Wadah Titian Harapan celebrated its 5th Anniversary on 28 January 2013 at the Intercontinental Jakarta Midplaza Hotel. This simple celebration was attended by various social women activists and assisted community members of Wadah.
Ms. Retnaning Tyas, chairperson of Wadah, gave a presentation on what has been done by the foundation in the last five years, prticularly in 2012. Ibu Tyas also presented programs for 2013 as the beginning of the second five-year plan of Wadah activities.
Meanwhile, Ibu Anie Hashim Djojohadikusumo, patron of Wadah, introduced a "new" set of Wadah advisers and executives to run various programs of Wadah.
In the face of challenging years ahead and to maximize services to the needy, Wadah has made some changes in its vision, mission and strategy. To get more thorough information on how Wadah plans to move in the future, please see Wadah presentation slides.


The holiday season is upon us, and most homeowners are going away for a few days. Most locations across the globe experience heavy winter frost and snow, so it's important that you don't leave without taking care of your plumbing. Forgetting something simple such as keeping your heating turned on or taking care of your water heater before leaving can result in a messy situation.
1. Though it may seem rather counterproductive to leave your heat on while you're away, it's important to do so. During the winter and early spring months, the frigid cold can freeze your plumbing pipes while your home is not in use. This issue can be avoided by setting your thermostat to 60 degrees and leaving it on while you're away. Frozen plumbing pipes can sometimes be defrosted, but more often than not, they need to be replaced– that can be costly!
2. Your water heater can also be a silent culprit in prolonging your potential plumbing nightmares. Before going on a holiday, make sure that you check your water heater to ensure there's no water on the floor. If you find a small leak or puddle near the water heater, you should call a plumber right away as your water heater will need to be replaced.
Hopefully, you won't find any problems before heading off on your vacation. However, it's best to play it safe and turn off your water heater. Doing so can prevent it from working unnecessarily and should your electricity get turned off, it won't cause the water heater to malfunction.
3. Odors are a result of clogged drain pipes. Don't go on vacation without doing a bit of DIY plumbing pipe maintenance. There are some household chemicals that you can pour down your drains to help break up the particles causing odors and potential clogging. Additionally, make sure to remove manually hair from the surface of your bathtub drain and get rid of food particles that may be clogging your garbage disposal.
Leaving home without caring for your plumbing can make the odors worse, and it can also cause sludge buildup. If you want to play it completely safe, hire a plumber to perform optimal drain cleaning.
4. If you actively use your washing machine, make sure to check it over as well. A washing machine hose has a life expectancy of about three years before you need to go ahead and install a new one. It's wise not to go on vacation without replacing the old one if it has hit the three-year mark. Not taking care of this problem can cause the machine to malfunction!
5. Is there something wrong with your plumbing right now? There's always the possibility that you know there's something wrong with your plumbing. Never go on vacation without having any potential problems fixed. Waiting until you get back from your travels can make the problem worse, and having to hire an emergency plumber like bestportlandplumbers.com can be infinitely more expensive.
6. Shut off the water supply leading to your toilet. In the case of an emergency, while you're away, the amount of water that gets released back into your toilet will be minimal. Additionally, there's no possibility of your toilet getting clogged while you're not at home.
7. If you have an active sprinkler system or use an outdoor water supply on a regular basis, it's best to shut it off while on vacation. Sometimes, homeowners can be absentminded in all of the excitement, therefore, forgetting that their sprinkler system is turned on. Of course, this is most often the case in areas where the weather is fairly warm and sunny year round.
Not only can you save a great deal of money on your utility bill, but it prevents from any potential plumbing problems from getting worse. If your yard needs constant care, have a neighbor or family member do the watering regularly.
8. You may be taking your refrigerator for granted, and if you have a built-in icemaker or filtration system, it could be plumbing trouble if you're not paying attention. Before heading out, make sure to pull your fridge away from the wall and give it a thorough inspection. It's best to unplug your fridge and remove food if you're going to be gone for a long time. However, if you're only leaving for a few days, just make sure to leave your fridge in good working condition.
Most homeowners have found it helpful to make a checklist of the different plumbing things they need to take care of. Before heading off on vacation, look around your house and check the things highlighted on your list. Many homeowners don't do this, and you can end up spending hundreds or even thousands of dollars on a plumber because of your mistake.
The tips highlighted above are also reasonable to use if you're traveling during the summer months of the year as well. Instead of cranking up the thermostat and setting your heater on, just leave your air conditioning running on the thermostat. It's very important that your home remains at room temperature as it can prevent your furnishings from getting ruined as well as your plumbing.
When in doubt, you can shut off your entire water supply and turn it on again when you get home. This is the best course of action to choose if you're going to be gone for some time, and it can help save you money in terms of utility bills and potential plumbing problems. If you encounter any problems, make sure to call a professional local plumber for help!


Size 5/8" 3/8" SPECIAL OFFER 5/8" & 3/8"
Easily spot these bright handled chisels on any work site. Fitted with resilient plastic handles. These chisels come in two sizes, a 5/8" and a 3/8", we offer a special price if purchased together. Select it in the drop down menu.


Herbs For Health is located at the address 101 Woods Cove Rd in Scottsboro, Alabama 35768. They can be contacted via phone at (256) 259-3821 for pricing, hours and directions.
For maps and directions to Herbs For Health view the map to the right. For reviews of Herbs For Health see below.


text:
Canaxır è un comune dell'Azerbaigian situato nel distretto di Xaçmaz. Conta una popolazione di 682 abitanti.

Collegamenti esterni
Canaxır su GEOnet Names Server

Comuni del distretto di Xaçmaz

redpajama_set_name: RedPajamaWikipedia


How well a patient recovers after having a stroke is directly linked to the quality of medical care the person receives after leaving the hospital, says Michael Frankel, MD, professor of neurology at the Emory University School of Medicine, and chief of neurology at Grady Memorial Hospital in Atlanta. Thanks to a recent $500,000 grant from the Association of American Medical Colleges and the Centers for Disease Control and Prevention, Dr. Frankel and other researchers will soon learn more about how well patients recover after a stroke, their quality of life, and ways to improve outcomes after hospitalization.
The grant is specifically designed to study stroke outcomes, track information, and improve quality of life for stroke survivors. According to the American Stroke Association, stroke occurs when a blood vessel that carries oxygen and nutrients to the brain is either blocked by a clot or bursts. When that happens, part of the brain cannot get the blood (and oxygen) it needs, so it starts to die.
Emory University was the only site in the country selected to spearhead the two-year study. Based at Grady Hospital, the project will focus on ongoing data collection to help improve quality of care for study participants. Overall, Dr. Frankel hopes that hospitals across the country will use newly developed online tool to improve care for patients after stroke discharge.
"This is a groundbreaking study because no one has ever created a prototype tool for data collection to improve the quality of stroke care after hospital discharge," says Dr. Frankel, principal investigator of the project. "This project is focused on post-hospital care that including inpatient rehabilitation, medical care, functional recovery, medication adherence, and quality of life and survival."
Dr. Frankel plans to enroll 1,000 patients in the study. Patients will be followed for one year by telephone and office visits. Along with Grady, University Hospital in Augusta and Candler and St. Joseph's hospitals in Savannah will participate in follow-up care by identifying stroke patients and enrolling them into the study. The goal is for all four hospitals, which represent approximately 10 percent of the stroke patient population throughout the state, to contribute to the same database and create quality improvements.
"One of the other aspects that we're going to focus on is whether or not there are racial differences in stroke outcomes," Dr. Frankel adds. "We will look at racial and socioeconomic differences in outcomes after stroke. We hope to learn a bit more about why those differences exist so that we can improve the care in communities that are disproportionately affected by stroke."
Dr. Frankel hopes that with more frequent contact after discharge, patients will learn to adhere to medical therapy and follow up with their physicians through clinical appointments.
"We realize that there is a continuum of care that goes beyond the hospital period," he says. "This project is the first attempt at linking what happened in the hospital with what happens after patients are discharged to assure good continuity and quality of care."
According to the American Stroke Association, stroke is the nation's No. 3 killer and a leading cause of severe, long-term disability. Every 45 seconds, someone in America has a stroke. The ASA estimates that approximately 700,000 Americans will have a stroke this year.


text:
Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients
D. J. Kilmartin, D. W. Wilson, Janet Mary Liversidge, A. D. Dick, J. Bruce, R. W. Acheson, Stanislaw Urbaniak, John Vincent Forrester
Applied Medicine
Background/aims-Sympathetic ophthalmia (SO) is a classic example of autoimmune disease where human leucocyte antigen (HLA) genomic associations could provide further understanding of mechanisms of disease. This study sought to assess HLA genetic polymorphism in British and Irish patients with SO, and to assess whether HLA gene variants are associated with clinical phenotype or disease severity.
Methods-High resolution DNA based HLA typing using polymerase chain reaction sequence specific primers was performed in 27 patients with SO and 51 matched healthy controls. Clinical phenotype and markers of disease severity were determined prospectively in 17 newly diagnosed patients and from medical record review and repeat clinical examination in 10 previously diagnosed patients.
Results-HLA-Cw*03 (p=0.008), DRB1*04 (p=0.017), and DQA1*03 (p=0.014) were significantly associated with SO. For class IT alleles at higher resolution, only HLA-DRBl*0404 (relative risk (RR) = 5.6, p = 0.045) was significantly associated with SO. The highest relative risk for any of the associated haplotypes was with HLA-DRB1*0404-DQA1*0301 (RR=10.9, p = 0.019). Patients with the DRB1*04-DQA1*03 associated haplotype were significantly more Likely to develop SO earlier, with fewer inciting ocular trauma events, and to require more systemic steroid therapy to control inflammatory activity.
Conclusions-Sympathetic ophthalmia is associated with HLA-DRB1*04 and DQA1*03 genotypes in white patients, similar to Japanese patients. Differences in DRB1*04 gene variant associations (-0404 in Britain and Ireland and -0405 in Japan) may have implications for HLA peptide binding in disease initiation. The DRB1*04-DQA1*03 haplotype is a marker of increased SO susceptibility and severity, as in Vogt-Koyanagi-Harada disease, which also has similar clinicopathological and HLA associations.
https://doi.org/10.1136/bjo.85.3.281
KOYANAGI-HARADA DISEASE
RHEUMATOID-ARTHRITIS
T-CELLS
10.1136/bjo.85.3.281
Kilmartin, D. J., Wilson, D. W., Liversidge, J. M., Dick, A. D., Bruce, J., Acheson, R. W., Urbaniak, S., & Forrester, J. V. (2001). Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients. British Journal of Ophthalmology, 85(3), 281-286. https://doi.org/10.1136/bjo.85.3.281
Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients. / Kilmartin, D. J.; Wilson, D. W.; Liversidge, Janet Mary; Dick, A. D.; Bruce, J.; Acheson, R. W.; Urbaniak, Stanislaw; Forrester, John Vincent.
In: British Journal of Ophthalmology, Vol. 85, No. 3, 2001, p. 281-286.
Kilmartin, DJ, Wilson, DW, Liversidge, JM, Dick, AD, Bruce, J, Acheson, RW, Urbaniak, S & Forrester, JV 2001, 'Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients', British Journal of Ophthalmology, vol. 85, no. 3, pp. 281-286. https://doi.org/10.1136/bjo.85.3.281
Kilmartin DJ, Wilson DW, Liversidge JM, Dick AD, Bruce J, Acheson RW et al. Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients. British Journal of Ophthalmology. 2001;85(3):281-286. https://doi.org/10.1136/bjo.85.3.281
Kilmartin, D. J. ; Wilson, D. W. ; Liversidge, Janet Mary ; Dick, A. D. ; Bruce, J. ; Acheson, R. W. ; Urbaniak, Stanislaw ; Forrester, John Vincent. / Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients. In: British Journal of Ophthalmology. 2001 ; Vol. 85, No. 3. pp. 281-286.
@article{4f748a7d11dc4cbba3c74826f837d4b1,
title = "Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients",
abstract = "Background/aims-Sympathetic ophthalmia (SO) is a classic example of autoimmune disease where human leucocyte antigen (HLA) genomic associations could provide further understanding of mechanisms of disease. This study sought to assess HLA genetic polymorphism in British and Irish patients with SO, and to assess whether HLA gene variants are associated with clinical phenotype or disease severity.Methods-High resolution DNA based HLA typing using polymerase chain reaction sequence specific primers was performed in 27 patients with SO and 51 matched healthy controls. Clinical phenotype and markers of disease severity were determined prospectively in 17 newly diagnosed patients and from medical record review and repeat clinical examination in 10 previously diagnosed patients.Results-HLA-Cw*03 (p=0.008), DRB1*04 (p=0.017), and DQA1*03 (p=0.014) were significantly associated with SO. For class IT alleles at higher resolution, only HLA-DRBl*0404 (relative risk (RR) = 5.6, p = 0.045) was significantly associated with SO. The highest relative risk for any of the associated haplotypes was with HLA-DRB1*0404-DQA1*0301 (RR=10.9, p = 0.019). Patients with the DRB1*04-DQA1*03 associated haplotype were significantly more Likely to develop SO earlier, with fewer inciting ocular trauma events, and to require more systemic steroid therapy to control inflammatory activity.Conclusions-Sympathetic ophthalmia is associated with HLA-DRB1*04 and DQA1*03 genotypes in white patients, similar to Japanese patients. Differences in DRB1*04 gene variant associations (-0404 in Britain and Ireland and -0405 in Japan) may have implications for HLA peptide binding in disease initiation. The DRB1*04-DQA1*03 haplotype is a marker of increased SO susceptibility and severity, as in Vogt-Koyanagi-Harada disease, which also has similar clinicopathological and HLA associations.",
keywords = "KOYANAGI-HARADA DISEASE, RHEUMATOID-ARTHRITIS, T-CELLS, HLA, ASSOCIATION, UVEITIS, GENES, GAMMA",
author = "Kilmartin, {D. J.} and Wilson, {D. W.} and Liversidge, {Janet Mary} and Dick, {A. D.} and J. Bruce and Acheson, {R. W.} and Stanislaw Urbaniak and Forrester, {John Vincent}",
doi = "10.1136/bjo.85.3.281",
journal = "British Journal of Ophthalmology",
T1 - Immunogenetics and clinical phenotype of sympathetic ophthalmia in British and Irish patients
AU - Kilmartin, D. J.
AU - Wilson, D. W.
AU - Liversidge, Janet Mary
AU - Dick, A. D.
AU - Bruce, J.
AU - Acheson, R. W.
AU - Urbaniak, Stanislaw
AU - Forrester, John Vincent
N2 - Background/aims-Sympathetic ophthalmia (SO) is a classic example of autoimmune disease where human leucocyte antigen (HLA) genomic associations could provide further understanding of mechanisms of disease. This study sought to assess HLA genetic polymorphism in British and Irish patients with SO, and to assess whether HLA gene variants are associated with clinical phenotype or disease severity.Methods-High resolution DNA based HLA typing using polymerase chain reaction sequence specific primers was performed in 27 patients with SO and 51 matched healthy controls. Clinical phenotype and markers of disease severity were determined prospectively in 17 newly diagnosed patients and from medical record review and repeat clinical examination in 10 previously diagnosed patients.Results-HLA-Cw*03 (p=0.008), DRB1*04 (p=0.017), and DQA1*03 (p=0.014) were significantly associated with SO. For class IT alleles at higher resolution, only HLA-DRBl*0404 (relative risk (RR) = 5.6, p = 0.045) was significantly associated with SO. The highest relative risk for any of the associated haplotypes was with HLA-DRB1*0404-DQA1*0301 (RR=10.9, p = 0.019). Patients with the DRB1*04-DQA1*03 associated haplotype were significantly more Likely to develop SO earlier, with fewer inciting ocular trauma events, and to require more systemic steroid therapy to control inflammatory activity.Conclusions-Sympathetic ophthalmia is associated with HLA-DRB1*04 and DQA1*03 genotypes in white patients, similar to Japanese patients. Differences in DRB1*04 gene variant associations (-0404 in Britain and Ireland and -0405 in Japan) may have implications for HLA peptide binding in disease initiation. The DRB1*04-DQA1*03 haplotype is a marker of increased SO susceptibility and severity, as in Vogt-Koyanagi-Harada disease, which also has similar clinicopathological and HLA associations.
AB - Background/aims-Sympathetic ophthalmia (SO) is a classic example of autoimmune disease where human leucocyte antigen (HLA) genomic associations could provide further understanding of mechanisms of disease. This study sought to assess HLA genetic polymorphism in British and Irish patients with SO, and to assess whether HLA gene variants are associated with clinical phenotype or disease severity.Methods-High resolution DNA based HLA typing using polymerase chain reaction sequence specific primers was performed in 27 patients with SO and 51 matched healthy controls. Clinical phenotype and markers of disease severity were determined prospectively in 17 newly diagnosed patients and from medical record review and repeat clinical examination in 10 previously diagnosed patients.Results-HLA-Cw*03 (p=0.008), DRB1*04 (p=0.017), and DQA1*03 (p=0.014) were significantly associated with SO. For class IT alleles at higher resolution, only HLA-DRBl*0404 (relative risk (RR) = 5.6, p = 0.045) was significantly associated with SO. The highest relative risk for any of the associated haplotypes was with HLA-DRB1*0404-DQA1*0301 (RR=10.9, p = 0.019). Patients with the DRB1*04-DQA1*03 associated haplotype were significantly more Likely to develop SO earlier, with fewer inciting ocular trauma events, and to require more systemic steroid therapy to control inflammatory activity.Conclusions-Sympathetic ophthalmia is associated with HLA-DRB1*04 and DQA1*03 genotypes in white patients, similar to Japanese patients. Differences in DRB1*04 gene variant associations (-0404 in Britain and Ireland and -0405 in Japan) may have implications for HLA peptide binding in disease initiation. The DRB1*04-DQA1*03 haplotype is a marker of increased SO susceptibility and severity, as in Vogt-Koyanagi-Harada disease, which also has similar clinicopathological and HLA associations.
KW - KOYANAGI-HARADA DISEASE
KW - RHEUMATOID-ARTHRITIS
KW - T-CELLS
KW - HLA
KW - ASSOCIATION
KW - UVEITIS
KW - GENES
KW - GAMMA
U2 - 10.1136/bjo.85.3.281
DO - 10.1136/bjo.85.3.281
JO - British Journal of Ophthalmology
JF - British Journal of Ophthalmology

redpajama_set_name: RedPajamaCommonCrawl


text:
You don't need me to tell you these are hard times. The pandemic is getting worse and, while we can optimistically anticipate widespread distribution of coronavirus vaccines in coming months, we still have to get through the winter and early spring. We will feel a sense of loss during the holidays.
We can still give to charity, which typically gets more attention toward year-end. The surge in giving partly reflects the holiday spirit and partly the rules of the tax code. Taxpayers who itemize can deduct their charitable donations from their taxable income. To be sure, tax-law changes that went into effect in 2018 sharply reduced the number of itemizers by roughly doubling the standard deduction. Still, whether you itemize or not, giving remains incredibly important with so many people suffering during the pandemic.
A special provision allows individuals to deduct cash donations of up to $300 if made to qualifying charities before Dec. 31. The deduction is part of last spring's fiscal-relief package, the Coronavirus Aid, Relief and Economic Security (CARES) Act.
Nearly nine in 10 taxpayers take the standard deduction, according to the IRS and they could potentially qualify for this new tax deduction for 2020. The deduction lowers both adjusted gross income and taxable income — a (small) tax savings. The donations must be made by cash, check, credit card or debit card to a qualified charitable institution.
You should send the money to the charitable organization(s) of your choice, of course. But many small local charities are finding it hard to serve their mission. The pandemic revealed how valuable are small locally owned businesses to the vibrancy of our neighborhoods. The same goes with small local nonprofits. Typically founded by a social entrepreneur and staffed with dedicated people, these organizations are deeply embedded into the fabric of our local communities.
By the way, for those who do itemize even after the tax law changes, the CARES Act also allows you to deduct charitable contributions of up to 100% of adjusted gross income in 2020. That's up from 60% in current law.
There are many ways to give, ranging from donor-advised funds to cash. Whatever strategy works for you, thinking about where to give your money helps define what really matters to you and how you would like to help make the world a better place. Isn't that the goal of personal finance? I think so.
Chris Farrell is senior economics contributor for "Marketplace" and Minnesota Public Radio.
Chicago teachers began voting Thursday to defy orders to report for in-person class next week ahead of elementary students' return, actions the nation's third-largest school district said could lead to "an illegal strike."


Understanding organizational culture and why change is difficult.
Analyzing current versus desired culture and identifying gaps.
The six stages of change management.
Assessing your company's readiness for change.
Ways to successfully implement change and manage resistance to it.
This course is designed for human resources, total rewards and work-life professionals along with business leaders with an interest in or responsibility for work-life programs.It is a required course for the Work-Life Certified Professional certification. The course includes real-world case studies and examples that provide practical application in organizational change management. It is a required course for the Work-Life Certified Professional certification. The course includes real-world case studies and examples that provide practical application in organizational change management.
Define organizational culture and understand how it is formed within an organization. Learn why culture is difficult to change and the realities of trying to change it.
Learn to diagnose the current organizational culture, define the desired culture and perform a gap analysis.
Learn the six stages of change and assess organizational readiness.
Prepare to plan for change, manage change and reinforce it.
Upon completing this work-life course on organizational culture change, you will have new insights on how to manage change within your organization within the area of work-life.
Ready to learn more about organizational culture change?
This course is intended for human resources, total rewards and work-life professionals as well as business leaders with an interest in and/or responsibility for work-life programs designed to attract, motivate and retain employees.
1. Which of the following best describes organizational culture?
2. Which of the following has the most significant influence on the formation of an organization's culture?
3. Which of the following best describes why it is so difficult to change organizational culture?
4. Which of the following is key to look at when diagnosing the organization's current culture?
5. Which of the following must be done when defining the desired culture?
6. What is the desired outcome of a gap analysis?
7. Which of the following best describes the contemplation stage of change?
8. Why is it helpful to understand the stages of the change readiness model?
A. It helps determine the decision-maker's openness and motivation to support change.
B. It points out how to overcome resistance to change.
C. It provides a step-by-step process for facilitating change.
D. It describes how to motivate people to change.
9. Why is it important to create a sense of urgency when planning for change?
A. It catches the attention of stakeholders when it's shown how change will result in either avoiding a great loss or adding great value.
B. It helps identify key stakeholders more quickly and effectively.
C. It allows for change agents to pilot programs early on.
D. It results in a business case that will be approved and supported by all.
10. Which of the following is most accurate when planning to communicate the change?
It helps determine the decision-maker's openness and motivation to support change.
It points out how to overcome resistance to change.
It provides a step-by-step process for facilitating change.
It describes how to motivate people to change.
It catches the attention of stakeholders when it's shown how change will result in either avoiding a great loss or adding great value.
It helps identify key stakeholders more quickly and effectively.
It allows for change agents to pilot programs early on.
It results in a business case that will be approved and supported by all.


What are "flash crowds" and how do we recruit them?
Our bread and butter working with clients is organizing their employees to participate in crowdsourcing exercises. Recently we have been approached more to help get forecasts from external crowds, either to support research projects, or to better understand what outside experts or customers think.
Register an account for Cultivate Forecasts mobile directly in the app.
Creating a logo for a company can be a daunting task. In this post our Creative Director, Jessica Price explains how we landed on the final logo for Cultivate Labs.
Two key take-aways from the emerging scandal surrounding Daily Fantasy sites: one, gambling data can be extremely valuable, and two: the only thing Americans love more than gambling is hating on gambling. Taken together, these findings illustrate why large-scale prediction markets present a path towards improving human knowledge in a wide range of topics.


text:
Упразднённые муниципальные районы, как муниципальные образования, ранее существовавшие в России, представлены в списке ниже.

В некоторых регионах упразднение муниципальных районов сопровождается преобразованиями на административно-территориальном уровне (обозначены в комментариях и примечаниях).

На 2021 год полностью упразднены муниципальные районы Калининградской, Магаданской, Московской, Сахалинской областей и Ставропольского края, на 2023 год - Удмуртии, Пермского края и некоторых других регионов.

Список районов

Список районов разделён на четыре группы в их хронологической последовательности:

 упразднённые до 2003 года, до проведения муниципальной реформы;
 упразднённые в 2004—2009 годах, в ходе основного этапа реформы;
 упразднённые в 2010—2019 годах, после основного этапа реформы;
 упразднённые (упраздняемые) в 2019—2023 годах с введением нового вида муниципального образования — муниципального округа.

В комментариях указываются, если были, сопутствовавшие административно-территориальные преобразования.

В примечаниях указываются информация о последовавших преобразованиях и иного рода дополнительные сведения.

Остальные муниципальные районы предполагается упразднить в период 2023—2028 годов.

Районы, упразднённые до проведения муниципальной реформы

Муниципальные образования, официально называвшиеся районами, упразднённые до 2003 года, то есть до проведения реформы местного самоуправления.

Районы, упразднённые в ходе муниципальной реформы
наверх к оглавлению

Районы, упразднённые в 2004—2009 годах, во время основного этапа муниципальной реформы.

В это время были сформированы муниципальные образования современного типа:
 муниципальные образования, официально называвшиеся районами, как правило, получили наименование муниципальных районов;
 внутрирайонные муниципальные образования всех видов были преобразованы в городские и сельские поселения
 в составе трёх муниципальных районов сельские и городские поселения образованы не были — до настоящих дней из всех трёх районов сохранён Северо-Енисейский Красноярского края;
 муниципальные наименования, официально называвшиеся городами и посёлками, как правило, были преобразованы в городские округа;
 за исключением муниципальных образований города федерального значения Санкт-Петербурга;
 внутригородские муниципальные образования городов федерального значения были сохранены;
 все внутригородские муниципальные образования в городах, не являвшихся городами федерального значения (районы и округа в том числе), были упразднены;
 уникальные муниципальные образования были также упразднены (муниципальные округа Ярославской области были преобразованы в муниципальные районы, Вепсская национальная волость Карелии была присоединена к Прионежскому муниципальному району).

Преобразование района в городской округ в 2004—2005 годах могло происходить двумя путями:
 муниципальное образование со статусом района было сразу в ходе реформы наделено статусом городского округа — такие районы отмечены звёздочкой (*);
 муниципальное образование со статусом района (также, реже, города) было наделено статусом муниципального района, а в дальнейшем муниципальный район был преобразован в городской округ либо объединён с другим муниципальным образованием (районом или городским округом).

Преобразование муниципального района в городской округ означало упразднение всех входящих в район сельских и городских поселений, а фактически (что иногда декларировалось) наделение городского поселения статусом городского округа и присоединение к нему всех других поселений (официальное определение городского округа было — городское поселение, не входящее в состав муниципального района).

Муниципальные районы, упразднённые в 2010—2019 годах
наверх к оглавлению

Муниципальные районы, упразднённые после проведения основного этапа муниципальной реформы до введения 1 мая 2019 года нового вида муниципального образования — муниципального округа.

Муниципальные районы, упразднённые с 1 мая 2019 года
наверх к оглавлению

Муниципальные районы, упразднённые после утверждения нового вида муниципального образования — муниципального округа. После введения муниципального округа преобразование муниципальных районов в городские округа было практически приостановлено, кроме того, в муниципальные округа начали преобразовываться муниципальные районы без городского населения.

См. также
 Муниципальный район (Россия)
 Упразднённые городские округа Российской Федерации
 Упразднённые районы субъектов Российской Федерации

Примечания

 Комментарии

Ссылки

 Стратегии регионов по наделению муниципальных образований статусом городского округа

Упразднённые муниципальные районы России


text:
Anna Kwaśny
"Next we drove into the city of Mirebalais to see the new hospital run by PIH and the Haitian government. I was blown away. The hospital opened last summer and was built using money donated after the 2010 earthquake (people who were injured in the quake still need ongoing treatment). They spared no expense to make it a first-class facility. There's a machine for performing CAT scans. There's a sophisticated system for keeping medical records. The staff can send digital images to Harvard and get input from specialists there."
These are the words of Bill Gates, commenting on his trip to Haiti in 2014 (read the full article here). The place he described is called University Hospital of Mirebalais and, as mentioned above, it was opened by Partners in Health and Haitian government.
The sophisticated system for keeping records is OpenMRS, which served as great help and support in the process of rebuilding and improving the healthcare standards in Haiti. In this article we will introduce you to the case study of OpenMRS' implementation in the Haitian hospital.
University Hospital of Mirebalais
In 2010 Haiti was hit by a massive earthquake, the biggest since the 18th century. Thousands of people have lost their lives. Country's infrastructure was not prepared for such a disaster. Many buildings collapsed, leaving Haiti in ruins. Among destroyed buildings there were also hospitals and health clinics. Many injured people were left helpless, without access to medical care.
This enormous tragedy took a heavy toll on Haitian society and battered its economy. In 2013, in order to support rebuilding of the country's infrastructure, Partners in Health (known locally as Zanmi Lasante) opened a University Hospital in Mirebalais, a small city in the Central Plateau of Haiti. The new hospital had a place for 300 beds and served 1000 outpatient visits per day. Its management and workflow is supported by OpenMRS.
Rebuilding healthcare system in Haiti
OpenMRS allows to record diagnosis, plan treatment and save the data of the patients. All of this information is stored in a digital form. Not only is it convenient, but also protected from eventual disasters, like a flood or an earthquake. Physicians can capture primary care data, such as patient registration, check-in, vital signs, etc., as well as specialistic diagnosis and lab results.
Since its implementation, the system has been upgraded many times, to meet the needs of the local community. Functionalities that were at first available in UHM included:
Identifying and registering all patients at UHM and Outpatient clinic.
Point-of-care system for all users, leading to reduced data backlogs, higher quality data and improved access to data for patient care.
Integration with PACS (Picture Archive and Communication System) so that digital radiology images (especially CAT scans) can be analyzed by radiologists and results reported back to UHM clinicians.
Point-of-care post-surgery note to capture details of the surgery (team, diagnoses, procedures, medications, and recommendations).
OpenMRS became useful also in other Haitian healthcare facilities supported by Partners in Health. Depending on the capabilities of certain clinics or hospitals, different modules and functionalities are implemented.
If you are interested in more technical specifications, we encourage you to read this case study published on OpenMRS Wiki.
Our mission continues
Partners in Health, as well as OpenMRS, are constantly improving their initiatives in Haiti, collaborating with the Haiti Ministry of Health and other important partners.
University Hospital of Mirebalais is just one link in the big chain of implementations. But every link of this chain is as important as the others, because every implementation brings actual, real help to the people that are in need, making their lives easier.
OpenMRS will continue its support in the process of improving and developing this chain of life-saving solutions.
University Hospital of Mirebalais (UHM) EMR Case Study
Partners In Health Haiti EMR
Britannica | 2010 Haiti earthquake
GatesNotes | A visit to Haiti, and the biggest hellraiser I know
EMRS Cloud
Solution for your Medical Record System


power of the witch Download power of the witch or read online here in PDF or EPUB. Please click button to get power of the witch book now. All books are in clear copy here, and all files are secure so don't worry about it.
The earth, the moon, and the magical path to enlightenment. Written by a practicing witch who conducts classes and seminars on witchcraft--the oldest Western religion, a means of power and enlightenment, and a healing art.
W.I.T.C.H. is an Italian fantasy comics series written by Elisabetta Gnone, Alessandro Barbucci, and Barbara Canepa. The series was first published by Disney Italy in April 2001 before the series was released in other countries.


I sure do not know why my account was deleted i done nothing wrong and broke none the rules.
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Jeremy works as a painter for 4 years. He works with paint very delicate.
Jeremy knows about everything and even more! He successfully completed apprenticeship program and got a plumber license in 2003. Jeremy started working and got certified parallel. He has got GreenPlumbers USA certificate and National Inspection Testing Certification (NITC) certificate. Before JohnnyGo Jeremy had worked at such respected companies as Sears Home Repair and Kaufman's Experts. In 2011 Jeremy joined our team and quickly gained a reputation of responsible, careful worker and talented.


text:
"""Makes sure that the app/ code is cpplint clean."""

INCLUDE_CPP_FILES_ONLY = (
  r'.*\.cc$', r'.*\.h$'
)

EXCLUDE = (
  # Autogenerated window resources files are off limits
  r'.*resource.h$',
)

def CheckChangeOnUpload(input_api, output_api):
  results = []
  black_list = input_api.DEFAULT_BLACK_LIST + EXCLUDE
  sources = lambda x: input_api.FilterSourceFile(
    x, white_list=INCLUDE_CPP_FILES_ONLY, black_list=black_list)
  results.extend(input_api.canned_checks.CheckChangeLintsClean(
      input_api, output_api, sources))
  return results

redpajama_set_name: RedPajamaGithub


text:
\section{Introduction}

Black holes are one of the most fascinating objects in classical
general relativity. They represent the endpoint of gravitational
collapse of a large mass object, independent of initial conditions.
The prototypical black hole, the Schwarzschild solution, was first
presented barely a year after Einstein put forward his new theory
of gravity, yet it took half a century before relativists were
confident of the interpretation of this solution, and began to construct
a rigorous set of theorems describing the properties of black holes.
One of the more poetically labelled set -- the ``no hair'' theorems
\cite{nohair} -- has been perhaps the most contentious. Originally
demonstrated for static vacuum black holes, \cite{Cart,Be72}, the
no hair theorems have been refined and extended to a wide range
of interacting particle and gravitational theories, \cite{NHF,NHG,MB}.
Nonetheless, there are many known ``violations'' of the
no hair theorems, from the dressing of black holes by scalar or gauge
condensates \cite{hair}, to literal hair, in the form of topological
defects which extend out from the black hole to infinity, \cite{AGK}.

The issue of the most basic hair however, scalar hair, is thought to be
understood, yet is perhaps the most perplexing. For a wide range of
potentials, it is easy to show that a static black hole cannot have
a nontrivial scalar field on its event horizon (unless the space-time is
asymptotically anti-de Sitter, \cite{TMN}, or the scalar potential has
been specifically tailored, \cite{Z}). However, within cosmology,
scalar fields are widely used, not only for inflation, but as an
expedient model of quintessence, \cite{CDS}, or late time acceleration
(see \cite{CST} for a review of dark energy models).
Indeed, the standard exponential
scalar potential - widely used to give power law acceleration, was shown
to be in conflict with spherically symmetric asymptotically flat or de
Sitter static black hole space-times, \cite{PW}.
How then can these cosmological scalars interact with a
black hole event horizon? Generally, the scalar field is varying on a very
slow time scale relative to the light crossing time of the black hole,
thus we might expect that it has little effect on the event horizon itself,
yet, like the inexorable flow of time, the scalar must evolve
cosmologically, and it seems contradictory that it is pinned to a single
value for all time at the black hole -- an issue explored by Barrow,
\cite{Barrow}, in the context of primordial black holes.

In fact, the resolution of the conflict is quite straightforward:
The no hair theorems were explored in the context of static black
holes, and quite clearly a rolling cosmological scalar can never be
static.  Correspondingly, the presence of a black hole in a cosmology
implies that the cosmology cannot be spatially homogeneous, and
therefore does not have the canonical FRW form. While we can use
cosmological perturbation theory to describe the far field effect
of the black hole, we cannot describe the full spatial geometry
including the event horizon within the context of perturbation
theory -- and it is the effect of the event horizon which is
critical in determining the behaviour of the scalar.
We therefore need a time-dependent black hole solution.

Exact black hole solutions are surprisingly thin on the ground,
given how ubiquitous black hole are in nature, and time dependent
ones even more so. The first dynamical black hole `solution' was
postulated by McVittie, \cite{McV}, who modified the Schwarzschild
solution to include an FRW-like cosmology, with the black hole
event horizon at fixed comoving radius and a fluid energy density
dependent only on time.  However, as pointed out in \cite{KKM},
one expects the black hole to break the spatial homogeneity of
the cosmology, and thus (except in the special case of a de Sitter
universe) this unrealistic set-up leads to a singularity on the
would be event horizon. The McVittie solution has been generalised,
\cite{Sultana:2005tp,Faraoni:2007es}, to allow
for radial accretion, although the generalisations follow the
method of `metric engineering', in that a specific ansatz is
proposed, then the matter stress energy inferred (see also
\cite{Carrera:2009ve} for a discussion of some possible issues
with these approaches).

Instead of imposing a particular metric ansatz, a successful
approach has been instead to postulate a particular format
for the behaviour of the solution, notably self-similarity, first
used to estimate primordial black hole accretion in \cite{CH},
but also extended to allow more general perfect fluid
equations of state, \cite{LCF,BH,MHC}, and scalar tensor
gravity, \cite{Harada}. Although these solutions do make an
assumption about the behaviour of the metric, and are
restricted to a perfect fluid, they have the advantage that
they are exact, allow for time-dependence of the black hole,
to be explored without resorting to complex numerical methods.
(See \cite{Crev} for a brief review.)

There is also the time dependent Vaidya solution, \cite{Vaidya},
which is somewhat special, as the mass of the black
hole now becomes dependent on a null coordinate, requiring
a null matter source.
There are also exact solutions for Einstein plus scalar field
which either represent a collapsing scalar field, \cite{Husain:1994uj},
or use solution generating techniques to add scalar profiles to a
black hole, \cite{Fonarev:1994xq}. In both cases however, the
would be event horizon is singular, and indeed in \cite{Husain:1994uj},
identifying event horizons becomes an issue.
Thus a direct approach to finding an exact solution seems to have been
unsuccessful in the sense that in cosmology, we expect a solution which
will be locally interpretable as a ``black hole'' (Schwarzschild solution)
but that nonetheless will also have large scale cosmological evolution,
which on long time scales will give a natural evolution of
the black hole event horizon area due to scalar accretion.
(See \cite{Carrera:2008pi} for a review and discussion of the
interplay between cosmological expansion and local systems).

Another approach in the literature is to find a probe solution
for the scalar field, i.e.\ one in which the scalar field evolves
on a Schwarzschild background, \cite{TJ,FK}. Here, near the
event horizon, the scalar field must be
a function of the advanced null coordinate, $v \sim e^{t+r^*}$,
which parametrises the black hole future event horizon.
One can then estimate the back-reaction on the event horizon
using the energy momentum of this approximate solution.
A problem with this approach however, is that the coordinates being
used are local static Schwarzschild coordinates, which do not
correspond to the cosmological flow of time at large distances
and therefore give no guarantee that any `solution' will be well
behaved at cosmological event horizons.
One can also worry that estimates using local intuitive
notions of energy, rather than an analysis of the Einstein equations
with a scalar source, might be misleading.

In order to be confident that probe calculations give a good estimate
of scalar accretion onto black holes, we require a time-dependent
scalar field with a time dependent black hole. Here,
we present a resolution of this problem, by expanding the equations
of motion for the geometry and the scalar field order by order in
a ``slow roll'' parameter.  We present a procedure for solving
for the time dependent scalar on the black hole, finding the leading
order solution which extends from the near black hole expectation
of \cite{TJ,FK} to the cosmological solution at large distances.
Our solution is valid independent of the relative sizes of the black
hole and cosmological event horizons.
We also present the back reaction of the scalar field
on the black hole, and calculate the expansion rate of the black
hole  due to scalar accretion. An advantage of our method is that
we can identify the event horizons accurately as null surfaces,
therefore the usual ambiguity of apparent vs.\ event horizons
does not occur.

It is perhaps worth emphasising that our approach is explicitly
to construct a natural extension of the Schwarzschild `vacuum' solution,
and not some engineered exact solution of Einstein's equations, either
by making a metric ansatz, or by taking an ansatz for the behaviour of
the solution. Our only input will be the symmetries of the physical set-up,
and the output a nonsingular solution corresponding to the physical set-up
of an FRW expanding universe at large scales, and a (Schwarzschild)
black hole with some local scalar field on small scales.

\section{Scalar fields and black holes: set-up}

In this section, we set up the equations of motion for the scalar
field with the black hole. The idea is to write down the general
equations of motion compatible with the symmetries, then to
expand them order by order in the kinetic energy of the scalar
field.

To motivate our approach, consider a universe in which the
acceleration of the universe is driven by a slowly rolling scalar field,
somewhat analogous to inflation though clearly at a much lower scale.
A simple toy model consists of an FRW universe,
\begin{equation}
ds^2 = dt^2 - a^2(t) d{\bf x}^2
\end{equation}
and a scalar field with an exponential
potential $W = M^4 e^{-\beta\phi}$,
which leads to a power law acceleration
\begin{equation}
a(t) = \left ( \frac{t}{t_0} \right)^k \;\;,\;\;\;\;\;
\phi = \phi_0 + \frac{2}{\beta} \ln \frac{t}{t_0}\;\;,\;\;\;\;\;
k = \frac{2\kappa}{\beta^2} = \frac{2 W(\phi)^2}{M_p^2 W'(\phi)^2}
=\varepsilon^{-1}
\end{equation}
where $\kappa=8\pi G=M_p^{-2}$, and $\varepsilon$
is the conventional slow roll parameter introduced
here to emphasise that $k\gg1$.

Now consider the solution in conformal time $\eta
= \eta_0 (t/t_0)^{(\varepsilon-1)/\varepsilon}$:
\begin{equation}
ds^2 = \left[ \frac{\eta_0}{\eta} \right ]^{2
+\frac{2\varepsilon}{1-\varepsilon}}
\left [ (d\eta - d\rho)(d\eta+d\rho) - \rho^2 d\Omega_{{\rm II}}^2\right]
\label{sccos}
\end{equation}
where $d\Omega_{{\rm II}}^2$
is the standard line element on the unit sphere, and
\begin{equation}
\phi = \phi_0 - \frac{2\varepsilon}{\beta(1-\varepsilon)}
\ln \frac{\eta}{\eta_0} \;.
\label{phicost}
\end{equation}
Then, if we assume that $\varepsilon\ll1$, and expand
$[\eta_0/\eta]^{\frac{2\varepsilon}{1-\varepsilon}} \sim
1 - 2\varepsilon \ln |\eta/\eta_0|$,
this metric is perturbatively
close to the de Sitter (dS) metric:
\begin{equation}
g_{ab} = g^{(DS)}_{ab} \left ( 1 - 2 \varepsilon \ln
\left | \frac{\eta}{\eta_0} \right | + {\cal O} (\varepsilon^2)\right)
\end{equation}
over a Hubble time interval. The dark energy universe can
therefore be expressed as a linear perturbation of a known
exact solution to Einstein's equations -- the de Sitter universe.
Looking at \eqref{phicost}, we see that $\phi = \phi_0$, plus a
correction of order ${\cal O} \left (\varepsilon^{1/2} M_p \right )$,
and thus for small $\varepsilon$, we can express the
cosmology as a de Sitter universe with a small correction
of order ${\cal O}(\varepsilon^{1/2})$ for the scalar, and
${\cal O}(\varepsilon)$ for the geometry.

Now consider adding a black hole to this cosmological rolling
scalar solution. Given that the background solution is
a perturbation of a de Sitter universe, it is reasonable to
suppose that the black hole plus scalar might be
expressible as a perturbation of a Schwarzschild de
Sitter space-time. Note however, that this is distinct from
conventional cosmological perturbation theory, where one
perturbs a given spatial section and evolves forward in time.
Rather, here we seek to write the fully interacting
black hole-plus-scalar system as a perturbation
expansion around the static solution
in the kinetic motion of the scalar.
Just as the rolling scalar cosmology is perturbatively
close to the de Sitter manifold, we expect that the
rolling scalar plus black hole manifold should be
close to the Schwarzschild de Sitter manifold, and
just as the linear expansion above has a range
of validity, we expect that our expansion will also
be valid only over Hubble time-scales.

The geometry of the time-dependent black hole will not
now have constant curvature spatial slices,
but we do expect an SO$(3)$ symmetry, corresponding to the
spherical symmetry of the black hole. We also expect
both time and radial dependence in the metric. The general
metric may therefore be written in the form \cite{BCG,CG}
\begin{equation}
ds^2 = 4 e^{2\nu}B^{-1/2}dUdV - Bd\Omega_{{\rm II}}^2 .
\label{weylform}
\end{equation}
This form of the metric elucidates both the symmetry of the
space-time (SO(3)), as well as the remaining gauge freedom (the
conformal group in the $U,V$ directions). By rewriting
the coordinates in light-cone form, it will be clear how to deal
with the event horizons present in the anticipated
solution (the cosmological and black hole event horizons),
as well as how to change gauge to analytically extend across
these horizons. In particular, the null coordinates allow us to
identify the actual event horizons of the solution, as opposed to
apparent horizons, as an horizon is of course
always a null surface, defined by $U$ or $V=$ constant.

Using \eqref{weylform}, the coupled Einstein-scalar
equations for the variables $B, \nu, \phi$ are
\begin{eqnarray}
\phi_{,UV} &=& - W_{,\phi}(\phi)B^{-1/2}e^{2\nu}
- \frac{1}{2B}\left(B_{,U}\phi_{,V}+B_{,V}\phi_{,U}\right)
\label{phiUVeq}\\
B_{,UV} &=& 2\left(\kappa W(\phi)B^{1/2} - B^{-1/2}\right)e^{2\nu}
\label{BUVeq}\\
\nu_{,UV} &=& \frac{1}{2}\left(\kappa W(\phi)B^{-1/2}
+ B^{-3/2}\right)e^{2\nu} - \frac{\kappa}{2}\phi_{,U}\phi_{,V}
\label{nuUNeq}\\
B_{,VV} &=& 2\nu_{,V} B_{,V} - \kappa B \phi_{,V}^2
\label{Vint}\\
B_{,UU} &=& 2\nu_{,U} B_{,U} - \kappa B \phi_{,U}^2
\label{Uint}
\end{eqnarray}
where $W(\phi)$ is a general potential, the only stipulation
being that it satisfies the slow roll condition $\varepsilon\ll1$.

For a constant scalar field (i.e.\ briefly ignoring \eqref{phiUVeq})
a generalisation of the Birkhoff theorem shows that
the Einstein equations have Schwarzschild de Sitter (SdS)
as a general solution, \cite{BCG}. Given that we follow
a similar procedure in analysing the rolling scalar, it is
worth briefly reviewing the steps of this argument.

If $\phi$ is constant, \eqref{Vint} and \eqref{Uint}
can be integrated directly to give
\begin{equation}
2\nu = \ln B_{,V} + \ln G'(U) = \ln B_{,U} + \ln F'(V)
\end{equation}
where $F'$ and $G'$ represent arbitrary integration functions.
Consistency of these expressions leads us to deduce that $B$
must be a function of $\left[F(V) + G(U)\right]$, and hence
\begin{equation}
e^{2\nu} = F'(V) G'(U) B'(F+G)\,.
\end{equation}
Inserting into \eqref{BUVeq} then gives
\begin{equation}
\begin{aligned}
F'G' B'' &= 2F'G'B' \left ( \kappa W_0 B^{1/2} - B^{-1/2} \right)\\
\Rightarrow \quad
B' &= \frac43 \kappa W_0 B^{3/2}- 4 B^{1/2} + 8GM
\end{aligned}
\end{equation}
where $8GM$ is an integration constant (suggestively labeled!),
$W_0=W(\phi_0)$, and primes denote differentiation with
respect to the argument of the function.
However, writing $N(r)$ as the SdS potential
\begin{equation}
N(r) = 1 - \frac{2GM}{r} - H^2 r^2
\end{equation}
shows that in fact
\begin{equation}
B' = - 4 \sqrt{B} N(\sqrt{B})
\end{equation}
with $H^2 = \kappa W_0/3$, the vacuum density of the constant
scalar field. Changing coordinates to
$r = B^{1/2}$, $t=2(G(U)-F(V))$, then gives
\begin{equation}
ds^2 = \frac{F'G'B'}{B^{1/2}} 4 dUdV - B d\Omega_{{\rm II}}^2
\to N(r) dt^2 - \frac{dr^2}{N(r)} - r^2 d\Omega_{{\rm II}}^2
\label{UVmet}
\end{equation}
i.e.\ the Schwarzschild de Sitter metric in static coordinates.
In this form, we can see explicitly that the arbitrary integration
functions $F$ and $G$ are simply gauge degrees of freedom
of the metric \eqref{UVmet}, and in fact represent the conformal
transformations on the $(U,V)-$plane. Since $B'$ can vanish,
this metric will in general have singularities at certain values of
$B$. These are none other than the black hole and cosmological
event horizons of the static co-ordinates. However, ``cosmological''
coordinates at large `$r$' would not have an horizon, and
would asymptote a standard cosmological
de Sitter space-time; we therefore need to identify the (Kruskal)
transformations which provide extensions across each
horizon.

Writing $r^*$ as the usual tortoise co-ordinate, note that
\begin{equation}
r^* = \int \frac{dr}{N(r)} = - 2 \int \frac{dB}{B'} = -2(F+G)
\end{equation}
thus $t-r^* = 4G$, $t+r^* = -4F$. Following the usual Kruskal
method, we now choose the functions $F(V)$ and $G(U)$ to
make the metric regular at the cosmological event horizon $r_c$:
\begin{equation}
\begin{aligned}
F(V) &= -\frac{1}{2N'(r_c)} \ln \left [ N'(r_c) V \right]\;,\;\;
&{\rm or} \;\;
V &= R_c \exp \left [ \frac{(t+r^*)}{2R_c}\right] \\
G(U) &= \frac{1}{2N'(r_c)}\ln \left [N'(r_c) U\right] \;,\;\;
&{\rm or} \;\;
U &= R_c \exp \left [ \frac{(t-r^*)}{2R_c}\right]
\end{aligned}
\label{kruskcos}
\end{equation}
where we have written $R_c = 1/N'(r_c)$ as shorthand
(see appendix).

Thus, the original functions of the metric \eqref{weylform}
are
\begin{equation}
\begin{aligned}
B(U,V) &= r^2 = \left ( {r^*}^{-1} \left [R_c \ln \frac{V}{U}
\right ] \right)^2\\
e^{2\nu} &= F'G'B' = \frac{R_c^2\sqrt{B}N(\sqrt{B})}{ UV}
= \frac{R_c^2}{UV} r N(r)
\end{aligned}
\end{equation}
where ${r^*}^{-1}$ is the inverse tortoise function, which does
not in general have a closed analytic form, and $r$ is
understood to be a function of $U$ and $V$.
In these co-ordinates, as $r\to r_c$,
\begin{equation}
V = U \exp \left [ \frac{r^*}{R_c} \right] \approx U (r-r_c)
\end{equation}
thus the cosmological event horizon is at $V=0$ and is
parametrized by $U$. Moreover
\begin{equation}
e^{2\nu} = - \frac{R_c^2}{U^2} \frac{r_cN}{(r-r_c)}
\end{equation}
is explicitly regular as expected.

For future reference, the Kruskal extension at the black hole
event horizon $r_h$ would be given by the null co-ordinate choice
\begin{equation}
\begin{aligned}
F(v) &= -\frac{1}{2N'(r_h)} \ln \left [ N'(r_h) v \right]\;,\;\;
&{\rm or} \;\;
v &= R_h  \exp \left [ \frac{(t+r^*)}{2R_h}\right] \\
G(u) &= -\frac{1}{2N'(r_h)}\ln \left [-N'(r_h) u\right] \;,\;\;
&{\rm or} \;\;
u &= R_h \exp \left [ -\frac{(t-r^*)}{2R_h}\right]
\end{aligned}
\label{kruskhor}
\end{equation}
writing $R_h=1/N'(r_h)$ as before. The black hole event
horizon is at $u=0$, and parametrized by $v$.
We will mostly work with the `cosmological' co-ordinates
$U$ and $V$, however, we will refer to the black hole
Kruskals $(u,v)$ when checking regularity at the event
horizon.

Now suppose that we take into account that $\phi$ is not
constant, and write
\begin{equation}
\begin{aligned}
\phi &= \phi_0 + \sqrt{2\varepsilon} M_p \phi_1(U,V)\\
B &= r^2 \left ( 1 + \varepsilon \delta_1(U,V) \right)\\
\nu &= \nu_0 + \varepsilon \delta_2(U,V)
\end{aligned}
\end{equation}
then, recalling the expressions for $B_0=r^2$ and $\nu_0$,
and expanding the equations of motion shows that the
equation for $\phi_1$ is at order ${\cal O}(\sqrt{\varepsilon})$,
and decouples from the perturbations to the geometry, which
appear at order ${\cal O} (\varepsilon)$
\begin{eqnarray}
\sqrt{2\varepsilon}\,\phi_{1,UV} &=& \sqrt{2\varepsilon}\,
\frac{N}{UV} \left [ 3H^2 R_c^2 + \frac{R_c}{r}
\left (V\phi_{1,V} - U \phi_{1,U} \right ) \right]
\label{phiUVeqeps}\\
\varepsilon r^2 \delta_{1,UV} &=& - 2\varepsilon R_c \frac{rN}{UV}
\left ( U \delta_{1,U} - V\delta_{1,V} \right) \label{BUVeps}\\
&&+\varepsilon R_c^2 \frac{N}{UV} \left [ 4\delta_2(3H^2r^2-1)
+ 3 \delta_1 (1-H^2r^2) - 12 H^2 r^2 \phi_1 \right ]
\nonumber\\
\varepsilon r^2 \delta_{2,UV} &=& \varepsilon \frac{R_c^2N}{UV}
\left[ (1+3H^2 r^2) \delta_2 - \frac{3\delta_1}{4}(1+ H^2 r^2)
-3H^2r^2\phi_1\right] - \varepsilon r^2 \phi_{1,U} \phi_{1,V}
\quad \label{nuUNeqeps}\\
\varepsilon r^2 \delta_{1,VV} &=&
4\varepsilon R_c \frac{rN}{V} (\delta_{2,V} - \delta_{1,V})
+\varepsilon \frac{\delta_{1,V}}{V} \left ( rR_c (rN)' - r^2 \right)
- 2 \varepsilon r^2 \phi_{1,V}^2
\label{Vinteps}\\
\varepsilon r^2 \delta_{1,UU} &=&
4\varepsilon R_c \frac{rN}{U} (\delta_{1,U} - \delta_{2,U})
- \varepsilon \frac{\delta_{1,U}}{U} \left ( rR_c (rN)' + r^2 \right)
- 2 \varepsilon r^2 \phi_{1,U}^2
\label{Uinteps}
\end{eqnarray}
We therefore solve first for the scalar field rolling in the
SdS background, then compute the back-reaction on
the geometry.

\section{The scalar field}

In order to solve \eqref{phiUVeqeps}, it is most transparent
to present the equation in terms of our SdS variables:
\begin{equation}
\ddot{\phi}_1 - \frac{1}{r^2} \frac{\partial~}{\partial r^*}
\left ( r^2 \frac{\partial\phi_1}{\partial r^*}\right) = 3 H^2 N(r)
\label{phipt}
\end{equation}
Clearly, this equation will have oscillatory solutions for $\phi_1$,
corresponding to partial waves scattering off the black hole,
however, we are interested in the background, `vacuum'
solution where $\phi_1$ rolls according to the potential $W$.
Thus we set
\begin{equation}
\phi_1 = \lambda t + \varphi(r)
\label{gendphi}
\end{equation}
where \eqref{phipt} gives
\begin{equation}
\frac{d~}{dr} \left ( r^2 N \frac{d\varphi}{dr}\right) =
-3H^2 r^2
\end{equation}
which is solved by
\begin{equation}
\varphi = - \sum_i \left [ H^2 r_i
+ \frac{C}{ r^2_i} \right] R_i \ln | r - r_i|
+\frac{C}{2GM} \ln r
\end{equation}
with $C$ an integration constant. (See the appendix for
definitions of the $R_i$ etc.~together with useful identities.)

For a nonsingular solution, the $\phi$ field must be regular
in a locally regular coordinate system at both the black hole
($r_h$) and cosmological ($r_c$) future event horizons.
At the cosmological event horizon the appropriate co-ordinates
are $(U,V)$, with $V\to0$ at the cosmological event horizon, and
$t\sim R_c \ln V$, $r^* \sim R_c \ln |r-r_c| \sim R_c\ln V$.
Conversely, using \eqref{kruskhor} near the black hole event
horizon shows that $u\to0$, with $t\sim -R_h \ln(-u)$, and
$r^*\sim R_h \ln(r-r_h)\sim R_h \ln(-u)$. Therefore,
demanding regularity of $\phi_1$
gives two constraints on $\lambda$ and $C$:
\begin{equation}
\lambda - H^2 r_c - \frac{C}{r^2_c} =0
=\lambda + H^2 r_h + \frac{C}{r^2_h}
\end{equation}
solved by
\begin{equation}
C = -H^2 \frac{r_h^2 r_c^2 (r_h+r_c)}{r_h^2+r_c^2}\;\;\;,\;\;\;
\lambda = \frac{(r_c-r_h)}{r_h^2+r_c^2}\;.
\end{equation}
revisiting the expression for $\varphi$, we see
\begin{equation}
\varphi = - \lambda R_c \ln|r-r_c| + \lambda R_h \ln(r-r_h)
+ \lambda \,\frac{r_c^2R_h - r_h^2R_c}{2r_hr_c}\,\ln(r-r_N)
-\frac{r_hr_c}{r_h^2+r_c^2} \ln r
\label{varphiexpression}
\end{equation}
(using various identities from the appendix).

Pulling this together we can write the $\phi$ field in the
Kruskal coordinates (remembering that $r=r(V/U)$ or $r(uv)$)
\begin{equation}
\begin{aligned}
\phi &= \phi_0 + \sqrt{2\varepsilon} M_p\, \lambda
\Bigl [ 2 R_c \ln \frac{U}{R_c} + 2 R_h \ln(r-r_h)
+ \frac{r_c R_h}{r_h} \ln(r-r_N)- \frac{r_h r_c \ln r}{(r_c-r_h)}
\Bigr] \qquad \\
&= \phi_0 + \sqrt{2\varepsilon} M_p\, \lambda
\Bigl [ 2 R_h \ln \frac{v}{R_h} - 2 R_c \ln|r-r_c|
- \frac{r_h R_c}{r_c} \ln(r-r_N)- \frac{r_h r_c \ln r}{(r_c-r_h)}
\Bigr]
\end{aligned}
\end{equation}
which is manifestly nonsingular at the horizons, and illustrated
in figure \ref{fig:phicontours}.
\FIGURE{
\includegraphics[scale=1]{phicontours.pdf}
\caption{Contours of constant $\phi$ (thick blue) within our
Hubble volume. The Penrose diagram is obtained by
compactifying along the diagonal directions $U$ and
$V$ using the map $x \to (1+x)/(1-x)$.
For comparison, contours of constant $t$ and $r$ are shown in grey,
and a constant {\it cosmological} time contour ($U+V$) shown in red.
The horizons are labelled, as are the singularity and future infinity.}
\label{fig:phicontours}
}

Figure \ref{fig:phicontours} shows that the rolling of the scalar lags
behind on the black hole event horizon, what is less clear is a slight lagging
on the cosmological event horizon. This is more clearly seen if we plot
$\phi$ as a function of $r^*$,
as this makes the effect of the event horizons on the rolling of the
scalar clearer. Figure \ref{fig:phiofrstar} shows the profile
of the scalar field as a function of $r^*$ at differing values of
the `cosmological' time parameter $\eta=(U+V)/2$. The
lag due to the event horizon ($r^*\to-\infty$) is clearly shown
here, together with a slight lag (relative to $r^*\approx0$)
towards the cosmological event horizon, although the $\phi$
profile becomes flat at larger $r^*$, as indeed it should as
we expect to be close to the cosmological solution which
depends only on $U+V$. (For both figure \ref{fig:phicontours}
and \ref{fig:phiofrstar}, the parameter values $r_h=1$, $r_c=15$
were used.)
\FIGURE{
\includegraphics[scale=0.75]{phiofrstar.pdf}
\caption{The profile of the perturbation of the scalar field
shown as a function of $r^*$. The field is illustrated at three
different time steps, showing the field rolling to larger $\phi$
values. This figure was produced using the values $r_c=15$,
$r_h=1$, $\eta_0=R_c\sim-8.3$, and for clarity the scalar
field is normalised to its value at $\eta_0$ and
$r^*=0$, or alternately $t=-2R_c$, $r=2$: ${\hat \phi}_1
= \phi_1/\phi_1(-2R_c,2)$ where, recall, $\phi_1=
\lambda t + \varphi$, given in \eqref{varphiexpression}.
(For reference, $\phi_1(-2R_c,2)\simeq-2.7$).
}
\label{fig:phiofrstar}
}

Finally, note that as $r_h\to0$,
\begin{equation}
\phi = \phi_0 + \sqrt{2\varepsilon} M_p\, \Bigl [
\frac{2R_c}{r_c} \ln \frac{U}{R_c} + \ln(r+r_c) \Bigr]
\sim \phi_0 - \sqrt{2\varepsilon} M_p\, \ln |U+V|
\end{equation}
i.e., the cosmological rolling scalar solution
to order ${\cal O}(\varepsilon^{1/2})$, (cf \eqref{phicost}).
On the other hand, near the black hole event horizon,
\begin{equation}
\phi \sim \phi_0 + \sqrt{2\varepsilon} M_p 2 \lambda R_h \ln v
\end{equation}
in agreement with the linearized solutions of \cite{TJ,FK}.

\section{Back-reaction on the black hole geometry}

Clearly, since $\phi$ is regular from the black hole event horizon
out to the cosmological event horizon with regular derivatives,
its energy momentum is finite in this region. We can therefore
compute the back-reaction on the geometry to
get a consistent solution to order ${\cal O}(\varepsilon)$.

We start by comparing the first integrals of \eqref{Vinteps}
\begin{equation}
\begin{aligned}
2\delta_2 &= 2\delta_1 + \int \frac{rV \phi_{1,V}^2}{R_cN} dV
+ \int \left [ \frac{rV\delta_{1,VV}}{2R_cN}
+ \frac{r\delta_{1,V} }{2R_cN}
- \frac{(rN)'}{2N} \delta_{1,V} \right] dV + g(U)\\
&= \delta_1 + \int \frac{rV \phi_{1,V}^2}{R_cN} dV
+ \frac{rV}{2R_cN} \delta_{1,V} + g(U)
= \delta_1 + I_V
+ \frac{rV\delta_{1,V} }{2R_cN} + g
\end{aligned}
\label{VVint}
\end{equation}
and \eqref{Uinteps}
\begin{equation}
\begin{aligned}
2\delta_2 &= 2\delta_1 - \int \frac{rU \phi_{1,U}^2}{R_cN} dU
- \int \left [ \frac{rU\delta_{1,UU} }{2R_cN}
+ \frac{r\delta_{1,U} }{2R_cN}
+ \frac{(rN)'}{2N} \delta_{1,U} \right] dU + f(V)\\
&= \delta_1 - \int \frac{rU \phi_{1,U}^2}{R_cN} dU
- \frac{rU}{2R_cN} \delta_{1,U} +f(V)
= \delta_1 +I_U
- \frac{rU\delta_{1,U} }{2R_cN} +f
\end{aligned}
\label{UUint}
\end{equation}
Where $f$ and $g$ are (for now) arbitrary integration functions,
and can be thought of as the perturbation of $F'$ and $G'$.

Substituting for $\phi_1$ from \eqref{gendphi} shows that the
$\phi$-integrals in (\ref{VVint},\ref{UUint}) can be written as
functions of $r$. For example
\begin{equation}
\begin{aligned}
\phi_{1,V} &= \frac{R_c}{V} \left ( \lambda + N\varphi'\right)
= \frac{R_c}{V} \left ( \lambda - H^2 r - \frac{C}{r^2} \right )\\
\Rightarrow \quad I_V&= \int \frac{rV \phi_{1,V}^2}{R_cN} dV
= \int r \frac{dr}{dV} \left ( \lambda - H^2 r - \frac{C}{r^2} \right )^2
dV + \delta g(U)
\end{aligned}
\end{equation}
where the $\delta g(U)$ is added to acknowledge the fact that
an integral over $V$ can have an arbitrary integration factor
that is $U-$dependent, which may not be the same factor
as the $r$ integral. However, since our expressions in \eqref{VVint}
and\eqref{UUint} already contain integration functions, we
will now without loss of generality define
\begin{equation}
\begin{aligned}
I_V &= \int \frac{rdr}{N^2} (H^2 r + \frac{C}{r^2}-\lambda)^2\\\
I_U &= \int \frac{rdr}{N^2} (H^2 r + \frac{C}{r^2}+\lambda)^2
\end{aligned}
\end{equation}
and take it that the functions $f$ and $g$ are appropriately adjusted.

Next, consistency of (\ref{VVint},\ref{UUint}) requires
\begin{equation}
U\delta_{1,U} +V\delta_{1,V} = 2R_c\frac{\partial~}{\partial t}
\delta_1 = \frac{2R_cN}{r} \left ( I_U-I_V+f-g\right)
\end{equation}
which determines the general form of $\delta_1$ as
\begin{equation}
\delta_1 = \frac{R_cN}{r} \left [ \ln(\frac{UV}{R_c^2}) (I_U-I_V)
+ \int \frac{2f}{V} dV - \int \frac{2g}{U} dU
+ h(r) \right]
\label{delta1}
\end{equation}
where $h(r)$ is an arbitrary integration function. Combining
\eqref{VVint} and \eqref{UUint} then implicitly gives $\delta_2$:
\begin{equation}
\delta_2 =  \frac{\delta_1}{2} + \frac{r}{4} \frac{\partial~}
{\partial r} \delta_1 + \frac{I_U+I_V}{4} + \frac{f+g}{4} \;.
\label{delta2form}
\end{equation}
We now substitute these expressions into \eqref{BUVeps}, and
after some algebra, the only nonzero terms give
a second order ODE for $h(r)$:
\begin{equation}
R_c \left [ rN^2 h' \right ] '= 12 H^2 r^2 \varphi
+ (rN)' \left( I_U+I_V \right) \;.
\end{equation}
It proves helpful to manipulate this equation using integration
by parts, and the fact that $12H^2r^2 = [rN^2(I_U'-I_V')]'/\lambda$,
to find an expression for h:
\begin{equation}
h(r) = (I_U-I_V) \frac{\varphi}{\lambda R_c} + h_2(r) + h_3(r)
\end{equation}
where
\begin{equation}
\begin{aligned}
h_2(r) &= \int \frac{I_U}{\lambda R_cN} \left ( \lambda + H^2 r + \frac{C}{r^2}\right)
+ \int \frac{I_V}{\lambda R_cN} \left ( \lambda - H^2 r - \frac{C}{r^2}\right)\\
h_3(r) &= \int \frac{1}{R_c rN^2} \int \frac{2r^2}{N}
\left ( \lambda + H^2 r + \frac{C}{r^2}\right)\left ( \lambda - H^2 r - \frac{C}{r^2}\right)
\end{aligned}
\end{equation}
Thus
\begin{equation}
\delta_1 = \frac{R_cN}{r} \left [ \frac{\phi_1}{\lambda R_c} (I_U-I_V)
+ \int \frac{2f}{V} dV - \int \frac{2g}{U} dU
+ h_2(r) + h_3(r) \right]
\label{delta1}
\end{equation}

It is reasonably clear that $\delta_1$ is regular at both event
horizons, provided $f$ and $g$ are no more divergent than
$V^{-1}$ or $U^{-1}$, however, we must examine regularity of
$\delta_2$, as we still need to determine the integration functions.
Inputting $\delta_1$ into \eqref{delta2form} gives
\begin{equation}
\begin{aligned}
\delta_2 = &\frac{\delta_1}{4} + \frac{f+g}{2}
+ \frac{R_cN'}{4} \left ( \int \frac{2f}{V} dV - \int \frac{2g}{U} dU
\right)+ \frac{R_c}{4} \left[N(h_2+h_3)\right]' \\
&+ \frac{\phi_1}{4\lambda} \left [N(I_U-I_V)\right]'
+ \frac{I_U}{4\lambda}\left ( \lambda - H^2 r-\frac{C}{r^2}\right)
+ \frac{I_V}{4\lambda}\left ( \lambda + H^2 r+\frac{C}{r^2}\right)
\end{aligned}
\label{deltanu}
\end{equation}
Clearly, the terms involving $I_U$, $I_V$ and $\delta_1$ are regular
from the definitions of $C$ and $\lambda$,
however, the residual pieces contain divergences, and we
must choose $f$ and $g$ to regularise these. We will show this
process in detail for the cosmological event horizon, the black
hole event horizon follows the same steps.

First we identify the potentially singular behaviour of the relevant
functions
\begin{equation}
\begin{aligned}
I_U &= \frac{a_U}{r-r_c} + b_U \ln |r-r_c| + c_U + J_U(r)\\
I_V &= \frac{a_V}{r-r_h} + b_V \ln (r-r_h) + c_V + J_V(r)\\
N h_3 &= \frac{\alpha_c}{R_c} (r-r_c)\ln|r-r_c|
+ \frac{\alpha_h}{R_h} (r-r_h) \ln(r-r_h) + N{\tilde h}_3
\end{aligned}
\end{equation}
where the constants can be inferred from the appendix,
$J_U={\cal O}(r-r_c)$, $J_V={\cal O}(r-r_h)$, and
$(N{\tilde h}_3)'$ is regular. Then the singular parts appearing in
\eqref{deltanu} are:
\begin{equation}
\begin{aligned}
&\frac{\phi_1}{\lambda} \left [N(I_U-I_V)\right]'\Big |_{\rm{sing}}
+ R_c\left [N(h_2+h_3)\right] ' \Big |_{\rm{sing}}
=\frac{R_h}{R_c} b_V \left [ \ln(r-r_h)\right]^2 &\\
&
+\left [ \alpha_c + 2b_U+ 2 c_U + \frac{b_U\phi_1}{\lambda R_c}
+ 3 a_U H^2 \frac{r_h(r_h+r_c)}{(2r_c+r_h)}
\right]\ln |r-r_c|+b_U \left [ \ln|r-r_c|\right]^2
\qquad\\
&+ \frac{R_h}{R_c}
\left [ \alpha_h+2b_V+ 2 c_V + \frac{b_V\phi_1}{\lambda R_h}
+ 3a_V H^2 \frac{r_c(r_h+r_c)}{(2r_h+r_c)}\right]\ln (r-r_h)
&\end{aligned}
\label{singh}
\end{equation}
These can be cancelled by choosing $f=f_0 + f_1 \ln V$
and $g=g_0 + g_1 \ln U$, where the constants $f_i$ are chosen
to make $\delta_2$ regular at $r_c$, and the $g_i$ from
regularity at $r_h$. For example, as $r\to r_c$,
\begin{equation}
V \sim (2r_c+r_h)U \left ( \frac{r_h-r_c}{2r_c+r_h}
\right)^{\frac{R_h}{R_c}}(r-r_c)
\end{equation}
hence
\begin{equation}
\begin{aligned}
2f + \int\frac{2f}{V} dV \Bigg |_{\rm{sing}} &\sim
f_1 \left ( \ln V\right)^2 + (f_0+f_1) \ln V\\
& \sim f_1 \left [ \ln|r-r_c|\right]^2 + 2 f_1 \ln U \ln |r-r_c|\\
+ \Bigl [f_0+2f_1&+\frac{2f_1R_h}{R_c} \ln(r_c-r_h)
+ \frac{2f_1R_N}{R_c} \ln(r_c-r_N) \Bigr] \ln|r-r_c|
\end{aligned}
\end{equation}
Comparing this with \eqref{singh}, and recalling that $\phi_1
\sim 2 R_C\lambda \ln(U/R_c)$, we see that
\begin{eqnarray}
f_1 &=& -b_U\\
f_0&=& \alpha_c + 4b_U+ 2 c_U
+\frac{2b_U}{R_c} \left [ R_h\ln(r_c-r_h)
+ R_N\ln(r_c-r_N)\right]
+ 3 a_U H^2 \frac{r_h(r_h+r_c)}{(2r_c+r_h)}
\nonumber
\end{eqnarray}
with similar expressions for the $g_i$.
The remaining, regular, parts of $\delta_1$ and $\delta_2$ are then
expressible in terms of regular dilogarithms and logarithms, but the full
expressions are rather lengthy and cumbersome.

Instead, by focussing on the event horizons, it is
easiest to obtain results of most physical interest. For the
cosmological event horizon, the $\{U,V\}$ coordinate system is
appropriate, with the CEH being at $V=0$, and parametrized by $U$.
Since $r=$ const.\ along the horizons, \eqref{Uint} gives
\begin{equation}
B = r_c^2 \left ( 1-8\varepsilon \lambda^2 R_c^2\ln |U| \right)
\simeq r_c^2 |U|^{-8\varepsilon \lambda^2 R_c^2}
\end{equation}
Setting $r_h \to 0$ gives $4 \lambda^2 R_c^2 =1$, and hence $B
\propto |U|^{-2\varepsilon}$, in complete agreement with the cosmological
event horizon area of the pure rolling scalar solution, \eqref{sccos}.

Of more interest however is the accretion of scalar field onto
the black hole. Here, using the Kruskal $\{u,v\}$ system and
\eqref{Vint}, we get
\begin{equation}
B = r_h^2 \left ( 1+8\varepsilon \lambda^2 R_h^2\ln v \right)
\simeq r_h^2 v^{8\varepsilon \lambda^2 R_h^2}
\label{hplusgrow}
\end{equation}
In other words, the event horizon creeps out very slowly.
We can compare this with an order of magnitude estimate based
on  naive physical notions of mass and energy flow, \cite{TJ,FK}.
The flow of energy into the black hole should be governed by
the difference of the energy momentum tensor from being null,
$T^0_0-T^r_r$, which is of order
${\dot\phi}^2 \sim W'^2/ H^2 \sim \varepsilon H^2/\kappa$.
Integrating this over the black hole event horizon gives
$\kappa\delta {\dot M} \sim r_h^2 \varepsilon H^2$, or
using the relation between horizon radius and mass:
$\delta A \sim r_h^3 \varepsilon H^2 \delta t $.
Of course, we should be careful of using a time coordinate
near the black hole event horizon, as
$t \sim 2 r_h \ln v + \ln(r-r_h)$ is singular,
however, in the spirit of this heuristic argument, we can identify
$\delta t \sim 2r_h \delta (\ln v)$, which gives
$\delta A \sim A \varepsilon(\delta \ln v) r_h^2/r_c^2 $,
in qualitative agreement with \eqref{hplusgrow}.

For an astrophysical black hole, this accretion rate is glacially
slow, and far outweighed by the local environment, in which
the accretion disc far outweighs local interstellar matter, let alone
this cosmologically coasting scalar. However, the fact that naive
local estimates of the back-reaction of accretion of scalar matter
in this set-up are fully backed up by this analytic calculation, valid
in the full region between the black hole and cosmological event
horizons, means we should have confidence in these physically
motivated techniques.

To illustrate the effect of the rolling of the scalar, in figure
\ref{fig:horizons} we show the effect on the event horizon
areas; for the purpose of illustration choosing $\varepsilon=0.1$,
and the rather artificial initial values of $r_c=2$, $r_h=1$.
Both horizons grow during the Hubble time, although the
cosmological event horizon has a larger relative growth of c.\ 22\%,
as opposed to approximately 13\% for the black hole event horizon.
\FIGURE{
\includegraphics[scale=0.8]{rcrh.pdf}
\caption{A plot of the variation of the event horizon areas for the
initial choice of $r_c=2, r_h=1, \varepsilon=0.1$.}
\label{fig:horizons}
}

\section{Discussion}

In this paper, we have shown how to couple a slowly rolling scalar field
to a black hole. We first set up the most general metric describing
the physical set-up -- an SO(3) symmetric geometry with dependence
on both ``time'' and ``radial distance''. This geometry is most
naturally described in light-cone coordinates, which elucidate the
integrable nature of the vacuum equations, and also lend themselves
to an accurate determination of the black hole event horizon.
Writing down the equations of motion reveals that if the potential is
not too steep, the scalar field evolution will be slow, and the equations
of motion can be solved perturbatively in the dynamics of the scalar field.

It is worth emphasising that although we perform an expansion
in the dynamics of the scalar field, the solutions we find are
exact across the the full radial range from the black hole to
cosmological event horizons, and are not in any sense perturbative
in the spatial (radial) coordinate. Not only do we correctly identify
what the dynamical dependence is, we
are able to correctly identify the cosmological evolution (and hence
cosmological time) far from the black hole, as well as how the scalar
field drives this expansion, and how it is dragged by the black hole.
For example, we can apply these results to
black holes whose event horizon constitutes a significant fraction
of the Hubble volume. These black holes accrete at a similar rate
to the increase in area of the cosmological event horizon.

It is interesting to compare the accretion rate of the black hole
to the evaporation rate, to see whether black holes, or radiation,
will dominate the final state of the universe. The black hole
evaporation rate is inversely proportional to the area of its
event horizon: ${\dot M}_H \sim 10^{-4} \hbar/r_h^2$,
whereas the accretion rate is proportional to horizon area:
$G \delta M \sim  \varepsilon c H^2 r_h^2 \delta t$.
Thus in order for evaporation to dominate, the horizon
radius of the black hole would have to satisfy
\begin{equation}
r_h \lesssim 0.1 \varepsilon^{-1/4} \left [
\frac{\hbar G}{ c H^2} \right] ^{1/4}
\sim 5 \times 10^{-6} \varepsilon^{-1/4} {\rm m}
\end{equation}
Since $\varepsilon \sim 1+w$, where $w$ is the equation of state
for the dark energy, in order for astrophysical black holes to
preferentially evaporate, we would require an equation of state fine tuned
to approximately $|1+w| \leq {\cal O} (10^{-36})$!

We should point out that while we have a time dependent
scalar field in a time dependent cosmological black hole background,
this should not be viewed as a violation of the no hair theorems.
The solution corresponds to a rolling cosmological scalar field in
which there is a black hole, and the rolling of the scalar adjusts to
its presence. The scalar does roll in the vicinity
of the black hole, although it lags behind the cosmological
evolution, in the sense that the constant $\phi$
contours lie in front of the constant $\eta$ contours in figure
\ref{fig:phicontours}. However, the black hole does not have any
scalar charge -- there is no 1-parameter solution for $\phi$ in
the black hole background. The solution \eqref{gendphi} is
not the most general solution, there will be wave like fluctuations
around this background, but we have not been able to find a
family of solutions with space-like dependence, which would
be a signature of a scalar charge on the black hole. Thus,
our results should be viewed as a way of reconciling the ``no hair''
intuition with more general time dependent situations.

Finally, to our knowledge, this is the first analytic procedure for
finding a non-singular accreting black hole space-time from first
principles (i.e.\ without making assumptions as to the form
of the metric or solution) that results from consideration of a physically
realistic matter system with physically motivated symmetries and
boundary conditions. The results apply to a general potential,
and only require that the scalar field is slowly rolling.
As such, they represent a testing ground for investigation
of black hole phenomena in the time dependent regime.

\acknowledgments
We would like to thank Anne Davis for helpful discussions.
RG is supported in part by STFC (Consolidated Grant ST/J000426/1),
in part by the Wolfson Foundation and Royal Society, and in part
by Perimeter Institute for Theoretical Physics. SC is supported by an
EPSRC studentship.
Research at Perimeter Institute is supported by the Government of
Canada through Industry Canada and by the Province of Ontario through the
Ministry of Economic Development and Innovation.

redpajama_set_name: RedPajamaArXiv


text:
HomeConservation MattersDemolish illegal structures in NNNP
Demolish illegal structures in NNNP
Tito Marv Monday, May 12, 2014
The Protected Area Management Board, the site-based policy and administrative body of the Northern Negros Natural Park, should heed the recommendation of its Technical Working Group to order the demolition of illegal structures in the protected area, especially those that were constructed by private individuals, who have no right to stay in this biodiversity-important site.
The recommendation of the TWG came after it was tasked by the PAMB to assess and evaluate the different structures in the NNNP and to come out with possible courses of action.
It can be recalled that the Provincial Environment and Natural Resources Office has issued at least 89 cease-and-desist orders to private individuals, who have been found to have constructed vacation houses in the NNNP without prior permit from the PAMB. Since NNNP is a component of the National Integrated Protected Areas System of the Philippines, as provided for in Republic Act 7586, it is a requirement that the construction or maintenance of any kind of structure, fence or enclosures, and conducting business enterprise, require the issuance of appropriate permit from the PAMB.
The PAMB is not in the position to make any position and decision that are contrary to the NIPAS. The executive director of the Department of Environment and Natural Resources in Region VI, who acts as the chair of the management board, should make sure that the PAMB acts within its power and authority, and in conformity with appropriate laws, rules and regulations. The DENR Secretary has the power to overturn decisions rendered by the PAMB that are not appropriate in the management of protected areas, like the NNNP.
While it is true that NNNP is a protected area, it is not absolute that occupancy is not allowed. However, it is only allowed in the designated multiple use zone and restricted only to the so-called tenured migrants. Based on the revised implementing rules and regulations of the NIPAS Act, the household head shall be considered a tenured migrant if proven to have actually and continuously occupied a portion of the protected area five years before its designation under the NIPAS, and solely dependent therein for subsistence.
Tenured migrants should be organized to avail a land tenure privilege, known as the Protected Area Community Based Resource Agreement, which shall be awarded by the DENR upon the endorsement of the PAMB. The purpose of this arrangement is to control occupancy and create strong social fence. It is the responsibility of the beneficiaries of land tenure to ensure that no additional migrants will stay in the awarded sites.
Based on the initial evaluation by the DENR, the recipients of the CDOs are not actually tenured migrants, since all of them are residents of areas outside the NNNP and they are not subsistence persons.
Aside from violating the NIPAS once the PAMB allows the owners of these vacation houses to occupy portions of the NNNP, it shall become a precedent and others may also follow. If that is the scenario, the PAMB will be out of control and becomes an ineffective management body of the NNNP.*


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text:
Pennsylvania je američka savezna država smještena na Istočnoj obali SAD-a, omeđena saveznim državama New York, New Jersey, Delaware, Maryland, West Virginia i Ohio. Glavni grad je Harrisburg.

Razvijena je poljoprivreda, šumarstvo te metalurška, kemijska i prehrambena industrija.

Ime

Svoje ime Pennsylvania je dobila po britanskom admiralu Williamu Pennu i svojoj prirodnoj specifičnosti (sylvania - šumska zemlja).

Okruzi (Counties)

Pennsylvania se sastoji od 67 okruga (counties)

Stanovništvo

Popisom iz 2002. Pennsylvania ima 12,335,091 stanovnika
Etnička struktura 2000. je izgledala ovako:
Angloamerikanci
Afroamerikanci 1,224,612
Portorikanci i manji dio Kubanaca 394,088
Kinezi 50,650
Korejci 31,612
Vijetnamci 30,037
Američki Indijanci: 18,348
Filipinci 14,506
Polinezijci 14,126

Indijanci

Domorodačko indijansko stanovništvo Pennsylvanije je nestalo. Prastanovnici su bili plemena Susquehanna ili White Minqua s rijeke Susquehanna River, a prostirali su se i po državama New York i Maryland. Drugo pleme bili su Honniasont ili Black Minqua s gornjeg Ohia, a prostirali su se i u Zapadnu Virginiju.

Najveći gradovi

Bilješke

Literatura

 Opća i nacionalna enciklopedija u 20 svezaka, sv. XVI, Zagreb, 2007.


text:
Midway USA's Gun Stories
Action | Adventure | Nature
Outdoor Channel (US)
Hosted by actor and gun enthusiast Joe Mantegna, Midway USA's Gun Stories takes viewers through a firearm's history, from the heart of the design through its use on the range. Using state-of-the-art, high-speed photography, Gun Stories looks at the operation and performance of each weapon, from classics like the Mauser bolt-action, to cutting-edge firearms like the Adaptive Combat Rifle. Throughout the series, historians, shooters, trainers and industry experts place these weapons in their historical and social context, making Gun Stories a unique and definitive collection on the history of firearms.
Midway USA's Gun Stories Next Episode Air Date
S7E8 - The Guns of Teddy Roosevelt
Joe Mantegna takes an in-depth look at the President's famed trip to Africa.
Air Date: 02 Aug 2017 18:30 (CDT)
S7E9 - The MP38, MP40
The MP 38 and MP 40 submachine guns.
S7E10 - The History of Ignition Systems
Joe Mantegna discusses various ignition systems dating back to the 17th century.


text:
Home > True Crime > Ana Walshe
'Physically Violent' Sociopath: Longtime Friends Of Missing Mother Ana Walshe Slam Husband Brian
Source: @analjubicic/facebook
By:Alexandra Stone
Days after Massachusetts mother Ana Walshe mysteriously went missing, her husband, Brian, was arrested for misleading investigators on his whereabouts.
Now, friends and family members are slamming the 47-year-old as "violent," untrustworthy and a "diagnosed sociopath."
Jeffrey Ornstein, who was once a close friend of Brian's late father, Dr. Thomas Walshe, claimed Brian was disinherited after conning his father out of money, according to a legal filing from his 2019 dispute over the elder Walshe's estate.
CASEY ANTHONY 'DOESN'T GIVE A S**T IF PEOPLE BELIEVE HER' OR BLAME HER FOR DEATH OF TODDLER: SOURCE
"Brian is not a trustworthy person and his Affidavit is based on lies and misrepresentations," Jeffrey stated at the time, noting that Brian was a "diagnosed" sociopath who had done a long-term stint at a psychiatric hospital.
Another one of Thomas' former friends, Dr. Fred Pescatore, described Brian as a "very angry and physically violent person" and also referred to him as a "sociopath."
The father-of-three was arrested on Sunday, January 8, one week after Ana allegedly left home to go on an emergency work trip to Washington, D.C. Brian stated she went to Logan International Airport via rideshare, but police later found there were no records of the 39-year-old paying for a car service or taking a flight.
Ana Walshe
Search Warrants Executed In Missing Mom Ana Walshe Case As Husband Brian Remains In Police Custody
Brian Walshe Charged With Murder After Wife Ana Mysteriously Vanished On New Year's Day
Ana Walshe's Friend Believes Massachusetts Mom's 'Kindness' Towards Husband Brian Got Her Killed
Source: cohasset police department
They also discovered remnants of blood in the basement and a broken knife. On top of that, Brian allegedly searched "how to dispose of a 115-pound woman's body" on the Internet and bought hundreds of dollars of cleaning supplies from Home Depot prior to his wife's disappearance.
JONBENÉT RAMSEY PETITION NEARS RECORD NUMBERS AS DNA FROM 52 YEARS AGO USED TO SOLVE ANOTHER COLD CASE
He is currently being held in police custody on charges of "misleading investigators" after telling cops that once Ana left their home around 6 a.m., he spent Sunday, January 1, with their three children and ran assorted errands. Authorities believe he gave them a false timeline of the events of the day.
As OK! previously reported, the couple's mutual friend, who attended their New Year's Eve festivities, claimed that everything felt completely normal only hours before Ana's shocking disappearance.
"We hugged and celebrated and we toasted, just what you do over New Year's," Gem Mutlu told WBZ-TV news. "There was a lot of looking forward to the New Year. There was no indication of anything other than celebrating the New Year, problems on hold."
Brian is currently being held on $500,000 bail.
CNN reported the character witness statements on Brian found in the 2019 filing.


The men of Israel retreated in the place they had gathered for battle, but Eleazar stood his ground and attacked the Philistines until his hand was tired and stuck to his sword. The Lord brought about a great victory that day. Then the troops came back to him, but only to plunder the dead. After him was Shammah son of Agee the Hararite. The Philistines had assembled in formation where there was a field full of lentils. The troops fled from the Philistines, but Shammah took his stand in the middle of the field, defended it, and struck down the Philistines. So the Lord brought about a great victory.
These are the names of David's warriors: Josheb-basshebeth the Tahchemonite was chief of the officers. He wielded his spear against eight hundred men that he killed at one time.
At that time David was in the stronghold, and a Philistine garrison was at Bethlehem. David was extremely thirsty and said, "If only someone would bring me water to drink from the well at the city gate of Bethlehem!" So three of the warriors broke through the Philistine camp and drew water from the well at the gate of Bethlehem. They brought it back to David, but he refused to drink it. Instead, he poured it out to the Lord. David said, "Lord, I would never do such a thing! Is this not the blood of men who risked their lives?" So he refused to drink it. Such were the exploits of the three warriors.
They brought it back to David, but he refused to drink it. Instead, he poured it out to the Lord. David said, "Lord, I would never do such a thing! Is this not the blood of men who risked their lives?" So he refused to drink it. Such were the exploits of the three warriors.
Benaiah son of Jehoiada…went down into a pit on a snowy day and killed a lion. He also killed an Egyptian, an impressive man. Even though the Egyptian had a spear in his hand, Benaiah went down to him with a club, snatched the spear out of the Egyptian's hand, and then killed him with his own spear.


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text:
Don't Be Afraid to Organize
By: Office of Public Affairs • October 27, 2021
Ahead of Labor Day, Secretary Marty Walsh and AFL-CIO President Liz Shuler hosted a virtual roundtable on collective bargaining and organizing in America. We asked AFL-CIO member Anders Bloomquist to share his experience with organizing and how his union has supported him.
What made you and your coworkers want to organize?
Several of us had been talking about it for a number of months, but ultimately it was a combination of the pandemic, the George Floyd protests, and recognizing the lack of internal structures around things like discipline. Initially, no one was opposed, but some people were uncertain. By the time we announced to management, over 80% of the workers were on board.
What has your experience with organizing and collective bargaining been like?
It has been respectful. There have certainly been points of contention, but we've found that we were able to establish a level of mutual respect with management that both sides have worked to maintain. We just finished our collective bargaining agreement and are extremely proud of what we've accomplished.
How has your union supported you?
UNITE HERE! Local 17 has been wonderful. First, the organizing committee received lots of effective guidance and support. Then, despite an overwhelming majority of the Local's members being out of work, the leadership team was willing to take a chance on a handful of smaller units at our workplace and the others organizing in the area.
Over 60 million Americans say they would join a union if they could. What would you say to someone who asked you whether they should organize a union at their workplace?
I won't say it's quick or effortless, but it's less intimidating than you may think. The ability to get to know people, cultivate relationships of trust and mutual respect, then ask them to take a step with you are all basic steps in the process. If you do these things already then you are ready to begin building. There are of course many more specifics, but those are some of the core fundamentals.
Power in Solidarity
Strength in Numbers: Organizing in the South
Remembering America's Nuclear Weapons Program Workers


The Global All Terrain Vehicle (ATV) Market 2017 research report provides several essential elements such as the market size & share, forecast trends, applications, and specifications. The report also delivers a full abstract of the economic ups and downs in terms of demand rate and fulfillment ratios. The All Terrain Vehicle (ATV) report explains the in-depth summary of current innovations, parameter, specifications, and creation.
The MRS Research Group report provides a detailed study of the All Terrain Vehicle (ATV) market, enlightening the major areas such as future market scenario, market growth factors, market growth restraints, and others. Segments are broadly segmented based on the constant updates in the development parameters, quality parameters, reliability parameters and end user demands. The advanced technological trends and various new opportunities are also provided in All Terrain Vehicle (ATV) research report.
The report has information of global All Terrain Vehicle (ATV) market that comprises of a large number of reputed organizations, firms, vendors, manufacturer and can deliver in-detail summary of the overall key players who hold major count in terms of revenue, sales, demand, through their reliable services, products, and post-sale processes. The All Terrain Vehicle (ATV) report provides a thorough analysis of the prominent driving factors that are identified based on the end-user demands, variable market changes, restraining elements and regulatory compliance. Many trends such as globalization, technology advancement, over-capacity in developed markets, market fragmentation regulation & environmental concerns, and product proliferation are covered in All Terrain Vehicle (ATV) report.
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The All Terrain Vehicle (ATV) report covers the precisely studied and evaluated data of the global market players and their scope in the market using a number of analytical tools. The analytical tools such as investment return analysis, SWOT analysis and feasibility study are used to analyze the key global market player's growth in the Teeth Whitening Kits industry. Apart from that, the statistical data are represented in the form of graphs, diagrams, pie charts, etc. so that the users are able to understand the market figures easily.


Both Daniel Murphy (Luray 2004-05) and Cory Spangenberg (Winchester 2010) signed free agent contracts with new teams yesterday.
Murphy signed a two-year, $24 million deal with the Colorado Rockies, possibly to play first base instead of his usual second. In 91 games and 328 at-bats split between Washington and Chicago in 2018, Daniel hit 299/336/454, with 15 doubles and 12 home runs.
Spangenberg, released by the San Diego Padres a couple weeks ago (my hunch is because of a 40-man roster crunch), has signed a one-year, $1.2 million contract with the Milwaukee Brewers, where, if he makes the team, he will play with Erik Kratz, another former Valley Leaguer. Cory hit 235/298/362 in 298 at-bats for the Padres in 2018, while playing four different positions (not including pitcher or designated hitter). He has a shot to win the starting second base job.


This is a free and comprehensive report about noguchi-trans.co.jp is hosted in on a server with an IP address of 120.136.14.43. This website hosted on Japan to the world. The website has registered on 2000-07-31 and has updated on 2016-08-01 and will expire on Connected . The website noguchi-trans.co.jp is expected to be earning an estimated $ 480.00 USD on a daily basis. noguchi-trans.co.jp report : html tags, whois, traffic report, safety information, social engagement, search preview and EZ SEO analysis. We have listed the list of different most common domain typos for your noguchi-trans.co.jp domain based on below. You can review more detailed statistical information of this domain name below and express your thoughts.


text:
Holographic Universe — третий студийный альбом шведской мелодик дэт-метал группы Scar Symmetry, вышедший в 2008 году, последний альбом, записанный с вокалистом Кристианом Альвестамом, который вскоре покинул группу.

Видео к композиции «Morphogenesis» было представлено 18 сентября 2008 года.

Список композиций

Участники записи
 Кристиан Альвестам — вокал
 Йонас Кьеллгрен − гитара
 Пер Нильсон − гитара
 Кеннет Сейл − бас-гитара
 Хенрик Ольссон − ударные, тексты песен

Ссылки
 Описание альбома на сайте Nuclear Blast Records

Альбомы Scar Symmetry
Альбомы Nuclear Blast Records