattresses can be difficult to get rid of in most circumstances, so give us a call today and we will give you a helping hand!
We have a very organized program in which we recycle old beds and bed products. We want to make sure we are preserving and protecting not just Arizona but our entire earth in any way we can. If you would like an estimate of how much our professional bed and mattress removal service would cost you, click here or give us a call at (480) 454-5585.
Let us deal with the stress of getting rid of your old mattresses and beds! Once you give us a call we will ask you a few questions to get more information about the job. Once enough information is received, we will present you with a friendly estimate based off of what we think it will cost and an appointment time will be established. Two professional employees will then get to your property at the scheduled time to give you a free, no obligation quote after the trash is inspected.


8190 x losing cards: Sorry you have not won.
Shakeaway Milkshake Bar wanted a campaign to generate customer loyalty and create a bit of a 'Buzz' and interest and scratch cards were seen as a great solution to give something back to customers and create interest.
They commissioned our Bespoke 'MULTI WIN' Game as it allowed the inclusion of a variety of winning cards with varied quantities (ranging from, 10, 20, 150, 200, 5000 and 8190). This variety is not offered by our standard Hot Card game. The ability to vary winning combinations cheaply and easily, meant the client was able to put together a suite of prizes that reflected their product range. Because of the way we produce our bespoke ranges, the client in theory could of had 10,000 different card combinations is they so wished.


Lots of Styles and Sizes to choose from!
carries only the best selection of women's shoes from a variety of name brands.
No wonder the second fastest growing profession is podiatry (the care and treatment of human feet in health and disease). Foster's Shoes is perfectly aware of these problems and we aim to educate our customers and find them the right shoe size. With over 30 years of service, we have the knowledge and offer sizes and stylish women's shoes selections to get you walking comfortably again.


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La présidence chypriote du Conseil de l'Union européenne en 2012 désigne la première présidence du Conseil de l'Union européenne effectuée par Chypre depuis son entrée dans l'Union européenne en 2004.

Elle fait suite à la présidence danoise de 2012 et précède celle de la présidence irlandaise du Conseil de l'Union européenne à partir du .

Programme

Identité visuelle
Le logo de la présidence chypriote de 2012 représente la personnalité du pays dans sa vision de présider le Conseil de l'Union européenne : le voilier qui reprend l'idée d'insularité de Chypre, prend ici le large pour se diriger vers le cœur de l'Europe. Ce navire devient au cours de son voyage l'allure d'un oiseau qui symbolise le pays.

Les couleurs ont également une signification précise : le bleu du navire reprend la couleur du drapeau de l'Union européenne, les couleurs cuivre et verte des voiles reprennent celles du drapeau chypriote ainsi que la terre du pays baignée de soleil, parsemée d'oliviers, et produisant du cuivre. Enfin, le bleu clair de la voile représente la mer et le ciel qui se veut accueillant et permettant l'harmonie entre la coexistence des peuples.

Sources

Références

Bibliographie

Compléments

Liens externes
 Site officiel de la présidence chypriote du conseil de l'UE en 2012.
 , Le Dessous des cartes.

Chypre, 2012
2012 à Chypre
2012 dans l'Union européenne
Relations entre Chypre et l'Union européenne

redpajama_set_name: RedPajamaWikipedia


When working on large result sets, you should consider using one of the functions that fetch an entire row (specified below). As these functions return the contents of multiple cells in one function call, they're MUCH quicker than mysql_result(). Also, note that specifying a numeric offset for the field argument is much quicker than specifying a fieldname or tablename.fieldname argument.
Calls to mysql_result() should not be mixed with calls to other functions that deal with the result set.


Looking for a temporary (or not so temporary) furniture solution? CORT offers a wide selection of high-quality furniture for rent near 49085, as well as convenient delivery, setup, and pickup options.
When it's time for a transition in life, renting furniture can be one of the best decisions you make. With CORT, you can avoid spending big bucks on furniture you'll end up having to sell or donate. As a Berkshire Hathaway Company, CORT is committed to quality and affordability. That's why we offer flexible leases, helpful delivery and setup, and a variety of payment options. Wherever you're headed, we can be there, too. We have hundreds of furniture rental showrooms across the U.S. and a network of global partners in 85 countries.
Turn a short-term place into a relaxing retreat by renting everything you want, from luxurious towels to big screen TVs. CORT does more than lease out necessities like sectionals, coffee tables, and dining sets, we also have housewares for rent such as dishes, pans, pots, and even indoor grills. Our furniture for rent will have you putting out a "Home Sweet Home" doormat in no time. And if your temporary living situation becomes a permanent one, you can purchase your rented furniture at a major discount. So enjoy an easier move. Contact a CORT Furniture Rental Showroom near 49085.
Off to college? Awesome! We have a quick word of advice for you. Don't spend your money on furniture you won't use for long. With our student packages, you can focus on your studies while we do what we do best: make your life simple by taking care of all the furniture arrangements. Just tell us where your school is located. Then, select a lease length (like six to 12+ months), pick a furniture bundle that meets your needs, and decide whether you want to pick out the pieces or have our stylists do it. After you check out, we'll arrange a time to deliver and set up your furniture. We can pick it up when your rental period ends, too! Our student furniture packages are designed to fit your needs, whether those include a full apartment with a living and dining room, or just your bedroom essentials. Heading back to school never looked better! Our great plans and student discounts make renting furniture a breeze. Starting at $99 per month for a 12-month lease.
Adding new employees or moving your company to a new location in Michigan? Turn to CORT for corporate furniture. We have customizable workplace furniture solutions that grow alongside your company. Boost revenue and keep great employees by creating an environment that fosters productivity and impresses clients. Let's bring your vision to life with the right corporate furniture for rent near 49085. Whether you're furnishing a satellite office, bracing for a merger, or preparing for your busy season— CORT's office furniture for rent can help keep your business "in the green!"
If you're a home stager, real estate agent, or homeowner, you know selling a house is tough. The market is competitive around 49085! A stylishly staged home can turn an open house visitor into an interested buyer—but buying staging furniture makes little financial "cents." That's why we rent furniture for home staging near 49085, with a variety of style options to suit any type of home. Decorate a whole house or pick and choose strategic accent pieces. CORT has the flexibility and style professional home stagers need. Rent home staging furniture to highlight a space's best qualities and get it sold faster!
Moving for college? Furniture rental with CORT gives you the flexibility and student discounts you need to create a space you'll love. Is your military family sick of lugging heavy furniture from state to state? CORT military discounts and packages will make your next PCS a breeze. Hiring seasonal workers to get your biz through the busy season? Rent office furniture for your short-term hires! You have options with CORT, and never have to commit to furniture ownership. Find a CORT Showroom near 49085 to get started, or browse our catalog online.


'Lloyd George at War, 1916-1918' provides a much needed re-evaluation of this charismatic prime minister's wartime leadership. Calling on a wide range of primary sources and focussing on Lloyd George's role in the war cabinet, Cassar compellingly argues that George's reputation as the "man who won the war" was wholly unmerited. Instead Cassar shows that Lloyd George's heavy handed leadership was often detrimental to the Allied cause. From his wholehearted support for the disastrous Nivelle offensive, to his pursuit of a peripheral strategy that diverted troops away from the critical theatre of war on the Western Front, Cassar shows that Lloyd George consistently bucked the advice of his generals in preference for ineffectual and dangerous military strategies. Cassar's approach also differs from that of other studies of Lloyd George by adopting a thematic approach in preference to a chronological narrative, thereby allowing a closer evaluation of Lloyd George's handling of complex issues.
Cassar, G. H. (2009). Lloyd George at war, 1916-1918. London ; New York, N. Y.: Anthem Press.


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Q: Should I use id numbers or meaningful texts in HTTP requests payload I have been searching about that and I couldn't find any references to endorse my impression that it's worthier to use meaningful texts inside requests body or response than just ids in situations where you have a restricted and small scope of possible values. Let me exemplify that. What should I use:
{
 "idSystemStatus": 1
}

or that:
{
 "systemStatus": "alert"
}

What is the best practice? Could you please give me references?

A: Being an API, means that other systems will read it. So it is important to be bandwidth-optimized, and it makes sense to use shorter and numeric values where appropriate.
But if you explicitly need wording, try to make that as short and concise as possible.

redpajama_set_name: RedPajamaStackExchange


text:
Q: Ajuda com comparação de datas em Java Script Preciso comparar data final de um contrato de serviço para colocar em um relatório que vai ter 4 tipos de status:
1- contrato em vigor (Verde)
2- contrato próximo ao vencimento (Amarelo)
3- contrato vencido (Vermelho)
4- contrato com prazo indeterminado (Azul)

Estou recendo 2 valores pelo usuário, dt_inicio e dt_final, preciso que da dt_final seja comparada com a (new Date) dt_atual ou seja,
"Se a dt_final for >= dt_atual então o contrato está vencido." | "Se a dt_final for < dt_atual então preciso que o resultado dessa data seja transformado em meses para conseguir comparar, exemplo dt_final 27/10/2018 < dt_atual 27/06/2018 = 4 meses que vai adiciona esse valor na variável dt_vigor.
Se dt_vigor  =< 4(meses) então adiciona valor em (próximo_vencimento);
se dt_vigor > 4(meses) então adiciona valor em (vencimento_ok)
se não (sem_vencimento);

A: Trabalhar com datas em javascript é mais fácil utilizando o moment.js.
O moment é bem documentado e possui vários exemplos de uso.
Segue exemplo da comparação de data atual com outra(dt_vigor);

var dt_vigor = moment("01/05/2018", "DD/MM/YYYY");
if(dt_vigor <= moment().subtract(4, 'month')){
   alert('dt_vigor tem 04 meses ou mais.');
   //adiciona valor em (próximo_vencimento);
   }else{
   alert('dt_vigor tem menos de 04 meses.');
   //adiciona valor em (vencimento_ok)
}
<script src="https://cdnjs.cloudflare.com/ajax/libs/moment.js/2.22.2/moment.js"></script>

Espero ter ajudado!


To show off the amazing work of our AVID (Advancement Via Individual Determination) students and teachers, Rollins Elementary School and Butler High School recently hosted AVID Showcases. AVID is a multi-state initiative used to help underachieving students with high academic potential, prepare for post-secondary education through engaging, rigorous, and student-centered learning environments. A strong AVID system transforms the instruction, systems, leadership, and culture of schools, ensures college readiness, and improves academic performance for all students.
Our K-12 AVID schools are on the road to success!


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Selfless Among Us: Rhonda Frederick, CEO of People Inc.
Western New York's largest human service provider, People Inc., is led by Rhonda Frederick who is being celebrated as one of the "Selfless Among Us."
Author: Melissa Holmes
Published: 7:04 AM EDT May 25, 2022
BUFFALO, N.Y. — People Inc. is an agency that touches the lives of thousands of seniors and people living with disabilities in Western New York. Its leader, Rhonda Frederick, has been president and CEO since 2014, but has been with the agency for four decades, and has changed countless lives for the better along the way.
"I fell into this. I have to be absolutely honest," Frederick admits.
The first time she walked through the doors of a People Inc. facility was when she landed her first job there out of college in 1980.
"It wasn't as if I had a passion for this at this point. I got a job in a group home. I came here and absolutely fell in love," said Frederick.
And more than 40 years later, Rhonda is now CEO of the agency that helps people with developmental disabilities and seniors find independence and acceptance.
Before being named CEO in 2014, Frederick was COO of People Inc., managing the $143 million operating budget and its 3,400 employees. According to her biography, "she also oversaw all residential, day services, service coordination, in-home supports, senior services and health-related services and had administrative oversight of quality improvement, government relations, program development and legal."
But what is most meaningful to Frederick?
"We've been able to help people find jobs, to find meaningful activities during the day, to experience all life's pleasure," she said.
For Bill Collins' daughter Elena, the pleasure comes from just being able to live on her own with other girls in a People Inc. apartment.
"I don't know what we would do without People, Inc. because she's happy and she has her own life," said Collins, a People Inc. board member.
Jill Turchiarelli has her own life, too.
"I've been here for 24 years and love every minute of it," she said.
Turchiarelli doesn't just receive services from People Inc., she also works there as a receptionist.
"There's not a lot of people out there that employ people with disabilities, and we like everybody else need to have an opportunity, equal opportunity, to be able to show what we can do," she said.
Jill thanks Rhonda and her leadership for giving her the chance to live a happy and fulfilling life.
Frederick also serves as president of the Developmental Disabilities Alliance of Western New York (DDAWNY). She is the Board Chair for Person Centered Services (PCS) and currently serves on the boards of Episcopal Church Home and Affiliates, Inc., Hilbert College, New York State Industries for the Disabled (NYSIDD), Special Olympics NY, Amherst Meals on Wheels and Accountable Health Community Inc. She also sits on the Board of Regents for Canisius College and the Executive Committee of the Buffalo Niagara Partnership.
One of Rhonda's other passions is serving on the steering committee for WNY iCan Bike.
To nominate someone to be featured in the "Selfless Among Us" series, email Melissa.Holmes@wgrz.com.
Selfless Among Us: Roswell Park's Kim Sweeney
Good Neighbors: 2 firefighters in Amherst recognized for over 50 years of volunteer service
Selfless Among Us: Kenya Peoples
To see others featured in the "Selfless Among Us" series, click the videos below:


My first guide is a collection of selling resources which will show you how my marketing plan will benefit in the sale of your home. It explains my approach and how I will sell your home for the right price in the right time. I believe after reading this booklet and interviewing me you too will feel confident in your decision to use my real estate services. You can download it below!


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The Reverend Edward Lee Roy Elson (December 23, 1906 – August 25, 1993) was a Presbyterian minister and Chaplain of the United States Senate.

Life
Edward Lee Roy Elson, the first of nine children, was born in Ohio, to Leroy Elson, a locomotive engineer, and his wife, Pearl. Early on he was encouraged to study music and gave concerts in the Pittsburgh area on the cornet with his sister Hazel playing the piano.  One of his favorite memories of high school was the time he and his sister gave a concert in the very early days of radio on KDKA, the pioneer radio station.

Dr. Elson had his education a

at Asbury College in Wilmore, Kentucky, and then went to University of Southern California for a master's in theology.  He married Frances Sandys, a fellow Asbury College student in 1929.  At about the time of his ordination in 1930, he learned that his young wife had a very serious illness, and owing largely to this, he chose to go and serve at the La Jolla Presbyterian Church because of its proximity to the  Scripps Clinic in La Jolla, California.  His wife died three years later on his birthday.

Having been invited to join the American Seminar in Europe and Russia, Elson took an eye-opening trip to Europe in the summer of 1936. Shortly after returning from Europe,  Elson married Helen Chittick, a member of his church.

After having been in the chaplain reserves for ten years, he resigned his position with the church and went on active duty with the Army in 1941, arriving in France in December 1944.  Not long after, General Frank Wilburn requested that Elson be his personal representative at the execution by firing squad of a soldier for desertion.  This soldier, Eddie Slovik, was the first to be so executed by the American military since the American Civil War.  Another of his wartime assignments was to interview members of the clergy who had been imprisoned at Dachau.  After the German surrender, he was asked to represent Dwight D. Eisenhower before the Consistory, a ruling body of the German Protestant church, in order to determine how the German Church would be rebuilt.

Upon returning to the U.S. from the war, he soon learned that he was a candidate for the pastorate of the Covenant-First Presbyterian Church in Washington, D.C. and ultimately became its pastor in 1946.  One of his first duties there was to oversee the transition of the Covenant-First Presbyterian Church to the National Presbyterian Church, a move that had been in the works for many years. Eisenhower attended a pre-inaugural service at the church.  A few days later, on February 1, 1953, Dr. Elson baptized the president and admitted him to formal membership of the church.  The baptism came after the president's brother, Milton, confirmed that though Ike had regularly attended the River Brethren Church in Abilene, Kansas, he had never officially joined the church nor had he been baptized.  In the 1960s, Elson oversaw, along with the building committee, the construction of a large new church, which was dedicated in 1967 on Eisenhower's birthday, October 14.

In 1967, he was named to a special committee of the Presbyterian General Assembly to study the Vietnam War. In September 1967, while he and his wife were still at their summer home in Cape Breton Island, he received a phone call from the White House asking him to be on a team to observe the upcoming elections in South Viet Nam.

Dr. Elson was elected to the position of Chaplain of the United States Senate in 1969, retiring from that position after having served for a little over twelve years in February, 1981.  During his tenure at the Senate, he invited the first woman, Wilmina Rowland, to offer the opening prayer.

Elson and his wife Helen Chittick (1915–2007) are buried in Arlington National Cemetery.

Works
 America's Spiritual Recovery, 1954
 And Still He speaks, The words of the Risen Christ, 1960
 Inevitable encounter, 1962
 Prayers offered by the chaplain of the Senate of the United States/ Edward L.R. Elson, at the opening of the daily sessions of the United States Senate during the 96th and 97th congresses, 1979–1981, 1980
 Prayers offered by the chaplain of the Senate of the United States/ Edward L.R. Elson, during the Ninety-second Congress, 1971–72, 1973
 Wide was His Parish, An Autobiography, 1986

Bibliography
 Wide was His Parish, An Autobiography, Tyndale Press, 1986,

References

External links
 History of National Presbyterian Church
 Senate Chaplains on Senate Website
 Obituary for Helen C. Elson

1906 births
1993 deaths
People from Monongahela, Pennsylvania
American Presbyterian ministers
Chaplains of the United States Senate
Asbury University alumni
Burials at Arlington National Cemetery
20th-century American clergy


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Cardi B, JuiceWrld, Bazzi, Rosalia and more Astound at Made In America 2019 Day 1
Andrew Wendowski September 4, 2019	Featured, Festival Photo Galleries, Festival Reviews
The annual Made In America Festival produced by Live Nation has become a Philadelphia tradition, returning to the Benjamin Franklin Parkway each and every year in Philadelphia during Labor Day Weekend, giving fans a reason to get out and celebrate with some of the hottest names in music or artists who will soon become the biggest names in music. The two-day music festival is curated annually by Jay-Z himself, and we have got to give it up for him as each year he somehow chooses the hottest music artists today and adds in those who he thinks will be taking off rapidly usually becoming the next year's headliners. The festival return for the eighth year in Philadelphia bringing another stacked lineup of incredible performers to the parkway.
Headlining the festival for day one, August 31st, was the hottest female rapper in the industry right now, Cardi B. Returning to the festival for the second time, the first being in 2017 as the "Bodak Yellow" hitmaker, but now she is headlining with a full album and numerous collaborative efforts showcasing her talents to the masses. Her unfortunately short set was about 60 minutes long but it was full of ALL of her songs and her hits filling the setlist with fan-favorite songs like "Money," "Drip," "Be Careful," "Please Me," "I Like It," "Finesse" and of course her latest single "Press" and the song that put her on the maps "Bodak Yellow." Early on in her set she showcased some of her roots showing off some strip-club moves during her song "Money Bag," pausing to tell the crowd that, "I've always had a special love for Philly — even when I was a stripper."
What was your favorite part about @iamcardib's @miafest set this weekend? #TIDALxMIA #MIAFest #CardiB
A post shared by Music Mayhem (@musicmayhemmagazine) on Sep 2, 2019 at 10:11pm PDT
We were stunned by how amazing of an entertainer Cardi B was, we also got to check out a bunch of other amazing artists throughout day one of the iconic music festival like JuiceWrld, Rosalia, Jorja Smith, Bazzi, Anderson.Paak & The Free Nationals, Dominic Fike, Melii and Grace Carter.
Check out some photos from Day 1 below:
Tags Cardi B Dominic Fike Grace Carter Jorja Smith Juice Wrld JuiceWrld Made In America Melii MIA Fest MIAFest
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Rock Fest returns for another year of some of the best rock and metal acts …


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You are here: Home › Ottawa out of running for SWB Yanks — but in line for affiliated ball
Ottawa out of running for SWB Yanks — but in line for affiliated ball
By Kevin Reichard on September 17, 2011 in Minor-League Baseball, News
There's virtually no chance the Scranton/Wilkes-Barre Yankees (Class AAA; International League) will be playing next season in Ottawa Stadium, but a Canadian ownership group is working to bring an Eastern League team to Canada's capital city for 2013.
Where the Yankees will end up remains a matter of conjecture, and the issue will be decided at the upcoming International League meetings in Albuquerque. Coca-Cola Park, home of the Lehigh Valley IronPigs, is a contender, as are a few other regional ballparks cited by MiLB owners. We don't expect the team to stray too far from home.
At one point Ottawa was positioned as a contender for hosting the SWB Yankees, but issues with the facility — it needs a million dollars in improvements to be ready for affiliated ball, we're told — will prevent it from being used for just a season by Class AAA ball.
Now, having said that, the prospect of affiliated baseball returning to the former home of the Ottawa Lynx (Class AAA; International League) is stronger now than it's been in recent years, with what we've heard described as a "strong effort" to being an Eastern League team to the ballpark as soon as 2013. There are plenty of moving parts at play, including the sale of the team by the current EL team and a purchase of a short-season A NY-Penn League team to replace it. This also coincides with the efforts of another Eastern League team owner to explore placing a team in Montreal, an efforts already receiving the approval of the N.A. Montreal is seen as the better market except for one big issue: there's no minor-league ballpark in the city.
If the effort to bring an Eastern League team to Ottawa falls short, the potential local owners could buy a NY-Penn League team instead.
As several owners pointed out, there are plenty of moving parts to coordinate with these efforts — and where there are moving parts there are points of failure. Still, owners seem optimistic about the prospect to returning affiliated ball to Ottawa.
RELATED STORIES: NY Yankees making moves with minor-league teams; Fat Cats owners may seek affiliated team for Ottawa; Valcke: Baseball can work in Ottawa; Ottawa: Ballpark should be converted to concert venue; Affiliated ball may be returning to Ottawa
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Solid sign of spring: annual Whitecaps fan food submission drive begins
Albuquerque, team address Isotopes Park upgrades
Studers donate $500K to Rock County literacy program
Lake County Captains acquired by COLLiDE Sport
New Salt Lake Bees ballpark proposed for South Jordan
coca cola park, eastern league, international league, montreal, ny penn league, ottawa, ottawa lynx, ottawa stadium, scranton/wilkes barre yankees
Controversy dogs Keys lease negotiations to the end
For sale: Alliance Bank Stadium


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(Sputnik) – The released footage of drones, which attacked Russian military bases in Hmeymim and Tartus, shows three practically intact handicraft UAVs made from boards and plywood, with wires, wrapped in tape and green polyethylene. In addition, the photo shows the debris of three more apparatuses spread over separate heaps.
The Defense Ministry noted that the design used by the militants could only be obtained from a technologically advanced country, and warned of the danger of such attacks in any country in the world.
The photos were published in the wake of the Russian Defense Ministry's January 8 report of a terrorist attempt to attack Russian military positions in Syria with combat drones that had been disrupted on January 6. Ten of the drones targeted the Hmeymim airbase and three were sent toward the Tartus naval base. As a result, three of the 13 drones were brought to the ground in a controlled area outside the base, while three UAVs exploded after colliding with the ground and seven UAVs were destroyed by regular Pantsir-S air defense missile systems.
As the Krasnaya Zvezda newspaper, the official publication of the Russian Defense Ministry, has specified, the drones that attacked the Hmeymim airbase flew out of the area in the southwest of the Idlib de-escalation zone in Syria, controlled by the so-called moderate opposition.


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I'm not asking specific information to configure apache, nginx, lighthttpd or other!
I would like to know what kind of information is sent to clients when servers want rewrite url?


At the time of the Spanish Conquest, the indigenous population of what we now call Mexico, was about 20,000,000. By 1600, after the introduction of European diseases, only about a million remained. The four big killers were small pox, measles, mumps, and pneumonia. In 1545, over 800.000 people died in one small pox outbreak alone. Bartolome de Las Casas, the first clergyman ordained in the New World tells us that the conquistadors destroyed between 15,000,000 and 20,000,000 Native Americans in the Western Hemisphere. Most were enslaved, branded, and sold on the world market for fifty gold pesos.


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Broadway actress mistakes captioning device for illegal recording
Abby Sneed, Copy Editor|December 14, 2022
Photo provided by flickr.com
Actress Lillias White at a conference
On the night of Oct. 12, Samantha Coleman posted an Instagram video describing her "horrifying and embarrassing experience" at a Broadway production of "Hadestown." During the performance, Coleman was publicly heckled by actress Lillias White for using a closed captioning device, which she mistook Coleman to be illegally recording the show with. The captioning mechanism was provided by the theater itself, which could be used by attaching it to a phone.
Coleman took to social media to share her story, with the goal of spreading awareness of the inaccessibility in the field of theatre.
"Systemically [theater] is an exclusionary space for people who are disabled, has always been," Coleman said in her Instagram post. "This is just shining a light on that. If we do not address the underlying issues of inequality in theatre, we will never truly progress as an industry," all according to deadline.com.
White reprimanded the hard of hearing woman not once, but twice during the performance, putting the actress along with the production under fire. The Jujamcyn Theaters have since then contacted Coleman to apologize for the incident, along with "Hadestown" offering tickets for her to come see the show again to compensate for the dispute.
"We have a commitment to accessibility in all forms," a Jujamcyn Theaters spokesperson said in an interview with NBC New York. "The incident yesterday is a reminder that this is an ongoing process needing constant revisiting and renewal. We are reviewing our policies and internal protocols to ensure this doesn't happen again."
Although the exploit seems to be a truthful error, Coleman is determined to speak out against the injustice towards disabled people within the theater community.
"I don't think this is inherently [White's] malice," Coleman said. "I think it's a misunderstanding, but we still need to talk about it."
Other members of the hearing loss community have shown empathy towards Coleman's experience, sending condolences to her online. Many have also expressed their gratitude that the issue is being faced head-on, allowing for theaters to be more open and accepting of not only new technology, but respecting the people who need it, all according to nbcnewyork.com.
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Off the Web
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\section{Introduction}
\cite{Buratti91} found that all five of the primary Uranian satellites, excluding the innermost Miranda, exhibit systematic leading-trailing color asymmetries of roughly 2-23\% that increase with distance from the primary.  In particular, the leading hemispheres of these tidally locked satellites (pointing in the direction of motion) are redder than their respective trailing hemispheres.  Explaining the origin of this phenomenon is challenging.  We briefly consider several exogenic possibilities, dismissing endogenic alternatives due to the difficulty of geological processes producing an effect coinciding with the satellite's apex of motion.  Exogenic hypotheses can be divided into two categories:  sources from within the Uranian system, and sources from beyond.

For explanations that rely on particles that come from beyond the Uranian system, we consider alteration by:  (i) interplanetary dust particles (IDPs) \citep[see][for an analysis of the Saturnian system]{Cook70}, (ii) interstellar dust particles (ISDPs) \citep{Landgraf00}, (iii) solar radiation \citep{Hodyss09}, and (iv) cosmic rays \citep{Johnson90}.  A tidally locked satellite on a circular orbit (like the primary Uranian satellites, to an excellent approximation) rotates on its axis once per orbit at a constant rate.  For (iii) and (iv), the incoming particle velocity is large enough that the satellite's motion is negligible.  Furthermore, the paths of these satellites over an orbital period ($\lesssim$ 2 weeks) are small compared to the distances over which the incoming particles travel.  If one therefore ignores the moon's orbital motion and simply imagines it rotating in place, one can see that the leading and trailing sides will spend an equal amount of time facing each inertial direction.  Thus, a distribution of fast incoming particles like solar photons and cosmic rays cannot generate a hemispherical leading/trailing asymmetry.

On the other hand, if the incoming particles have speeds comparable to a satellite's orbital speed ($\sim 5$ km/s), the moon's motion introduces a detectable asymmetry.  Like a car's windshield, the satellite's leading side will accumulate more material relative to its trailing side the faster it ploughs through the rain of particles.  This is certainly the case for IDPs, whose speeds relative to the satellites is $v_{Rel} \sim 10$ km/s, and less so for ISDPs ($v_{Rel} \sim 30$ km/s).  However, this argument predicts that inner satellites with faster orbital velocities should exhibit stronger asymmetries, which is opposite to the trend found by \cite{Buratti91}.   Furthermore, gravitational focusing by Uranus would intensify the flux of IDPs and ISDPs nearer to the planet, which again runs counter to the observed pattern.  Thus, (iii) and (iv) cannot produce leading/trailing asymmetries, and while (i) and (ii) in principle could, they would generate the opposite trend with semimajor axis to what is observed.  It therefore seems unlikely that the source of the Uranian regular satellites' leading/trailing asymmetries lies beyond the Uranian system.

Explanations from within the Uranian system include magnetospheric effects \citep[see][for a discussion in the Saturnian system]{Schenk11}, and the infall of dust that originates at the irregular satellites.  Though resonant phenomena could in principle complicate the picture, magnetospheric effects would generally incorrectly predict a larger effect on inner moons, since all the satellites are beyond the co-rotation radius and the magnetic field strength falls off rapidly with semimajor axis \citep{Buratti91}.  We are therefore left with the last hypothesis, dust from the irregular satellites, which we evaluate in the remainder of this paper.  In fact, though the currently known Uranian irregular moons lay undiscovered at the time, \cite{Buratti91} argued that such dust from unseen outer satellites could account for the observed hemispherical differences.

\subsection{The Irregular Satellites}

To date, nine irregular satellites have been found around Uranus, and many more around the other giant planets.  In contrast to the large regular satellites nestled close to their planets, the irregular satellites are a separate population of distant, small moons.  These bodies, rather than forming in a circumplanetary disk, are thought to have been captured by their respective planets' gravity (perhaps with the aid of drag forces) early in the Solar System's history \cite[see][and references therein]{Nicholson08}.  As a result, the irregulars' orbits form a distant swarm of mutually inclined, highly elliptical, crossing orbits. This  suggests an intense collisional history that would have generated much debris and dust, particularly at early times \citep{Bottke10}.  Furthermore, micrometeoroid bombardment of the irregular satellite surfaces would contribute further dust over the age of the Solar System.

Dust particles of radius $10\mu$m will then slowly migrate inward through Poynting-Robertson (P-R) drag on a timescale of five million years, with the timescale for larger particles scaling linearly with grain radius \citep{Burns79}.  Upon reaching the inner Uranian system, this dust will coat the regular satellites.  We evaluate the dust grains' ability to generate leading/trailing asymmetries below.  Figure \ref{cartoon} shows this process schematically.  Note that the irregular satellites, which are dominantly affected by solar perturbations, lie (very roughly) symmetrically about the planet's orbital plane, while the regular satellites lie in the planet's equatorial plane, which, due to Uranus' extreme obliquity, is $98^{\circ}$ away!  The diagram also displays a chaotic range in semimajor axis that is more fully described below.

\begin{figure}[!ht]
\includegraphics[width=12cm]{fig1.eps}
\caption{\label{cartoon}  Schematic diagram showing the geometry of the Uranian system.  The regular satellite orbits lie in the planet's equatorial plane, which is inclined by $98^{\circ}$ to the planet's orbital plane, shown by the surrounding rectangle.  The irregular satellites (black dots) lie at large distance from the planet on inclined orbits to the planet's orbital plane.  They have only been drawn on the left and right for clarity, but there would also be moons at phases in their orbit such that they lie at the bottom and top edges of the plane pictured.  Dust from these satellites will spiral inward over millions of years through P-R drag, eventually entering a chaotic semimajor axis range schematically depicted by two concentric, dashed rings.  Upon doing so, the dust orbits will undergo chaotic large-amplitude oscillations in eccentricity and inclination.  See Sec. \ref{Dynamics} for details.}
\end{figure}

We pause to caution that several important aspects of these processes are poorly constrained.  For example, the lifetimes of dust particles orbiting planets in the outer Solar System are very uncertain.  The main mechanisms for grain destruction are sputtering, shattering by micrometeoroids, and sublimation.  The last of these is not thought to be important at Uranus and Neptune, and \cite{Burns01} give sputtering and shattering timescales of $\sim 10^{5\pm2}$ and $\sim 10^{6\pm2}$ years for 1-micron particles orbiting Uranus in its magnetosphere, respectively.  However, dust from the irregular satellites lives out its life in a very different environment to typically-considered circumplanetary grains.  Because the irregular satellites ($\sim 200-800$ Uranian radii, $R_p$) reside far beyond the magnetopause ($\sim 20 R_p$), sputtering should be much less important.  Also, far out in the Uranian gravity well, IDPs and ISDPs are not as gravitationally focused and have reduced orbital speeds, resulting in longer collision timescales.  However, depending on the optical depth of the generated dust cloud, one may have to consider mutual collisions between grains \citep{Tamayo11}.  Given our crude knowledge, it is not clear whether lifetimes of such particles can be very long ($\sim 100$ Myr), or whether large particles will be eroded into smaller particles that evolve inward faster and have longer collisional lifetimes \citep{Burns01}.

A second uncertainty is the total supply of dust available from the irregular satellites.  If this quantity is much smaller than the mass of IDPs striking the regular satellites, it would seem dubious to suppose that the irregulars could be responsible for the color asymmetries.  \cite{Cuzzi98} estimate an IDP mass flux $\sim 5 \times 10^{-16}$ kg m$^{-2}$s$^{-1}$ of IDPs in the outer Solar System.  This corresponds to $\sim 10^{14}$ kg on each of the regular satellites over 5 Gyr.  As for the irregulars, \cite{Bottke10} estimate that, over the Solar System's history, these satellites would produce $\sim 10^{20}$ kg of dust solely through mutual collisions (this number would be enhanced by micrometeoroid bombardment).  This value, however, is very uncertain since it assumes a number and distribution of primordial irregular satellites that is poorly constrained (it draws initial conditions from models of irregular satellite capture during a Nice-model reshuffling of the planets).  Furthermore, as discussed above, it is then not clear what fraction of this dust will survive on its way inward.  Nevertheless, we find below that the vast majority of surviving grains will strike one of the regular satellites; it therefore seems plausible that irregular satellite debris represents the dominant source of micrometeoroids impacting the regular satellites.

Finally, the precise mechanism through which incoming dust particles alters the satellites' surface color is unclear.  Does the altered color represent a contribution from the dust material?  Is the satellite's regolith mineralogy altered by the micrometeoroid impacts due to vaporization and/or melting?  Or is it something else?  Presumably the answer involves all three.

In the end, we take the view that the above considerations are unfortunately too uncertain to be of much guidance.  Yet if, as we have argued, other sources are unable to account for the hemispheric asymmetries and if, as we will try to show, irregular satellite dust can, then perhaps this provides constraints on these quantities that are so difficult to estimate, like the grain lifetimes and the total dust mass generated by the irregulars.

\subsection{Dynamics} \label{Dynamics}
\cite{Buratti91} favored an infalling-dust explanation of the hemispherical asymmetries by analogy to arguments for the Saturnian satellite Iapetus \citep{Soter74, Tosi10, Tamayo11}, which seems to display a much more extravagant hemispherical albedo pattern as a result of subsequent runaway water ice sublimation \citep{Spencer10}.  This analogy has been strengthened by the recent discovery on Iapetus of a color dichotomy similar to those observed on the Uranian satellites \cite{Denk10}.  However, a closer look at investigations in the Saturnian system reveals an important difficulty.

\cite{Tosi10} and \cite{Tamayo11} find that Iapetus, the outermost Saturnian regular satellite, intercepts the vast majority of dust grains from the irregular satellites.  This should also be the case in the Uranian system.  Because the collision time with each satellite ($\tau_{Col} \sim 10^5 $yrs) is much shorter than the P-R decay timescale on which the dust moves inward ($\tau_{P-R} \sim 5 \times 10^{6}$ yrs for the smallest particles), one would expect almost no dust to penetrate inside the orbit of the outermost moon Oberon---yet three moons further in are observed to also exhibit leading/trailing asymmetries.  The key breakdown in the analogy between the two planetary systems is a dynamical instability in a chaotic range of semimajor axes that occurs owing to Uranus' extreme obliquity of $98^{\circ}$.  The goal of this paper is to investigate the effects of this instability to assess whether it is consistent with the observed hemispherical color asymmetries.

\cite{Tremaine09} study the dynamics of circumplanetary-particle orbits under the combined effect of the quadrupole potentials due to the planet's oblateness and the solar tide.  They find that around planets with obliquities exceeding $71.072^{\circ}$, particles with orbits starting far from the primary in the planet's orbital plane that are slowly brought inward become unstable over a range of semimajor axes.  In this unstable region, orbits undergo chaotic, large-amplitude oscillations in eccentricity and inclination on a secular timescale that is $\tau_{Sec} \sim 10^4$ yrs for circumuranian particles.  The unstable range roughly coincides with the location where the strengths of the two perturbations are comparable, which around Uranus, is $\sim 75 R_p$ \citep{Tamayo13}.

This provides a possible mechanism for creating the color dichotomies observed on the four outermost Uranian satellites.  Instead of slowly drifting past Oberon through P-R drag, the grains' pericenters abruptly plunge inward upon entering the unstable semimajor axis range.  This would (nearly simultaneously) spread dust across all the inner moons rather than predominantly concentrating it on the outermost satellite.  However, the dynamical results of \cite{Tremaine09} cannot be immediately applied to dust particles, as dust grains are also strongly perturbed by radiation pressure \citep{Burns79}.

\cite{Tamayo13} investigate the orbital modifications created by this additional force.  The first important consequence of radiation pressure is that it induces a variation in the particle's orbital eccentricity and pericenter location on Uranus' orbital timescale of $\sim 100$ years \citep{Burns79}.  We are interested in much longer secular timescales ($\tau_\text{Sec} \sim 10^4$ yrs), so these fast oscillations can be averaged out.  However, radiation-pressure effects are stronger for smaller particles, leading to larger-amplitude eccentricity variations.  Below a threshold particle size, the eccentricity reaches unity within the first half of a Uranian year, and the grain either collides with the planet or escapes the system.  Integrations show that this threshold size is $\sim 5\mu$m; we therefore only consider particles of radius $10\mu$m and larger.  \cite{Tamayo13} also find that radiation pressure shifts the position of the chaotic zone for most orbits with low initial eccentricities and inclinations to the planet's orbital plane.  While these analytic results furnish good intuition, the Uranian irregular satellites (and therefore the dust grains they generate) lie on high-eccentricity and high-inclination orbits, forcing our detailed investigation to be primarily numerical.  The equation of motion we integrate in our simulations is
\begin{equation} \label{eom}
{\bf \ddot{r}} = - \frac{GM_p}{r^3}{\bf r} + \frac{SAQ_{pr}}{mc} {\bf \hat{S}} - \frac{SA}{mc^2} Q_{pr}[({\bf \dot{r} \cdot \hat{S})\hat{S} + \dot{r}}] - \frac{GM_\odot}{2a_p^3} \nabla[r^2 P_2 ({\bf \hat{n}_p \cdot \hat{r}})] + GM_pR_p^2 J_2' \nabla\Big(\frac{P_2({\bf \hat{s}_p \cdot \hat{r}})}{r^3}\Big),
\end{equation}
where overdots denote time derivatives, and the right-hand terms, in sequence, are due to the dominant Uranian gravity, solar radiation pressure, Poynting-Robertson drag, the Sun's tidal gravity, and Uranus' effective $J_2$, treating the inner satellites' averaged gravity as a contribution to the planet's quadrupole field.  $G$ is the gravitational constant, $M_p$ the planetary mass, $r$ the dust particle's distance from Uranus, $S$ the solar flux at the grain's position, $A$ the particle's cross-sectional area, $Q_{pr}$ the grain's radiation pressure efficiency factor, $m$ the particle mass, $c$ the speed of light, $a_p$ the semi-major axis of Uranus (assumed to be on a circular orbit about the Sun) and $P_2$ the second Legendre polynomial.  The remaining vectors can be seen in Fig. \ref{vectors};  ${\bf r}$ is the particle's displacement vector from Uranus, ${\bf \hat{S}} $ is the unit vector from the Sun to the particle position, ${\bf \hat{n}_p}$ is the unit vector along the planet's orbit normal, and ${\bf \hat{s}_p}$ is the unit vector along Uranus' spin axis.  The effective $J_2$ including the contribution from the inner satellites is denoted by $J_2'$, and is given by
\begin{equation}
J_2' = J_2 + \frac{1}{2} \displaystyle\sum_{i=1}^5 \Big(\frac{m_i}{M_p}\Big) a_i ,
\end{equation}
where $J_2$ is the planetary $J_2$ coefficient, and $m_i$ and $a_i$ are the ith satellite's mass and semimajor axis, respectively.

\begin{figure}[!ht]
\includegraphics[width=12cm]{fig2.eps}
\caption{\label{vectors}  Diagram showing the various vectors in Eq. \ref{eom}.  The unit vectors ${\bf \hat{n}_p}$ and ${\bf \hat{s}_p}$ point along Uranus' orbit normal and spin axis, respectively.  The unit vector ${\bf \hat{S}}$ points along the line from the Sun to the particle, and the vector ${\bf r}$ is the particle's displacement vector from Uranus.}
\end{figure}

In order to demonstrate the viability of the creation of the Uranian color dichotomies through dust infall from the irregular satellites, we aim to show four properties of the process:  (i)  the dynamics are capable of spreading dust across the four outermost satellites, rather than concentrating grains on the outermost moon Oberon, (ii) the innermost regular satellite Miranda is not exposed to a comparable effect, (iii) there is an increasing trend with target satellite semimajor axis, and (iv) the incoming dust-particle distribution creates hemispherical leading/trailing asymmetries.  The last point is certainly not obvious in view of Uranus' peculiar obliquity, coupled with the fact that the chaotic orbital evolution of the dust particles generates large-amplitude ($\gtrsim 90^{\circ}$) swings in the grains' orbital inclinations, allowing them to strike the regular satellites from any direction.  The distribution of impacting grains over the regular satellite surfaces is therefore {\it a priori} highly uncertain.

\section{Methods} \label{inicond}
To characterize the dust-transfer efficiency from the irregulars to Uranus' regular satellites (Miranda, Ariel, Umbriel, Titania and Oberon), one would ideally integrate a representative sample of dust particles along with the regular satellites, checking for collisions at each timestep.  Unfortunately, the orbital phase space occupied by the irregulars (and the dust particles they create) is enormous.  One can reduce the computational load by observing that the satellites' and dust particles' pericenters and their relative nodes circulate rapidly and are roughly uniformly distributed from $0$ to $2\pi$.  We verified this for our integrations, though our simulations approximate the motion of the regular satellites as a contribution to the planetary quadrupole \citep{Tamayo13}, and therefore ignore the effects of orbital resonances (we note that orbits almost exclusively destabilize prior to encountering the first-order resonance regions with the regular satellites).  After integrating a dust particle orbit, at each timestep we use the formalism of \cite{Greenberg82}, with corrections from \cite{Bottke93}, to calculate collision probabilities with each of the regular satellites.  These formulae calculate a weighted collision probability assuming the pericenters and relative node to be uniformly distributed.  The values calculated from a single integration are thus equivalent to an average over a much larger population of orbits so distributed.  Finally, we use the methods \cite{Tamayo11} applied in the Saturnian system to combine the probabilities at each timestep into aggregate values.  This approach renders the phase space of initial conditions more tractable.  We believe that the errors introduced by this approximation are not significant relative to the uncertainty in the dust grains' physical and orbital parameters.  In addition to calculating collision probabilities, we further use the techniques in \cite{Tamayo11} to calculate the ratio of material striking the leading vs. the trailing side of each satellite.  We performed all our integrations with the well-established dust integrator dI \citep{Hamilton93} using a Bulirsh-Stoer time-stepper with adaptive stepsize.

Most dust particles escaping irregular-satellite surfaces should have ejection speeds comparable to the satellites' escape velocities \citep{Farinella93}.  Since these escape speeds are much smaller than the satellites' orbital velocities, dust grains should inherit their parent satellites' orbital elements.  While our method outlined above circumvents having to sample a variety of pericenter and node positions, the irregular satellites also span a wide range in semimajor axis ($a$), eccentricity ($e$) and inclination ($i$) \citep{Brozovic09}.  In this paper, we limit ourselves to studying the effects of varying a single initial condition with all other parameters fixed.  For reference initial conditions, we took the approximate mean values across the known irregular satellites:  $a_0 = 460 R_p$, $e_0 = 0.35$ and $i_0 = 155^{\circ}$---where in averaging we have excluded the single prograde irregular, Margaret, and the inclination is measured relative to the Uranian orbital plane \citep{Brozovic09}.  These values should not be taken as necessarily representative of the irregular satellite population over time, as collisions and gravitational perturbations would alter the distribution; rather, they were chosen as sensible (albeit somewhat arbitrary) values for comparison.  We chose a reference particle radius $s$ of $50 \mu$m, which is large enough to be only moderately affected by radiation pressure, and adopted a particle density equal to that of Saturn's irregular satellite Phoebe, the only irregular satellite for which a density has been directly determined ($\rho = 1.6 \text{g cm}^{-3}$, \citealt{Porco05}).

Taking the above parameters, we performed three suites of integrations, each of which varied a separate initial value.  The first sampled the observed range of irregular-satellite orbital eccentricities ($e_0  = $0.05, 0.2, 0.35, 0.5, 0.65).  The second spanned a range of inclinations $i_0$ ($5^{\circ}, 15^{\circ}, 25^{\circ}, 35^{\circ}, 145^{\circ}, 155^{\circ}, 165^{\circ}, 175^{\circ}$), and the last varied $s$ (10, 20, 30, 50, and $100 \mu$m).  We ignore the intermediate inclinations between $\approx 40-140^{\circ}$ that will undergo Kozai oscillations since the importance of their contribution is unclear, and our methods cannot adequately handle them.  The Kozai effect generates large-amplitude oscillations in the orbital eccentricity.  If its eccentricity amplitude is high-enough, an irregular satellite will collide with a regular satellite on a short timescale, preventing it from generating dust with similar orbital elements.  It is therefore unclear how much these satellites would contribute to the total dust budget.  The reason our methods cannot handle such orbits is that our assumption that the pericenter orientation is uniformly distributed between $[0,2\pi]$ becomes poor.  Beyond a critical inclination that depends on the initial eccentricity, new solutions appear where the pericenter orientation oscillates around a fixed value (librating solutions), whereas circulating solutions cycle at significantly non-uniform rates.  Nevertheless, as discussed in the next section, we expect the behavior of particles undergoing circulating Kozai cycles to match our high-eccentricity cases.

We then calculated the collision probabilities and leading/trailing ratios every 450 yrs.  This choice of timestep carefully samples the secular evolution ($\tau_\text{Sec} \sim 10^4 \text{yrs}$) and changing collision probabilities ($\tau_\text{Col} \sim 10^5 \text{yrs}$), though only captures the fast radiation-pressure induced evolution ($\tau_\text{RP} \sim 100$yrs) in an average sense.

We started all particles with values of zero for the longitude of ascending node (measured from Uranus' vernal equinox), argument of pericenter, and true anomaly.  While it is true that within a single integration the pericenter and relative node (with any given satellite) are roughly uniformly distributed, the chaotic dynamics in the unstable region mean that slightly different initial choices for these values will yield divergent evolution through the chaotic region.  Performing the collision probability calculations on orbital histories of initially nearby orbits would then yield different (but equally valid) results.  To try and capture this chaotic effect statistically, we instead varied the initial position of the Sun, which also determines the amplitude of the eccentricity oscillation induced by radiation pressure on the fast Uranian orbital timescale \citep{Burns79, Tamayo13}.  Thus, in addition to creating divergent orbital evolution through the chaotic region, this angle choice affects which inner moons can be reached at a given time by changing the amplitude of the fast eccentricity oscillation that is superimposed on the secular evolution.  For each of the eighteen combinations of orbital elements given above (five varying $e$, eight varying $i$ and five varying $s$), we ran integrations for sixteen equally-spaced initial solar positions, yielding a total of two hundred and eighty-eight orbital integrations.

\section{Results}
For each group of simulations, we plot the ratio of particles striking the leading vs. trailing hemispheres of each satellite, as well as the ``intrinsic" collision probability, defined as the probability of striking a particular moon divided by its total surface area.  To see why this might be a better indicator for the generation of hemispherical asymmetries than a total collision probability, imagine that the infalling dust had an equal probability of striking two moons.  The two satellites would therefore receive equal quantities of dust; however, if one moon were larger than the other, one would expect a larger effect on the smaller satellite since each area element on its surface is subject to a greater quantity of dust.  Normalizing the collision probabilities by the satellite surface areas therefore provides a better comparison.

The results can be qualitatively understood as arising from a competition between three different timescales.  The longest is the P-R timescale over which the semimajor axis (and therefore the pericenter distance) slowly decays.  In the geometric optics limit, this timescale varies linearly with particle size \citep{Burns79}, and for the Uranian system is $\tau_{\text{P-R}} \sim s \times 10^6$ yr, with $s$ in microns.  Next is the much faster secular timescale on which the eccentricity changes when the instablility is reached, $\tau_\text{Sec} \sim 10^4 \text{yrs}$.  Finally, $\tau_{\text{Col}}$ is the typical timescale on which a dust grain collides with a regular satellite once the particle's orbital pericenter dips below the moon's orbital radius, allowing collisions.  While the latter collision time depends on the particle's orbital elements, our numerical calculations show that $\tau_{\text{Col}} \sim 10^5 \text{yrs}$, intermediate between $\tau_\text{Sec}$ and $\tau_{\text{P-R}}$.

Figures \ref{e}a) and \ref{e}b) show two representative cases.  In \ref{e}a), the unstable zone is reached at $t \approx 20.5$ Myr, at which point the orbit's pericenter abruptly plunges inward and the particle strikes Uranus.  However, prior to that at $\sim 15$ Myr, the pericenter occasionally crosses the orbit of the outermost regular satellite Oberon, due to the large orbital eccentricities ($e_0$ = 0.65, which radiation pressure periodically drives even higher).  Then, the pericenter slowly drifts past Oberon on a timescale $\tau_{\text{P-R}} \gg \tau_{\text{Col}}$, allowing that satellite to sweep up most dust particles before they can reach the next moon Titania.  By contrast, in panel \ref{e}b), $e_0$ is low (0.05), and when the orbit reaches the unstable zone at $t \approx 24 Myr$, the pericenter still lies beyond Oberon's orbit.  On the short timescale $\tau_{\text{Sec}}$, the pericenter then plunges inside the orbit of several regular satellites, leading to a more equitable distribution of collision probabilities among the inner moons.

We expect that particles undergoing circulating Kozai cycles (not integrated), should roughly match the high ($e = 0.65$) case, concentrating most material on Oberon.  Kozai oscillations will periodically drive the eccentricity to high values, allowing the pericenter to cross Oberon's orbit prior to the semimajor axis reaching the unstable range, like in the $e=0.65$ case.  Librating solutions reach lower maximum eccentricities, so this case is more complicated.  It is unfortunately not clear what fraction of irregular satellites would be captured onto librating vs. circulating Kozai trajectories, or how significant the Kozai population is to the total budget of dust generated by the irregular satellites.  If the Kozai population is found to be important, one would have to use alternate methods to ours for the estimation of collision probabilities, \citep[e.g.,][]{Vok12}.

While panels \ref{e}a) and \ref{e}b) showed cases on the extremes of our initial eccentricity distribution, panel \ref{e}c) displays the combined results from all integrations varying $e_0$ (see caption description).  The intrinsic collision probability with Oberon (red) increases substantially for high initial eccentricities, due to the effect discussed in the previous paragraph.  At lower eccentricities, the distribution is more equitable due to the interaction of two factors.  On the one hand, all other aspects being equal, one would expect inner satellites to intercept more dust due to their higher orbital speeds.  Higher relative velocities lead to more frequent encounters between the moon and dust particles, providing more chances for collision.  On the other hand, all other aspects are {\it not} equal, due to the ``random" distribution of successive minima in the pericenter distance upon entering the unstable region (panel \ref{e}b).  A smaller fraction of these minima dip low enough to strike an inner moon than an outer one, leading to a fractionation of collision probability.  Finally, we note that orbital pericenters rarely dip low enough to reach Miranda.  As a result, the intrinsic collision probabilities with Miranda are always much smaller than those with the other moons, consistent with the non-detection of a hemispheric color asymmetry on Miranda by \cite{Buratti91}.
\begin{figure}[!ht]
\includegraphics[width=12cm]{fig3.eps}
\caption{\label{e}  Integrations varying $e_0$ (0.05, 0.2, 0.35, 0.5, 0.65) with $a_0 = 460 R_p$, $i_0 = 155^{\circ}$, and $s = 50\mu$m.  Panels a) and b) plot the pericenter distance vs. time for a typical orbit with $e_0 = 0.65$ and $e_0 = 0.05$, respectively.  The semimajor axes of the five regular satellites are plotted as horizontal lines, see the color legend on the figure's bottom left (used in all panels).  Panel c) shows the intrinsic collision probabilities with each target (total collision probability divided by satellite surface area) for the five values of $e_0$.  The bars over each value of $e_0$ are offset and arranged from left to right in order of increasing distance from Uranus.  Thus, Miranda (left) is in black, and Oberon (right) is in red.  Each of the five sets of bar graphs represents an average over sixteen equally spaced initial conditions for the solar position, and the error bars correspond to the standard deviation across those sixteen integrations.  Panel d) displays the ratio of material striking the leading vs. the trailing side of each satellite.}
\end{figure}

Panel \ref{e}d) plots the ratio of material striking the leading vs.\ trailing side of each moon.  With Uranus' equatorial plane nearly perpendicular to the ecliptic, it is not {\it a priori} clear what leading/trailing ratio one would expect, particularly since the instability also scatters the orbital inclination over a wide range.  The plotted values are averaged over the sixteen initial solar positions, weighted by their corresponding collision probabilities.  Thus, the leading/trailing ratio in an integration where Miranda receives 0.03$\%$ of dust matters proportionately less than that in a simulation where the collision probability is $3\%$.  The standard deviations are similarly weighted.  The calculated leading/trailing ratios range between $\approx 2-4$.  Our numerical calculations show a definite preference for material striking the leading sides of all the regular satellites.  This is mostly due to the fundamental asymmetry induced by the satellite's motion discussed in the introduction for IDPs and ISDPs.  It is analogous to the increase in rain striking a car's windshield at faster speeds through a storm.  The slight decrease in the leading/trailing ratio with satellite distance from Uranus seems to be a peculiarity of the chosen initial inclination ($i_0 = 155^{\circ}$), as revealed by our next set of integrations (Fig. \ref{i}d).

Figure \ref{i} shows our results upon varying the initial inclination.  Ignoring for a moment the curious behavior for $i_0 = 35^{\circ}$ in panel \ref{i}c), the collision probabilities do not seem to depend strongly on $i_0$, though systematic differences occur between prograde and retrograde orbits.  The distribution is more equitable for prograde particles, while for retrograde particles the intrinsic collision probabilities increase with the target's distance from Uranus.  This is due to a difference in the manner the chaotic region is approached, visible in panels \ref{i}a) and \ref{i}b).  For prograde particles (panel a), the orbital eccentricity spikes abruptly upon entering the unstable region, and the pericenter plunges.  The dust can thereby access all the moons on a single $\tau_\text{Sec}$, leading to a flatter probability distribution among the satellites.  By contrast, the eccentricities of retrograde particles undergo gradual growth as the chaotic regime is approached.  The pericenter distance is thereby often able to dip inside Oberon's orbit (panel \ref{i}b) prior to being exposed to the remainder of the moons, concentrating the collision probability on the outermost satellite.  We note that each individual excursion inside Oberon's orbit is significant since $\tau_\text{Col}$ is not much longer than $\tau_\text{Sec}$, the relevant timescale on which the eccentricity evolves.
\begin{figure}[!ht]
\includegraphics[width=12cm]{fig4.eps}
\caption{\label{i}  Integrations varying $i_0$ ($5^{\circ}, 15^{\circ}, 25^{\circ}, 35^{\circ}, 145^{\circ}, 155^{\circ}, 165^{\circ}, 175^{\circ}$) with $a_0 = 460 R_p$, $e_0 = 0.35$, and $s = 50\mu$m.  Panel a) shows the pericenter distance vs. time for a typical orbit in the prograde group with initial inclination $i_0 = 5^{\circ}$.  Panel b) shows a typical orbit in the retrograde group with $i_0 = 175^{\circ}$.  For an explanation of panels c) and d), see the caption to Fig. \ref{e}.  }
\end{figure}

The dynamical cause of this prograde/retrograde asymmetry is not clear.  Similarly curious is the high collisional likelihood on Oberon for $i_0 = 35^{\circ}$.  We find upon inspection of our integrations that at such high inclinations below, but approaching, the critical $i_0$ at which Kozai oscillations occur ($i_0 = 43.5^{\circ}$ for $e_0 = 0.35$), the system undergoes nearly regular Kozai-like oscillations prior to reaching the chaotic semimajor axis regime.  These high eccentricities bring the pericenter inside Oberon's orbit, but outside the orbital radii of the remaining moons, thus concentrating material on Oberon.  The same does not occur for highly inclined retrograde orbits.  An analysis of the dynamics in this rich and highly non-linear regime is beyond the scope of this paper.  Low-eccentricity orbits close to the equilibrium Laplace plane are treated by \cite{Tamayo13}.

As in the case varying $e_0$, the leading/trailing ratio $\approx 3$, independent of $i_0$ (panel d of Fig. \ref{i}).  There is no systematic trend with target distance from Uranus.

Figure \ref{s} shows our results for various grain sizes.  Smaller particles, more affected by radiation pressure, have larger-amplitude eccentricity oscillations ($\tau_\text{RP} \sim 100$ yrs) superimposed on their secular evolution.  Radiation pressure also shifts the position at which orbits become unstable \citep{Tamayo13}.  Panel c) shows that the collision probability distribution for 50 and $100\mu$m grains are qualitatively similar.  Due to the enhanced effects of radiation pressure, we find that the orbital eccentricities of 20 and $30\mu$m particles reach unity within one to a few $\tau_\text{Sec}$ of entering the unstable region (panel b), and they strike Uranus.  The available time for impact with satellites is thus drastically reduced.  While in all of the previously discussed cases the fraction of particles striking Uranus was $\lesssim 5\%$, approximately $30\%$ and $40\%$ of particles strike the planet in the $20 \mu$m and $30\mu$m cases, respectively.  For 10$\mu$m particles, and for some 20$\mu$m grains, the rapid eccentricity oscillations induced by radiation pressure ($\tau_\text{RP} \sim 100$ yrs) are of such large amplitude that for some initial solar positions the pericenter dips inside Oberon's orbit before the semimajor axis reaches the unstable region (see panel a).  This concentrates the probability distribution on the outermost satellite.  We note that, especially for the 10$\mu$m particles, the orbital behavior varies substantially across different initial solar positions.  The above statement nevertheless remains qualitatively valid.
\begin{figure}[!ht]
\includegraphics[width=12cm]{fig5.eps}
\caption{\label{s}   Integrations varying $s$ (0, 20, 30, 50, and $100 \mu$m) with $a_0 = 460 R_p$, $e_0 = 0.35$, and $i_0 = 155^{\circ}$.  Panel a) shows the pericenter distance history vs. time for a typical $10 \mu$m particle orbit.  Panel b) shows a typical $30 \mu$m grain orbit.  For an explanation of panels c) and d), see the caption to Fig. \ref{e}.}
\end{figure}

From panel d), one can see that the leading/trailing ratio remains $\approx 3$ for $s \gtrsim 30 \mu$m.  While we cannot simply explain the decreased asymmetry for smaller particles, it remains true that dust grains will preferentially strike the leading sides of the regular satellites.  We performed analogous integrations for prograde particles ($i_0 = 25^{\circ}$, not plotted) of varying sizes, and found the distributions to be qualitatively similar in all the respects discussed above, with the exception that the anomalously high leading/trailing ratio on Miranda for $30 \mu$m particles disappeared, and similar spikes occurred for Titania at $s=20\mu$m and Ariel at $s=50\mu$m.  In all cases, the standard deviations are large, so we do not believe them to be observationally important.

\section{Conclusion}
In this paper we have tried to find a mechanism capable of explaining the hemispherical asymmetries on the Uranian regular satellites found by \cite{Buratti91}.  We argued that various sources beyond the Uranian system and magnetospheric effects are either incapable of producing leading/trailing differences, or in cases where they might create asymmetries, that the effect should be largest for the inner satellites.  This predicted trend is opposite to what is observed.  Innermost Miranda has no detectable asymmetry, and hemispherical differences grow with semimajor axis for the outer four moons \citep{Buratti91}.

We then investigated the dynamics of infalling dust from the irregular satellites as a possible mechanism.  This process is complicated by the fact that Uranus' extreme obliquity causes chaotic large-amplitude variations in particles' orbital eccentricity and inclination over a range of semimajor axes \citep{Tremaine09, Tamayo13}.  We found that:  (i) dust reaches the outermost four satellites, contrary to the expectation (in the absence of this dynamical instability) that the vast majority of dust would be concentrated on the outermost moon Oberon, (ii) dust-orbit pericenters rarely reach the semimajor axis of Miranda, consistent with the fact that this innermost moon shows no hemispherical asymmetry (cf. panel c of Figs. \ref{e}-\ref{s}), (iii) for retrograde dust particles, the intrinsic collision probability with each satellite tends to increase with semimajor axis (panel c of Figs. \ref{e}-\ref{s}), and (iv) despite the unusual Uranian geometry and the fact that the mentioned instability leads to chaotically varying orbital inclinations, approximately three times more dust strikes the leading hemispheres of each of the regular satellites than their respective trailing hemispheres, independent of initial conditions ($\approx 2$ times for the smallest dust grains); see panel d) of Figs. \ref{e}-\ref{s}.

We point out that not all initial conditions generate collision probabilities that increase with the semimajor axis of the target satellite.  Most notably, only retrograde particles with moderate-to-high orbital eccentricity do.  The directionality fits well with the fact that retrograde irregular satellites are more dynamically stable than prograde moons and are therefore longer-lived \citep{Carruba02, Nesvorny07}.  Today, out of nine known Uranian irregulars, only Margaret is prograde.  The eccentricity requirement does not preclude a population of low-eccentricity impactors (that would tend to produce comparable color asymmetries across the satellites)---it only requires that a significant fraction of the dust population be born on moderate-to-high eccentricity orbits to produce the trend.  If the current irregular satellite orbital eccentricity distribution is any indicator of this historical average, this seems plausible.

We therefore conclude that, despite the uncertainties, infall of dust from the irregular satellites furnishes the best explanation for the color asymmetries on the Uranian regular satellites.  If this hypothesis is correct, it implies that the lifetimes of dust grains orbiting Uranus at large semimajor axes ($\sim 100 R_p$) are much longer ($\gtrsim 10$ Myr) than in typical planetary magnetospheres.  It would also require that irregular-satellite dust infall overwhelm the flux from sources that would generate the opposite trend with semimajor axis, in particular, IDPs.  The flux of IDPs over the Solar System's history is quite uncertain, but one can obtain a rough lower limit for the total interplanetary dust mass intercepted by the Uranian satellites by extrapolating the current flux backward in time.  Using estimates for the current flux of IDPs in the outer Solar System by \cite{Cuzzi98}, this demands a dust mass generated by the irregulars $\gtrsim 10^{14}$kg over the system's history.  While no current dust ring associated with the irregular satellites has been detected thus far around Uranus, the production of dust through mutual collisions between irregulars should have been been strongly concentrated in the first few hundred Myr after the capture of the irregular satellites \citep{Bottke10}.  An analogous diffuse dust ring has been discovered around Saturn with the Spizer Space Telescope; it is generated by the irregular satellite Phoebe \citep{Verbiscer09}.  This Phoebe ring has an estimated mass $\sim 3$ orders of magnitude smaller than our lower limit of $10^{14}$ kg.  Thus, if our hypothesis is correct, the irregular satellites must have generated a substantial amount of dust in the past.

\section{Acknowledgements}
We thank Philip Nicholson, Matthew Hedman, Matthew Tiscareno, and Rebecca Harbison for their insightful comments.  This work was supported by the Cassini project and NASA's Planetary Geology and Geophysics Program.

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redpajama_set_name: RedPajamaArXiv


text:
Federico Dennerlein dit Fritz (né le  à Portici, mort le  à Naples) est un nageur, joueur de water-polo et entraîneur italien.

Biographie
Fritz Dennerlein est de père allemand et de mère roumaine mais n'a eu que la nationalité italienne. Il a établi 5 records européens de natation en papillon de 1959 à 1962. Il est mort à la suite d'un accident de circulation et est enterré au  Cimitero acattolico di Santa Maria delle Fede, le cimetière anglais de Naples.
La piscine de la Mostra d'Oltremare porte son nom.

Notes et références

Liens externes

Joueur italien de water-polo
Nageur italien
Entraîneur italien de water-polo
Nageur aux Jeux olympiques d'été de 1960
Joueur de water-polo aux Jeux olympiques d'été de 1964
Membre de l'International Swimming Hall of Fame
Naissance à Portici
Naissance en mars 1936
Personnalité italienne née d'un parent allemand
Personnalité italienne née d'un parent roumain
Décès à Naples
Décès en octobre 1992
Décès à 56 ans


text:
« Screening room
JANET MARRETT
Original Title: KINDRED
Spanish Title: FAMILIA
English Title: KINDRED
Year and month of production: 2019
Production country: United Kingdom
Subtitles: Spanish, English, French, Italian, German
Trailer (link): https://vimeo.com/292076345
Web: https://mediathirsty.co.uk
Facebook: https://www.facebook.com/mediathirsty/
KINDRED is a beautiful and heart-warming realist drama of Esther, a UK woman of Nigerian heritage. In a serious predicament Esther is forced to reconcile a bitter 8 year rift with her family.
Janet is the founder of Mediathirsty and is experienced writing, directing and producing independent films. Janet has successfully produced film projects over the past ten years. Internationally her work has been shown in Singapore, Kuwait, Spain, Luxembourg, Belgium, France, Ghana and the USA. Janet is passionate about featuring diverse ethnicities on film. A huge fan of realist dramatic styles, she is inspired by Writer/Directors Asghar Farhadi, Mahamat-Saleh Haroun, Barry Jenkins, Amma Asante, Céline Sciamma, Nadine Lebaki, Bong Joon-Ho and Andrea Arnold amongst many others. She completed her second independent short CLEARING in 2020, starring BAFTA-nominated Jasmine Jobson from Netflix's Top Boy, which is included in Cannes Court Métrage Short Film Corner and is set to tour the international festival circuit. Her first short KINDRED was well-received internationally, winning a Gold REMI in Houston, Texas and appearing on the winners list for the People of Color: The International Cultural Exchange, New York. It also screened at international festivals in the UK, Africa & USA. Janet is currently developing a slate of future projects. She was shortlisted then selected for the 2019 B3 Media TalentLab Showcase and completed the 2020 Film London Feature Screenwriting Lab.
Crystal Palace International Film Festival, London, UK
WorldFest Houston International Film Festival, Houston Texas, USA
Women of African Descent Crystal Palace International, Brooklyn, New York, USA
British Urban Film Festival, London UK
CPIFF Black Lives Matter, London UK
People of Color: The International Cultural Exchange, Ny, New York, USA
Accra Indie FilmFest, Accra, Ghana
Gold REMI Award - WorldFest Houston International Film Festival, Houston Texas, USA


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