text:
Schedule Your Reduced-Fee Initial Consultation Today
We have helped thousands of clients
nationwide & worldwide in over 75 countries.
International Tax Lawyers: Offshore Voluntary Disclosure Specialist
Who are Golding & Golding?
Our Offshore Tax Attorneys specialize exclusively in IRS Offshore & Streamlined Voluntary Disclosure of domestic & foreign accounts, assets, investments and income. Each case is led by a Board-Certified Tax Attorney Specialist. Our international tax lawyer team at Golding & Golding has helped thousands of taxpayers successfully navigate the complex maze of FBAR & FATCA. Our Tax Attorney & Enrolled Agent team represents clients nationwide and worldwide.
Board-Certified Tax Attorney
Becoming a Board-Certified Tax Specialist is a tough feat. There are more than 200,000 attorneys in California alone, and tens of thousands of them practice in some area of tax, including tax litigation, employment tax, real estate tax, & IRS Offshore Disclosure. Sean M. Golding is one of less than 350 Attorneys (out of more than 200,000 practicing California Attorneys) to earn the Certified Tax Law Specialist credential. The credential is awarded to less than 1% of Attorneys nationwide.
Flat-Fee, Full-Service (Tax & Legal)
Our Offshore Tax Attorney team offers flat-fee, full-service representation for tax preparation, legal representation and IRS tax audit/examination defense. We are the "go-to" international tax lawyers for clients, CPAs, Lawyers, Financial Planners, and businesses across the globe. Our EA and Offshore Voluntary Disclosure Lawyer team handles the entire tax, legal, & examination defense process, from beginning-to-end. Avoid less-experienced firms trying to mislead you.
International Tax Compliance: FBAR & FATCA
What is IRS Offshore Disclosure?
IRS Offshore Disclosure is the process for U.S. Taxpayers to disclose previously unreported foreign accounts, assets, income, & investments. The main programs are: Traditional Voluntary Disclosure Program; Streamlined Filing Compliance Procedures; Delinquent International Informational Return Submission Procedures, and Reasonable Cause. Our Tax Attorneys have helped 1000s of clients get domestic & offshore compliant.
IRS Voluntary Disclosure Program (VDP)
IRS Voluntary Disclosure Program: VDP is the oldest offshore voluntary compliance program. In recent years, the IRS developed several offshore voluntary disclosure tax amnesty compliance programs to allow Taxpayers to report and disclose unreported assets & income. Under the new version of the program, the IRS combined Offshore and Domestic Voluntary Disclosure into one program. Our Tax Attorneys can help you get compliant.
Streamlined Domestic Offshore (SDOP)
Streamlined Domestic Offshore Procedures: When U.S. resident Taxpayers have unreported offshore assets, income, accounts & assets and are non-willful, they may qualify for SDOP, and a reduced a 5% Title 26 offshore penalty. Our Tax Lawyers represent clients in the Streamlined Domestic Offshore Program in order to leverage a smaller penalty now, against a potentially larger penalty later. This reduces the chance of a tax audit or examination in the future.
Streamlined Foreign Offshore (SFOP)
The Streamlined Foreign Offshore Procedures or (SFOP) is a great program for expats and other individuals who do not qualify as a U.S. citizen or legal permanent resident. it a highly cost-effective method of quickly getting you into IRS (Internal Revenue Service) or DOT (Department of Treasury) compliance. Our Tax Attorneys represent you with getting into IRS Tax and Reporting Compliance, without having to pay any penalties. It also allows taxpayers to file original tax returns.
Delinquent Information Returns (DIIRSP)
Delinquent International Information Return Submission Procedures: If you have not filed one or more required international information returns, such as a 5471, 3520-A, or 8865, the IRS may penalize you extensively for not being in "IRS Offshore Compliance." Our Tax Lawyers are very experienced with DIIRSP. The program is designed to help safely bring people into compliance with a reduced risk of an "offshore penalty."
Expatriation, Exit Tax & IRS Offshore Disclosure
Expatriation Tax Lawyers
Expatriation is the process of relinquishing U.S. Citizenship or Legal Permanent Resident Status (Depending on if the filer is a Long-Term Resident). Some expatriates that are considered covered expatriates will have to prepare a shadow sale of their assets using a Mark-to-Market election on Form 8854, and possibly pay an Exit Tax. Our Expat Tax Attorneys can help with offshore disclosure and expatriation.
Covered Expatriate
A covered expatriate is a U.S. citizen or Long-Term Resident that meets one of the three tests. The three test include: the net-worth test ($2M); average tax liability test (~$165,000 5-year average) or the certification of accurate tax filings for the 5 prior years. If a person does not meet the requirements of being a covered expatriate, they will not have an exit tax. Otherwise, the filer may have to pay an Exit Tax.
Calculating Exit Tax
The exit tax is calculated using a Mark-to-Market analysis. Essentially, the person determines the adjusted basis of each asset and FMV on the date before expatriation. There are some exceptions to this rule, including: Eligible deferred compensation items; Ineligible deferred compensation items; Specified tax deferred accounts; and Interests in nongrantor trusts. Deferral of tax is possible.
Reduce & Avoid IRS Offshore Reporting Penalties
FBAR Penalties
FBAR penalties can range extensively. The main categories include: Civil Penalties and Criminal Penalties. Civil FBAR Penalties can be broken down further into Willful and Non-Willful. Non-Willful Penalties can go as high as $10,000 per account, per year. Willful Penalties can reach 50% penalty on the maximum value of the account(s). Our Tax Attorney & EA team helps people reduce, minimize, & avoid non-willful and willful FBAR penalties.
FATCA Penalties
A person may be subject to a FATCA penalty of $10,000. And, if you do not file a correct and complete Form 8938 within 90 days after the IRS mails you a notice of the failure to file, you may be subject to an additional penalty of $10,000 for each 30-day period (or part of a period) during which you continue to fail to file Form 8938 after the 90-day period has expired, up to $50,000. Our Tax Attorneys work to minimize and eliminate FATCA foreign asset penalties.
Form 3520 Penalties
The initial Form 3520 penalty is equal to the greater of $10,000 or: 35% of the gross value of any property transferred to a foreign trust; 35% of the gross value of the distributions received from a foreign trust; 5% of the gross value of the portion of the foreign trust's assets treated as owned by a U.S. person under the grantor trust rules, and potential additional separate penalties as well. Our Tax Attorneys work to minimize and eliminate Form 3520 penalties.
A $10,000 Form 5471 penalty is imposed for each annual accounting period of each foreign corporation for failure to furnish the information required by section 6038(a) within the time prescribed. If the information is not filed within 90 days after the IRS has mailed a notice of the failure to the U.S. person, an additional $10,000 penalty (per foreign corporation) is charged up $50K per failure. Our Tax Attorneys work to minimize and eliminate Form 5471 penalties.
A Form 5472 penalty of $25,000 will be assessed on any reporting corporation that fails to file Form 5472 when due. Each member of a group of corporations filing a consolidated information return is a separate reporting corporation subject to a separate $25,000 penalty, If the failure continues for +90 days after notification by IRS, an additional penalty of $25,000 will apply. Our International Tax Lawyers work to minimize and eliminate Form 5472 penalties.
Form 8621 is a form that is required to be filed by individuals who have a PFIC (Passive Foreign Investment Company) and are not exempt from filing. If you are required to report a form 8621 but failed to do so, that means your tax return is incomplete and the IRS can go back and audit you for years to come, on that return (aka the Statute of Limitations does not expire). This may lead to additional penalties. Our Tax Attorneys work to minimize and eliminate Form 8621 penalties.
A $10,000 Form 8865 penalty is imposed for each tax year of each foreign partnership for failure to furnish the required information within the time prescribed. If the information is not filed within 90 days after the IRS has mailed a notice of the failure to the U.S. person, an additional $10,000 penalty (per foreign partnership) up to a maximum of $50,000 for each failure. Additional penalties may apply. Our Offshore Tax Attorneys work to minimize and eliminate Form 8865 penalties.
A person may be subject to a Form 8938 penalty of $10,000. And, if you do not file a correct and complete Form 8938 within 90 days after the IRS mails you a notice of the failure to file, you may be subject to an additional penalty of $10,000 for each 30-day period (or part of a period) during which you continue to fail to file Form 8938 after the 90-day period has expired, up to $50,000. Our International Tax Attorneys work to minimize and eliminate Form 8938 penalties.
Offshore Tax Fraud Penalties
When a person is liable for international tax fraud or tax evasion, they may be subject to either civil and or criminal tax fraud and evasion penalties. These IRS offshore penalties may result in significant monetary penalties, and penalties on taxes due. In addition, the matter may be referred to an IRS Special Agent investigation, which may lead to prosecution, more financial penalties, & prison. Our Offshore Tax Fraud Attorneys can help minimize fraud risks.
Sean M. Golding - JD, LL.M., EA
International & Offshore Tax Lawyer
Our Managing Partner, Sean M. Golding, is a 20-year attorney with a license in both New York & California and has a Master's degree in Tax Law from University of Denver (where he also completed his undergraduate degree).
Sean M. Golding is one of less than 350 attorneys (out of more than 200,000 practicing California Attorneys) to earn the Board-Certified Tax Law Specialist credential. (Earned by less than 1% of attorneys nationwide). Sean has also earned the prestigious IRS Enrolled Agent credential. He represents clients before the IRS nationwide and worldwide in over 75 countries.
Jenny Minjung Golding
Jenny has been living in Southern California for over 30 years. She earned a Bachelor of Arts in Business Economics and then graduated from USC Gould School of Law (a Top 20 Law School). Jenny has over 15 years of legal experience and works directly with Sean on various complex tax and estate planning matters.
Having grown up helping her immigrant parents forge their way in America, she fully understands how confusing and overwhelming the American legal system can be. Thus, she truly enjoys assisting clients with diverse backgrounds and cultures and helping them with their legal issues.
What is a PFIC (IRS Summary 2020)
Golding and Golding, Board-Certified Tax Law Specialist Comments (0)
PFIC: Revisiting Passive Foreign Investments: PFIC is an IRS acronym that refers to Passive Foreign Investment Companies. The acronym can be misleading to U.S. taxpayers, because it gives the impression that PFIC only refers to...
FATCA Reporting (IRS Summary 2020)
FATCA Reporting: FATCA Reporting is a key enforcement priority, and penalties for not disclosing foreign financial assets is on the rise. In 2020, the IRS will continue aggressive enforcement of FATCA reporting. FATCA (Foreign Account Tax...
FBAR vs 8938 (IRS Summary 2020)
FBAR vs 8938: Comparing IRS Offshore Account Filing Rules: The FBAR vs FATCA Form 8938 is (unnecessarily) complex. The IRS provides some resources, but oftentimes these instructions and publications are unclear. The FBAR is the...
FBAR Insurance Policy & How to Report to IRS (Summary 2020)
FBAR Insurance Policy and how to report foreign life insurance to the IRS: The IRS FBAR Insurance rules for reporting life insurance for foreign policies are very complex. The IRS requires U.S. person owners of a...
Eggshell Audit (IRS Summary 2020)
Eggshell Audit: IRS High Risk Examination & Criminal Exposure: With an eggshell audit, the taxpayer is at a high risk for a potential IRS willful violation, tax fraud, and even a criminal investigation by the...
Foreign Life Insurance Taxation (IRS Summary 2020)
Foreign Life Insurance Taxation: The foreign life insurance taxation rules are complicated. In general, a foreign life insurance policy is an important component of an investment portfolio. When a U.S. person owns a foreign life...
Australian Superannuation Tax Rules in the U.S. (Summary 2020)
U.S. Tax on Australian Superannuation Funds: The U.S tax on Australian Superannuation Funds analysis is complicated and (unnecessarily) complex. U.S. persons who own an Australian Super may have a U.S. tax & reporting requirement for...
Can Green Holders Qualify for OVDP or Streamlined Procedures?
Do Green Holders Qualify for OVDP or Streamlined Procedures? Yes. Green Card Holders do qualify for the IRS (New) OVDP and the Streamlined Filing Compliance Procedures. The streamlined program is an IRS program designed to...
Offshore Cryptocurrency Reporting (IRS Summary 2019-2020)
Offshore Cryptocurrency & IRS: How to Report (2019-2020): The IRS rules for offshore reporting, and specifically foreign cryptocurrency reporting on FBAR & FATCA Form 8938 are still in flux. With the 2019 tax returns coming...
IRS Offshore Penalties (2019-2020 Summary Update)
IRS Offshore Penalties: In recent years, the IRS Offshore Penalties have become progressively worse. How the IRS dings overseas assets & accounts, and issues offshore penalties can be complicated. The Internal Revenue Service has taken...
Offshore Accounts: IRS Reporting Rules & Requirements: The reporting of Offshore Accounts is an enforcement priority for the IRS. The Internal Revenue Service has taken an aggressive position towards foreign accounts compliance. For U.S. persons...
IRS Quiet Disclosure (Summary 2019-2020)
IRS Quiet Disclosure: A Quiet Disclosure IRS involves the filing of late tax returns and international informational returns with the Internal Revenue Service. Quiet disclosure evolved from the increased and aggressive enforcement of foreign accounts...
Offshore Voluntary Disclosure Program (IRS Summary 2020)
Offshore Voluntary Disclosure Program: The Offshore Voluntary Disclosure Program was launched back in 2009 by the IRS. Back in 2009, it was referred to as the Offshore Voluntary Disclosure Initiative), but was later changed to...
Non-Willful FBAR Penalties (2019-2020 Update)
Non-Willful FBAR Penalty: Understanding how the IRS issues a non-willful FBAR penalty(s) can be complex. In recent years, the IRS has taken an aggressive position towards foreign accounts compliance. When a U.S. person has not...
FBAR Penalties (IRS Summary 2020)
FBAR Penalties: The FBAR penalties are on the rise. The IRS has significantly increased enforcement of offshore bank account violations and foreign accounts compliance. FBAR Penalties are more common now than ever. The penalty for...
FBAR Willful Penalties (Updated for 2019-2020)
FBAR Willful Penalty: The IRS FBAR Willful Penalty can be devastating. In recent years, the IRS has taken an aggressive stance against U.S. persons who are out of compliance for offshore assets, accounts, investments or...
IRS Offshore Tax Roundup Top 10 List (2019-2020)
2019 Offshore Tax Roundup: With 2019 coming to an end, and 2020 just around the corner — we wanted to provide you with our Top Ten important IRS offshore tax issues that are crucial for...
Are the Streamlined Offshore Procedures Ending?
When Are the Streamlined Filing Procedures Ending? The Streamlined Filing Offshore Procedures may be closing soon. The IRS developed the streamlined program to assist taxpayers with foreign accounts compliance. The Streamlined Filing Compliance Procedures are...
IRS Offshore Disclosure Testimonials
"The whole process of correcting unresolved tax issues went smoothly as Sean provided me with a courteous, timely and professional service" – Foreign Account Compliance Client
"The reason went with Golding & Golding was that we wanted to work with someone that had both knowledge and expertise as well as actual in-depth experience of working through international tax situations." – Offshore Compliance Client
"Sean has provided us with an outstanding service throughout the streamlined procedure. Sean is straightforward, knowledgeable, reliable and extremely responsive. His empathic approach and ability to explain complicated matters in a simple way are very comforting in such a stressful situation." – IRS Voluntary Disclosure Client
3 years of amended tax returns and 6 years of delinquent FBARs, plus a thoroughly researched reasonable cause statement citing the tax laws of both countries and the treaties between them. All from a jumble of papers faxed from my files. Sean had the issue resolved in less time than it took me to find out what the problem was in the first place" – Offshore Disclosure Client
"The Only Lawyer I don't have to Babysit – His Confidence, Expertise, and Experience are Truly Reassuring…Lastly, Sean cares for his clients. I can not stress how rare it is to find an attorney who genuinely cares." – Reasonable Cause Client
"Mr. Golding was prompt, professional, reassuring (and explained everything patiently and thoroughly) and very attentive. I was not aware about a filing requirement for several years, and he handled the process for me. He was always a pleasure to deal with, and he is as kind as he is skilled." – FATCA & FBAR Disclosure Client.
"Sean closely examined my situation and he educated me of various options available for me. He was very patient and answered all my questions on timely manner. After consulting him I felt relaxed. Sean and his firm were very supportive in the entire process to safely report my offshore accounts to the treasury. Overall I am very satisfied with the outcome." – Streamlined Disclosure Client
"During the entire process, we were extremely impressed with their in-depth knowledge of not only OVDP but also with various other IRS Tax Amnesty Programs, as well as with their professionalism and diligence. It is both an honor and a privilege for us to give them our highest possible recommendation." – OVDP Client
"Mr. Sean M. Golding's empathetic expertise and timely decision-making involved me in positive actions and actual solutions. My results were: no penalties, no legal issues. My own mind now rests easy, at peace." – OVDP & International Estate Tax Client
After hiring him as our tax attorney, Sean did not disappoint. He is always positive and proactive. He basically took my hand and walked me through the complex and ever-changing FATCA and voluntary disclosure maze." — FATCA & OVDP Client
"They did our OVDP. We got our final letter and now we have peace of mind. What a relief, thank you." – OVDP Client with various classes of assets in numerous different countries.
"Mr. Golding, thank you for helping me get through this without any problems." – High-Profile International Tax Law Client with 11 foreign accounts and real estate, while facing civil and criminal penalties


> After over 10 years of hosting http://code4lib.org at Oregon State University Libraries, we'd like to offer up the opportunity to another institution or group.
> The sites are currently hosted on an aging physical server, and we figured this would be a good time to transition.
> OSU has also been managing domain registration for code4lib.org for a few years now.
> Given the need for systems administration, software and security updates, maintenance, backups, etc. we're looking for an institution with sufficient resources to take this on. Making some server accounts for community members available is very important.
> There is also an opportunity to explore moving on from Drupal, since it's overkill for what very little we use it for. But I think it's important to preserve what we've created (especially past conferences) and for the community to control our content. I believe that should be a separate conversation than the hosting though, at least initially.
> I plan to continue assisting with user account management and some other back-end tasks, though I welcome any help with that.
> Let me know if there is serious interest, or if there are other questions or concerns.


text:
Happy Anniversary to the Regulatory Wolves of Wall Street
Friday, July 18, 2014 9:36 AM	by Emma Raymond
Four years after the enactment of Dodd-Frank, small banks are speaking out against the punishing regulations that were included in the 2010 financial reform legislation. In a hearing on Tuesday, the House Financial Services subcommittee on Financial Institutions and Consumer Credit considered several bills that will hopefully alleviate some of the regulatory costs imposed on these struggling banks.
One of the bills discussed was H.R. 3913, which would require federal banking agencies to consider whether a regulation will "promote efficiency, competition and capital formation" before implementing it. This bill and the others considered were attempts at providing a regulatory reprieve for community banks hurt by the passage of Dodd-Frank.
According to new research by AAF, four years after its passage Dodd-Frank's 398 imposed regulations have added upwards of $21.8 billion in regulatory costs and 60.7 million in paperwork burden hours. These costs hit small banks especially hard. According to the Washington Post, in the past four years many local banks and credit unions have merged with one another due to increased regulations.
The hearing on Tuesday also included consideration of a bill that would review President Obama's "Operation Choke Point," a campaign executed by the Justice Department and federal banking regulators that pressures banks to cut services to businesses "the administration considers objectionable." The bill reviewed on Tuesday says that federal banking agencies cannot restrict an "insured depository institution" from providing financial services to a business that is licensed to offer a product or service, registered as a money transmitting business and can demonstrate the legality of its business. In other words, the federal government is overstepping its bounds with this operation.
The hearing on Tuesday was a positive step in considering legislation that will reign in burdensome federal regulations and the costs that they impose. As noted previously by the Cost of Government Center, the regulations in Dodd-Frank that were meant to prevent another financial crisis only kill jobs and force banks to spend more of their resources implementing regulations and less on running profitable businesses. With a significant portion of the law still left to implement, these small banks can expect to see their costs rise if legislation that cuts back these regulations is not passed soon.
TAGS: Spending, Regulation, Financial Services, issues

redpajama_set_name: RedPajamaCommonCrawl


EASY TO FIT SELF CONTAINED UNIT. Brand new Quality range. Detects entry, loud 100db. Ideal for shop or workshop entry, or inside door house alarm, ideal elderly. Uses 4x AAA batteries (not included). Completely self contained Easy to fit , instructions on rear ACTIVATES WHEN DOOR / WINDOW OPENED Dis - arm using keypad. ENTRY / EXIT DELAY Ideal house shop entrance workshop shed etc SIMPLE, DOES THE JOB Fits in 10 mins (screws for hanging not included).


text:
Q: prototype function error : is not a function I tried to encapsulate a javascript object and declared some prototype function. But there were some errors.
Here is my code:
const editor_theme = require('./editor-theme.js')

let defaultTheme = new editor_theme.Editor_Theme('{"titlebar_color": "f0f0f0", "background_color": "ffffff"}')
defaultTheme.setTitlebarColor('888888')
console.log(defaultTheme.getTitlebarColor())

//main.js

module.exports = {
    Editor_Theme: function (data) {
        var _themeData = JSON.parse(data)

        var _titlebar_color = _themeData.titlebar_color
        var _background_color = _themeData.background_color

        const Func = function() { }

        Func.prototype = {
            getTitlebarColor : function () {
                return _titlebar_color
            },
            getBackgroundColor : function () {
                return _background_color
            },
            setTitlebarColor : function (titlebarColor) {
                _titlebar_color = titlebarColor || _titlebar_color
            }
        }

        Object.freeze(Func)
        Object.freeze(Func.prototype)

        return Func
    }

}

//editor-theme.js

The error log is it:

Uncaught TypeError: defaultTheme.setTitlebarColor is not a function

A: Your constructor now returns another constructor function, not an object. Return an instance of that constructor instead:

// module.exports = {
let moduleExports = {

  Editor_Theme: function(data) {

    var _themeData = JSON.parse(data)

    var _titlebar_color = _themeData.titlebar_color
    var _background_color = _themeData.background_color

    const Func = function() {}

    Func.prototype = {
      getTitlebarColor: function() {
        return _titlebar_color
      },
      getBackgroundColor: function() {
        return _background_color
      },
      setTitlebarColor: function(titlebarColor) {
        _titlebar_color = titlebarColor || _titlebar_color
      }
    }

    Object.freeze(Func)
    Object.freeze(Func.prototype)

    return new Func() //Instantiate constructor
  }

}

// const editor_theme = require('./editor-theme.js')
const editor_theme = moduleExports

let defaultTheme = new editor_theme.Editor_Theme('{"titlebar_color": "f0f0f0", "background_color": "ffffff"}')
defaultTheme.setTitlebarColor('888888')
console.log(defaultTheme.getTitlebarColor())

Or even better, just Object.create an object with a custom prototype:

// module.exports = {
let moduleExports = {

  Editor_Theme: function(data) {

    var _themeData = JSON.parse(data)

    var _titlebar_color = _themeData.titlebar_color
    var _background_color = _themeData.background_color

    const prototype = {
      getTitlebarColor: function() {
        return _titlebar_color
      },
      getBackgroundColor: function() {
        return _background_color
      },
      setTitlebarColor: function(titlebarColor) {
        _titlebar_color = titlebarColor || _titlebar_color
      }
    }

    Object.freeze(prototype)

    return Object.create(prototype) //Object with custom prototype
  }

}

// const editor_theme = require('./editor-theme.js')
const editor_theme = moduleExports

let defaultTheme = new editor_theme.Editor_Theme('{"titlebar_color": "f0f0f0", "background_color": "ffffff"}')
defaultTheme.setTitlebarColor('888888')
console.log(defaultTheme.getTitlebarColor())

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction}

Gamma-ray bursts (GRBs) are attractive astrophysics phenomena and
had puzzled astronomers for about twenty-four years after their
discovery in 1973 (Klebesadel et al. 1973). The discovery of
long-lived, multi-band counterparts of GRBs, namely, the afterglows
of GRBs, in 1997 is a watershed in GRB research (Costa et al. 1997;
Van Paradijs et al. 1997; Frail et al. 1997). Soon after that, the
so-called fireball model is recognized as the standard model in
view of the fact that it can explain most features of GRB
observations well. However, as the advance of observation techniques
and the accumulation of observational data, especially after the
launch of \emph{Swift} satellite (Gehrels 2004), a lot of unexpected
behaviours appear in GRB afterglows, such as the canonical
steep-shallow-normal decay and flares in X-ray afterglows, the
flattish decay phase and various rebrightenings in optical
afterglows (For review, see Zhang 2007).

In fact, there are more and more rebrightenings detected in GRB
afterglows, including GRB 970508 (Galama et al. 1998a), GRB 990123
(Sari \& Piran 1999), GRB 021004 (Lazzati et al. 2002), GRB 030329
(Berger et al. 2003), GRB 050525A (Blustin et al. 2006), GRB 050820A
(Cenko et al. 2006), GRB 050721 (Antonelli et al. 2006), GRB 060206
(Stanek et al. 2007; Liu et al. 2008), GRB 070125 (Updike et al.
2008), GRB 070311 (Guidorzi et al. 2007a), GRB 071003 (Perley et al.
2008), GRB 071010A (Covino et al. 2008). Many different mechanisms
have been proposed to explain these rebrightenings, such as density
jump (Lazzati et al. 2002; Dai \& Wu 2003; Tam et al. 2005), energy
injection (Huang et al. 2006), two-component jet (Huang et al. 2004,
2006; Liu et al. 2008), reverse shock (Sari \& Piran 1999),
reverberation of the energy input measured by prompt emission
(Vestrand et al. 2006), turn-on of the external shock (Stanek et al.
2007; Molinari et al. 2007), large angle emission (Panaitescu \&
Kumar 2007), and spectral peak of existing forward shock (Shao \&
Dai 2005).

Among all the mechanisms, the density jump model needs to be paid
special attention to, because density jump in surrounding medium of
GRBs is a very natural hypothesis. Since there are more and more
examples indicating that some GRBs are associated with Type Ic
supernovae (e.g. SN 1998bw/GRB980425, Galama et al. 1998b;
SN2003dh/GRB030329, Price et al. 2003) and many host galaxies of
GRBs are in process of active star formation (Fruchter et al. 1999;
Djorgovski et al. 1998), it is believed that the progenitors of long
GRBs are massive Wolf-Rayet (WR) stars (Woosley 1993). Massive stars
usually produce very strong stellar wind to push the initial
interstellar medium (ISM) in their neighborhood away during their
lifetime. The surrounding of these GRBs should be a wind bubble
following the density profile $\rho \propto r^{-2}$ rather than the
usual homogeneous ISM. Several authors (Castor et al. 1975; Weaver
1977; Ramirez-Riuz et al. 2001) further found that beyond some
typical radius of the wind bubble, the swept-up mass is too large to
be pushed by the wind. As a result, the wind materials pile up at
the edge of the wind bubble to form a density jump.

Lazzati et al. (2002) proposed that a density jump can lead to a
rebrightening in the afterglow. In usual case, when the observing
frequence is between the peak frequence ($\nu_{\rm m}$) and the
cooling frequence ($\nu_{\rm c}$), the amplitude of the
rebrightening should be proportional to the square root of the
density contrast. However, if the density contrast is too high, the
rebrightening will be weakened, since $\nu_{\rm c}$ will decrease
and become less than the observing frequence. In the more detailed
numerical simulations by Huang et al. (2007), no obvious
rebrightenings can be discriminated when the density jump amplitude
is set to 100, which suggests that the simple density jump model is
not an ideal mechanism to produce the rebrightenings. In the recent
studies by Nakar \& Granot (2007) and van Eerten et al. (2009), a
full treatment of the transient features at the jump moment, even
including the thickness of the blastwave, was considered. Thus these
studies should be a more accurate approximation to the reality.
Interestingly, no obvious rebrightenings associated with the density
jumps are found.

In short, a simple density jump model is difficult to explain the
observed rebrightenings in GRB afterglows. On the other hand, the
early afterglows of most GRBs exhibit flattish decays with $\alpha <
0.8$, where $\alpha$ is defined as $F_{\nu} \propto t^{-\alpha}$.
This is difficult to explain using the standard fireball model when
the density profile is $\rho \propto r^{-2}$. Some previous works
have suggested that the microphysics parameters may vary during the
evolution of the fireball (Rossi \& Rees 2003; Ioka et al. 2006; Fan
\& Piran 2006; Panaitescu et al. 2006; Granot, K\"{o}nigl \& Piran
2006). We believe that this kind of variation could resolve these
problems.

In this paper, we show that the observed rebrightenings in GRB
afterglows can be well reproduced by assuming varying microphysics
shock parameters associated with the wind bubble environments. The
outline of our paper is as follows: in \S 2 we introduce our model
detailedly. We then numerically investigate the effects of various
parameters on the afterglows in \S 3, and reproduce the R-band and
X-ray afterglow light curves of GRB 060206, GRB 070311 and GRB
071010A in \S 4. Our discussion and conclusions are presented in \S
5. We use an assumptive cosmology of $H_{\rm 0} = 65$ ${\rm km}$
${\rm s}^{-1}$ ${\rm Mpc}^{-1}$, $\Omega_{\rm M} = 0.30$ and
$\Omega_{\rm \Lambda} = 0.70$ throughout the paper.

\section{Model}

\subsection{Dynamics and radiation process}

In the standard fireball model, the outflow of GRB, which moves
relativistically, interacts with the surrounding medium to form an
external shock. A constant fraction $\xi_{\rm e}$ of the shock
energy will be transferred to the swept-up electrons and accelerate
them to relativistic velocity. Similarly, a constant fraction
$\xi_{\rm B}$ of the shock energy will go to the magnetic field.
These shocked relativistic electrons move in the magnetic field and
emit synchrotron radiation to produce broadband afterglows.

We use the convenient equations developed by Huang et al. (1999,
2000a, 2000b, 2003) to describe the dynamics and radiation process
of the ejecta. The evolution of the bulk Lorentz factor $\gamma$,
the shock radius $R$, and the swept-up medium mass $m$, is described
by three differential equations,
\begin{equation}
\frac{{\rm d} \gamma}{{\rm d} m} = - \frac{\gamma^2 - 1}
       {M_{\rm ej} + \epsilon m + 2 ( 1 - \epsilon) \gamma m},
\end{equation}
\begin{equation}
\frac{{\rm d} R}{{\rm d} t} = \beta c \gamma (\gamma +
\sqrt{\gamma^2 - 1}),
\end{equation}
\begin{equation}
\frac{{\rm d} m}{{\rm d} R} = 2 \pi R^2 (1 - {\rm \cos} \theta) n
m_p,
\end{equation}
where $m_p$ is proton mass, $M_{\rm ej}$ is the initial mass of the
outflow, $\theta$ is the half opening angle of the jet, $n$ is the
number density of the environment, $\beta = \sqrt{\gamma^2 -
1}/\gamma$,  and $\hat{\gamma} \approx (4 \gamma + 1)/(3 \gamma)$ is
the adiabatic index (Dai, Huang, \& Lu 1999). $\epsilon$ is the
radiative efficiency, which equals 1 for a highly radiative case,
and equals 0 in the adiabatic case. We ignore the sideways expansion
of the jet in our model, because many numerical simulations indicate
that it is a very slow process (Granot et al. 2001; Cannizzo,
Gehrels \& Vishniac 2004; Zhang \& MacFadyen 2009). We consider that
the afterglow flux mainly comes from the synchrotron radiation of
the shocked relativistic electrons.

Since the speed of light ( $c$ ) is finite, photons received by the
observer at a particular time $t$ are not radiated simultaneously,
but come from a distorted ellipsoid determined by
\begin{equation}
t=\int \frac{1 - \beta {\rm \cos} \Theta}{\beta c} {\rm d} R \equiv
{\rm const},
\end{equation}
within the jet boundaries, where $\Theta$ is the angle between the
velocity of emitting material and the line of sight. This is the
so-called EATS effect. We integrate
over the EATS to obtain an accurate observed flux in our
simulations (see Huang et al. 2007 for more details).

\subsection{Environment}

Massive stars usually produce very strong stellar wind during their
lifetime. This stellar wind interacts with the initial ISM and forms
two shocks: a reverse shock propagates back into the stellar wind
and a forward shock that propagates into the ISM. The resulting
surrounding medium is broken into four regions (Castor et al. 1975;
Weaver 1977; Ramirez-Riuz et al. 2005; Pe'er and Wijers 2006) as
shown in Figure~1. They are (from inside to outside):
(1) the unshocked stellar wind;
(2) the shocked stellar wind; (3) the shocked ISM; (4) the unshocked
ISM.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f1.eps}} \caption{The
illustration of the density profile used in our model.}
\end{figure}

Region (1) is a stellar wind bubble. The number density of this
region is given by
\begin{equation}
n_1=\frac{\dot M}{4 \pi m_p v_{\rm w} r^2} \propto r^{-2},
\end{equation}
where $\dot M$ is the mass loss rate of the progenitor, $v_{\rm w}$
is the launching speed of the stellar wind and $r$ is the radial
distance from the central star. We fix $v_{\rm w}$ as $10^8$ cm ${\rm
s}^{-1}$ and only vary $\dot M$ in our simulations, since
the density profile of the environment only depends on the
ratio $\dot M/v_{\rm w}$.

As the stellar wind expands, the swept-up mass of the ISM increases
and is finally comparable to the mass in the wind at a radius
$r_{\rm wind}$, which is determined by (Ramirez-Ruiz et al. 2001,
2005)
\begin{equation}
r_{\rm wind}=1.6 \times 10^{18} {\dot M}_{-6}^{3/10} n_{{\rm
ISM},3}^{-3/10} v_{{\rm w},8}^{1/10} t_{\star,6}^{2/5} \rm cm,
\end{equation}
where $n_{\rm ISM,3}$ is the initial density of the homogeneous ISM,
in units of $10^3$ ${\rm cm}^{-3}$, and $t_{\star,6}$
is the life time of the WR phase of the star, in units of $10^6$ yr. Beyond
this radius, in region (2), the swept-up mass is too large to be
pushed away by the wind. The material piles up in this region to form a
density jump. Because of the effect of the reverse wind shock, the
material is hot in this region. The density is approximately
constant and equals to $n_2 = 4n_1(r_{\rm wind})$, where $n_1(r_{\rm
wind})$ is the density in region (1) at the radius of $r = r_{\rm
wind}$.

As shown by Castor et al. (1975), the boundary between Region (2) and
Region (3) is at the radius of
\begin{equation}
r_{2-3}=1.6 \times 10^{19} {\dot M}_{-6}^{1/5} n_{{\rm
ISM},3}^{-1/5} v_{{\rm w},8}^{2/5} t_{\star,6}^{3/5} \rm cm.
\end{equation}
Region (3) is a thin, dense shell containing most of the swept-up
ISM. Its width is only about $r_{2-3}/12$ and the density in this region
is about $4n_{\rm ISM}$. Here $n_{\rm ISM}$ is also the density in region
(4).

We use the density profile introduced above as the environment
surrounding GRBs in this paper. As discussed by Pe'er and Wijers
(2006), for a GRB event, the blast wave can not reach Region (3) in
the relativistic phase. Our numerical results also prove that the
fireball is in Region (1) and Region (2) during typical observable
time. So we only use Region (1) and Region (2) as the environment in
our work. For simplicity, we take $r_{\rm wind}$ as a free parameter
in our calculations, so that we do not need to consider the detailed
values of $v_{\rm w}$ and $t_{\star}$.

Unfortunately, the simple density jump model alone is difficult to explain
the rebrightenings in GRB afterglows (Huang et al. 2006, 2007; Nakar \&
Granot 2007). Moreover, the early optical and/or X-ray
afterglow light curves of some GRBs are flatter than the prediction of a
normal fireball in a simple wind environment. So we need to
consider other effects. Varying microphysics shock parameters should be
a possible solution.

\subsection{Microphysics parameters}

In the standard afterglow model, it is usually assumed that the
microphysical parameters are constant throughout the evolution of
the fireball. However, the actual microphysical processes in the
relativistic shocks, for example, the energy transfer from protons
to electrons and magnetic fields, are still not clearly known. It is
possible that the microphysical parameters are variational. In fact,
the variation of the microphysics parameters during the evolution of
the fireball has been considered in many previous studies (Rossi \&
Rees 2003; Ioka et al. 2006; Fan \& Piran 2006; Panaitescu et al.
2006; Granot, K\"{o}nigl \& Piran 2006). Fan \& Piran (2006) and
Panaitescu et al. (2006) have engaged the assumption that the
equipartition factors $\xi_{\rm e}$ and $\xi_{\rm B}$ are functions
of $\gamma$ to explain the shallow decay phase in some X-ray
afterglows. Here we will use a similar idea to investigate the
observed rebrightenings in GRB afterglows.

In our model, the circum-burst environment is divided into two parts,
i.e. Region (1) and Region (2). The material in Region (1) is the
unshocked stellar wind thrown by the mass star. In
Region (2) the material consists of the shocked stellar wind mixed
with a small fraction of the swept-up ISM. It is hot because of the
effect of the reverse wind shock (Castor et al. 1975; Weaver 1977;
Ramirez-Riuz et al. 2005; Pe'er and Wijers 2006). We can imagine
that the physical condition, such as the strength of the magnetic
field, the temperature and density of the material, could be different
between these two regions, so the evolution of microphysics
parameters may also be different accordingly. In our study, we use different
parameters for these two regions. We assume that
\begin{equation}
\xi_e=\xi_{e,0} \gamma^{-\alpha1},
\end{equation}
\begin{equation}
\xi_B=\xi_{B,0} \gamma^{-\alpha1}
\end{equation}
in Region (1), and
\begin{equation}
\xi_e=\xi_{e,0} \gamma^{-\alpha2},
\end{equation}
\begin{equation}
\xi_B=\xi_{B,0} \gamma^{-\alpha2}
\end{equation}
in Region (2).

\section{Numerical Results}

In this section, we present our numerical results to show the
effects of various physical parameters on the R-band light curves,
using the model described in \S 2. For convenience, we first define
a set of ``standard'' parameters, as shown in the second column
of Table 1.
\begin{table*}
 \centering
 \begin{minipage}{100mm}
  \caption{Modeling Parameters}
  \begin{tabular}{c c c c c}
\hline \hline Parameters & Standard & GRB 060206 & GRB 070311 & GRB 071010A\\
\hline
$z$ & 1.0 & 4.045 & 1.0 & 0.98\\
$E_0$ (ergs) & $1.0 \times 10^{53}$ & $9.0\times 10^{52}$ & $8.0 \times 10^{51}$ & $1.3 \times 10^{52}$\\
$\theta_0$ (rad) & 0.1 & 0.06 & 0.08 & 0.11\\
$\dot M$ ($M_\odot/{\rm yr}$) & $1.0 \times 10^{-6}$ & $2.0 \times 10^{-5}$ & $6.0 \times 10^{-6}$ & $4.0 \times 10^{-5}$\\
$r_{\rm wind}$ (${\rm cm}$) & $1.0 \times 10^{18}$ & 3$.0 \times 10^{16}$ & $2.0 \times 10^{17}$ & $5.1 \times 10^{16}$\\
$p$ & 2.5 & 2.2 & 2.3 & 2.1\\
$\xi_{e,0}$ & 0.1 & 0.3 & 0.3 & 0.3\\
$\xi_{B,0}$ & 0.01 & 0.03 & 0.03 & 0.03\\
$\alpha1$ & 1.5 & 1.2 & 0.9 & 1.5\\
$\alpha2$ & 1.3 & 0.6 & 0.0 & 0.6\\
\hline
\end{tabular}
\end{minipage}
\end{table*}

Figure 2 illustrates the effect of the parameter $\theta_0$ on the
R-band light curves. The solid line corresponds to the ``standard''
parameters. The dashed line corresponds to $\theta_0 = 0.3$ rad and
the dotted line corresponds to $\theta_0 = 0.03$ rad. We can see
that when the change of microphysics parameters is considered, an
obvious rebrightening appears. Interestingly, when $\theta_0$ is
larger, the duration of the rebrightening becomes longer. This is
not difficult to understand. The afterglow brightness is dominated
by the high latitude emission, so that the EATS shows a ring-like
pattern. As a result, the brightness will be kept on a relatively
higher level after the density jump moment, to form a flat phase.
When $\theta_0$ becomes larger, the time delay of the photons from
the edge of the outflow also becomes larger. So the flat phase is
longer.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f2.eps}} \caption{The effect
of the parameter $\theta_0$ on the R-band light curve. The solid
line corresponds to the standard parameters. The dashed line
corresponds to $\theta_0 = 0.3$ rad and the dotted line corresponds
to $\theta_0 = 0.03$ rad.}
\end{figure}

Environment is an important factor that affects the evolution of GRB
afterglows. As mentioned before, the character of wind environment
is mainly determined by the ratio $\dot M/v_{\rm w}$. We fix $v_{\rm
w}$ as $10^8$ cm ${\rm s}^{-1}$ and only vary $\dot M$ here to
investigate the effect of the parameter $\dot M$ on the R-band light
curves. The results are shown in Figure 3. The solid line
corresponds to the ``standard'' parameters. The dashed line
corresponds to ${\dot M} = 1.0 \times 10^{-5}$ $M_\odot/{\rm yr}$
and the dotted line corresponds to ${\dot M} = 1.0 \times 10^{-7}$
$M_\odot/{\rm yr}$. It is clearly seen that for a smaller $\dot M$
value, the rebrightening appears earlier and the flux before the
rebrightening are lower. This result is easy to understand. A
smaller $\dot M$ corresponds to a smaller density, and the
deceleration of the external shock is slower. So the Lorentz factor
is larger and the fireball can meet the density jump earlier. A
larger Lorentz factor also makes $\xi_{\rm e}$ and $\xi_{\rm B}$
smaller and decreases the flux.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f3.eps}} \caption{The effect
of the parameter $\dot M$ on the R-band light curve. The solid line
corresponds to the ``standard'' parameters. The dashed line corresponds
to ${\dot M} = 1.0 \times 10^{-5}$ $M_\odot/{\rm yr}$ and the dotted
line corresponds to ${\dot M} = 1.0 \times 10^{-7}$ $M_\odot/{\rm
yr}$.}
\end{figure}

The parameter $r_{\rm wind}$ is another factor to describe the
character of the environment. The effect of $r_{\rm wind}$ on the
R-band light curve is illustrated in Figure 4. The solid line
corresponds to the ``standard'' parameters. The dashed line
corresponds to $r_{\rm wind} = 5.0 \times 10^{18} {\rm cm}$ and the
dotted line corresponds to $r_{\rm wind} = 5.0 \times 10^{17} {\rm
cm}$. We can see that the rebrightening appears earlier when $r_{\rm
wind}$ is smaller, because $r_{\rm wind}$ determines the position of
the density jump.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f4.eps}} \caption{The effect
of the parameter $r_{\rm wind}$ on the R-band light curve. The solid
line corresponds to the ``standard'' parameters. The dashed line
corresponds to $r_{\rm wind} = 5.0 \times 10^{18} {\rm cm}$ and the
dotted line corresponds to $r_{\rm wind} = 50 \times 10^{17} {\rm
cm}$.}
\end{figure}

The effect of the parameter $\alpha1$ on the R-band light curve is
shown in Figure 5. The solid line corresponds to the ``standard''
parameters. The dashed line corresponds to $\alpha1 = 1.7$ and the
dotted line corresponds to $\alpha1 = 1.3$. It is obvious that a
larger $\alpha1$ makes the flux before the rebrightening lower. This
is not difficult to understand. With the increase of $\alpha1$, the
values of $\xi_e$ and $\xi_B$ before the rebrightening become
smaller. This suppresses the radiation flux at early time.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f5.eps}} \caption{The effect
of the parameter $\alpha1$ on the R-band light curve. The solid
line corresponds to the ``standard'' parameters. The dashed line
corresponds to $\alpha1 = 1.7$ and the dotted line corresponds to
$\alpha1 = 1.3$.}
\end{figure}

The effect of the parameter $\alpha2$ on the R-band light curve is
illustrated in Figure 6. The solid line corresponds to the
``standard'' parameters. The dashed line corresponds to $\alpha2 =
1.5$ and the dotted line corresponds to $\alpha2 = 1.1$. As
expected, the effect of $\alpha2$ is similar to that of $\alpha1$
for the same reason.
\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f6.eps}} \caption{The effect
of the parameter $\alpha2$ on the R-band light curve. The solid
line corresponds to the ``standard'' parameters. The dashed line
corresponds to $\alpha2 = 1.5.$ and the dotted line corresponds to
$\alpha2 = 1.1$.}
\end{figure}

\section{Comparison With Observations}

In this section we select three GRBs with obvious rebrightenings in
both optical and X-ray bands, i.e. GRB 060206, GRB 070311 and GRB
071010A, and reproduce their R-band and X-ray afterglow light curves
numerically, using the model described in \S 2.

\subsection{GRB 060206}

GRB 060206 was detected at 04:46:53 UT on Feb. 6 by the Burst Alert
Telescope (BAT) onboard the \emph{Swift} satellite (Morris et al.
2006). The temporal profile of the BAT light curve shows a single
peak, with a total fluence of $8.4 \pm 0.4 \times 10^{-7}$ erg ${\rm
cm}^{-2}$ in the 15-350 keV band (Morris et al. 2006; Palmer et al.
2006). The total duration of the burst is $T_{90} = 7 \pm 2 {\rm
s}$, suggesting that it is a long-duration GRB (Palmer et al. 2006).

The UVOT telescope onboard the \emph{Swift} satellite first observed
the optical afterglow of GRB 060206 and found it located at the
position of $\alpha = 13^h31^m43^s.416$, $\delta =
+35^{\circ}03'03''.6$ (J2000.0; Boyd et al. 2006), corresponding to
the Galactic extinction of $A_R = 0.033$ mag (Schlegel, Finkbeiner
\& Davis 1998). After that, a number of telescopes made detailed
follow up observations, such as the 2-m robotic Liverpool Telescope
(Monfardini et al. 2006), the Rapid Telescopes for Optical Response
(RAPTOR; Wo\'zniak et al. 2006) and the MDM telescope (Stanek et al.
2007). From the calibrated ALFOSC spectrum of the afterglow, Fynbo
et al. (2006) determined the redshift of GRB 060206 as $z = 4.045$.
X-ray afterglow was also detected by XRT on \emph{Swift} at 58 s
after the trigger (Morris et al. 2006).

There are significant rebrightenings in both the optical and X-ray
afterglows of GRB 060206 at about 3000 s after the burst. Liu et al.
(2008) suggested that the rebrightening comes from a jet-like ejecta
with a larger viewing angle, which is produced by the central
engine.

Here we try to use our model described in \S 2 to reproduce the
rebrightenings in both R-band and X-ray light curves of GRB 060206.
Our best-fit physical parameters are presented in Table 1, and our
modeling curves are illustrated in Figure 7. The observed R-band
data are taken from Monfardini et al. (2006), Wo\'zniak et al. 2006
and Stanek et al. (2007), and the X-ray data are taken from the
\emph{Swift} XRT light curve repository\footnote{$\rm
http://www.swift.ac.uk/xrt_-curves/$} (Evans et al. 2007). We can
see in Figure 7 that our model can generally reproduce the light
curves well. Note that at the late stage, the observed X-ray light
curve is obviously too flat as compared with our theoretical result.
This may be due to the contamination from a nearby source, as
already mentioned by Stanek et al. (2007).

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f7.eps}} \caption{Our best
fit to the R-band and X-ray afterglow light curves of GRB 060206.
The lines are our theoretical curves and the fitting parameter
values are given in Table 1. The R-band observed data are taken from
Monfardini et al. (2006), (Wo\'zniak et al. 2006) and Stanek et al.
(2007), and the X-ray data are taken from the \emph{Swift} XRT light
curve repository (Evans et al. 2007). All optical data points have
been corrected for the Galactic extinction (Schlegel, Finkbeiner \&
Davis 1998).}
\end{figure}

\subsection{GRB 070311}

GRB 070311 occurred at 01:52:50 UT on 2007 March 11 and was detected
by the INTEGRAL/IBAS in IBIS/ISGRI data. The duration of the
$\gamma$-ray prompt emission is about 50 s in the 20-200 keV band,
with the peak flux of 0.9 photons ${\rm cm}^{-2}$ ${\rm s}^{-1}$ (1
s integration time) and the total fluence of $2 \times 10^{-6}$ erg
${\rm cm}^{-2}$ (Mereghetti et al. 2007).

The afterglow of GRB 070311 was first discovered by the Rapid Eye
Mount (REM) telescope at 55 s after the burst. A bright fading
source was found at $\alpha = 05^h50^m08^s.21$, $\delta =
+03^{\circ}22'30''.3$ (J2000.0; Covino et al. 2007). This location
has a low Galactic latitude ($l = 202^{\circ}.766, b =
-11^{\circ}.998$ in Galactic coordinates), so the Galactic
extinction is as much as $A_R = 2.038$ mag (Schlegel, Finkbeiner \&
Davis 1998). X-ray afterglow was also found by the observations of
XRT on \emph{Swift} at about 7000 s after the trigger (Guidorzi et
al., 2007b).

The optical afterglow of GRB 070311 has complex structures. Besides
a normal power law decay, there are two fast rise exponential decay
(FRED) shaped pulses peaking around 80 and 140 s after the peak of
the GRB and possibly accompanied by the tail of prompt $\gamma$-ray
emission (Guidorzi et al. 2007a). Another structure, which is the
most attractive feature, is a significant late rebrightening between
$3 \times 10^4$ s and $2 \times 10^5$ s after the trigger in both
optical and X-ray bands (Guidorzi et al. 2007a). Guidorzi et al.
(2007a) have used a power law function plus a FRED shaped pulse to
fit the afterglows in both R and X-ray bands. More physically, they
suggested that the late afterglow rebrightening of GRB 070311 can
come from a refreshed shock. Additionally, they argued that the
density jump in the surrounding medium can be the origin of the
rebrightening too, but less appealing.

Here we use our model described in \S 2 to reproduce the late
rebrightenings in both R-band and X-ray light curves of GRB 070311.
We take the observed R-band data from Guidorzi et al. (2007a; for
REM data) and GCN circulars (Cenko 2007; Dai et al. 2007; Garnavich
et al. 2007; Halpern \& Armstrong 2007a,b,c,d; Jel\'inek, Kub\'anek
\& Prouza 2007; Kann 2007; Wren et al. 2007), and the X-ray data
from the \emph{Swift} XRT light curve repository (Evans et al.
2007). Because the redshift of GRB 070311 is still unknown, we
simply assume a redshift of $z = 1.0$ in our calculation. Our
best-fit physical parameters are presented in Table 1, and our
modeling curves are illustrated in Figure 8. We see that the
interpretation of our model to this event is also generally
acceptable.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f8.eps}} \caption{Our best
fit to the late rebrightenings in the R-band and X-ray light curves
of GRB 070311. The lines are our theoretical curves and the fitting
parameter values are given in Table 1. The R-band observed data are
taken from Guidorzi et al. (2007a; for REM data) and GCN circulars
(Cenko 2007; Dai et al. 2007; Garnavich et al. 2007; Halpern \&
Armstrong 2007a,b,c,d; Jel\'inek, Kub\'anek \& Prouza 2007; Kann
2007; Wren et al. 2007), and the X-ray data are taken from the
\emph{Swift} XRT light curve repository (Evans et al. 2007). All
optical data points have been corrected for the Galactic extinction
(Schlegel, Finkbeiner \& Davis 1998).}
\end{figure}

\subsection{GRB 071010A}

GRB 071010A triggered the \emph{Swift} satellite at 03:41:12 UT on
2007 Oct. 10 (Moretti et al. 2007). It is a traditional long GRB
with the burst duration of $T_{90} = 6 \pm 1 {\rm s}$. The total
fluence of the burst is about $2.0 \times 10^{-7}$ erg $ {\rm
cm^{-2}}$ (Krimm et al. 2007).

TAROT telescope identified the optical afterglow of GRB 071010A
firstly, only 124 s after the trigger (Klotz, Boer \& Atteia, 2007).
Bloom et al. (2007) further found that the position of the burst was
$\alpha = 19^h12^m14^s.624$, $\delta = -32^{\circ}24'07''.16$
(J2000.0), corresponding to the Galactic extinction of $A_R = 0.263$
mag (Schlegel, Finkbeiner \& Davis 1998). Spectral observations were
done subsequently by Keck and the analysis of the Mg II and Fe II
lines gave the redshift of the burst as $z = 0.98$ (Prochaska et al.
2007). X-ray data were also acquired by XRT observations on
\emph{Swift} (Guidorzi et al. 2007b), but no radio afterglow was
detected at 8.46 GHz until almost 2 days after the burst (Chandra \&
Frail 2007).

The most interesting feature of the afterglows of GRB 071010A is the
appearance of a sharp rebrightening at about 0.6 days after the GRB,
clearly seen in both optical and X-ray bands. Covino et al. (2008)
have used a Beuermann et al. (1999) function, and a simple step
function for the rebrightening, to fit the afterglows. They
suggested that the rebrightening was due to an injection of abundant
energy, which was comparable to the initial energy in the fireball.
The steepening after the rebrightening was interpreted as a jet
break at around 1 day after the burst.

We try to use our model introduced in \S 2 to reproduce the R-band
and X-ray light curves of GRB 071010A. In our modeling, the observed
R-band data are taken from Covino et al. (2008), and the X-ray data
are taken from the \emph{Swift} XRT light curve repository (Evans et
al. 2007). Our best-fitting physical parameters are presented in
Table 1, and our modeling curves are illustrated in Figure 9. It is
clear that our model can reproduce the rebrightening features of GRB
071010A very well.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{f9.eps}} \caption{Our best
fit to the R-band and X-ray afterglow light curves of GRB 071010A.
The lines are our theoretical curves and the fitting parameter
values are given in Table 1. The R-band observed data are taken from
Covino et al. (2008), and the X-ray data are taken from the
\emph{Swift} XRT light curve repository (Evans et al. 2007). All
data points have been corrected for the Galactic extinction
(Schlegel, Finkbeiner \& Davis 1998).}
\end{figure}

\section{Discussion and Conclusion}

In the standard fireball model, it is assumed that the circum-burst
medium density is constant or following a single $\rho
\propto r^{-2}$ law. The microphysics shock parameters are also
usually assumed invariable during the evolution of the fireball.
These models can basically explaining many pre-$Swift$
GRB afterglows, whose spectrum and
light curves can be approximated as broken power-law functions
(Panaitescu \& Kumar 2001a, 2001b; Yost et al. 2003). The launch of
\emph{Swift} satellite (Gehrels 2004) makes it possible to
observe early afterglows of many GRBs in the first few hours after the
trigger. Many remarkable and unexpected features are found,
such as marked rebrightenings and the flattish decay phase in early GRB
afterglows.

In fact, the standard fireball model is obviously too simplified. If
long GRBs indeed originate from the death of massive stars, the
environment of GRBs should have complex structures rather than have
a constant or single power law profile. Some analytical (Castor et
al. 1975; Weaver 1977; Ramirez-Riuz et al. 2005; Pe'er and Wijers
2006) and numerical (Ramirez-Riuz et al. 2001) studies suggest that
the circum-burst density profile should be a wind bubble, associated
with a few density jumps. On the other hand, the microphysics
parameters, such as $\xi_{\rm e}$ and $\xi_{\rm B}$, may vary during
the evolution of the fireball (Rossi \& Rees 2003; Ioka et al. 2006;
Fan \& Piran 2006; Panaitescu et al. 2006; Granot, K\"{o}nigl \&
Piran 2006). Actually, the fast decrease of the cooling frequency
$\nu_c$ in some GRBs suggests that $\xi_{\rm B}$ may be evolving
(Panaitescu et al. 2006). Some previous studies also suggest that
$\xi_{\rm e}$ and $\xi_{\rm B}$ may be different for the forward
shock and the reverse shock (Fan et al. 2002; Wei, Yan \& Fan 2006),
and may also be different for Region (1) and Region (2) (Gebdre et
al. 2007; Kamble, Resmi \& Misra 2007). So, $\xi_{\rm e}$ and
$\xi_{\rm B}$ may depend on the strength of the shock and the
environment.

In our study, we combine the wind bubble environments and the change
of microphysics shock parameters together. Comparing with the
standard fireball model, our model has three more parameters (i.e.
$r_{\rm wind}$, $\alpha1$ and $\alpha2$).  We find that this model
can produce the observed rebrightenings and flattish decay in GRB
afterglows successfully. We have shown that the observed
rebrightenings in both the optical and X-ray afterglow light curves
of GRB 060206, GRB 070311 and GRB 071010A can be well explained by
our model.

We have also investigated the effects of various parameters on the
light curves numerically. We can imagine that if the
stellar wind produced by the progenitor is very strong, or the
launching speed of the stellar wind $v_{\rm w}$ is small, or
the value of $r_{\rm wind}$ is large enough, there will be no
rebrightening within the usual observation time.
So, basically the wind bubble environment can also give birth to
a steadily decaying afterglow that shows no rebrightening.

In our work, we neglect the effect of the reverse shock.
According to the study by Dai \& Lu (2002),
when an ultrarelativistic blast wave interacts with a density jump
medium, the resulting reverse shock is relativistic only if the
amplitude of the density jump is much larger than 21. In our model, the
amplitude of the density jump is only 4, so the corresponding reverse
shock is Newtonian. The emission from the Newtonian reverse shock is
very weak, and can be omitted.
Moreover, although we use an abrupt density jump, the actual increase
of density may be gradual. In this situation, the emission
from the reverse shock will even be much weaker.

Currently, a complete understanding of the microphysical processes
in the relativistic shocks is still lacking. Using the derived
microphysical parameters from GRB modeling, people may be able to
get some constraints on the shock physics. The derived parameter
values of $\dot M$ and $n_{\rm ISM}$ are also very important. They
are closely related to the evolution and the environment of the
massive star. They may give some hints on the characters of the
progenitor, such as the initial main-sequence mass and the
metallicity. So, from the modeling parameters, we can also obtain
some useful information about GRB origin.

\section*{Acknowledgments}

We thank the anonymous referee for stimulating suggestions that lead
to an overall improvement of this study. We also would like to thank
Kinwah Wu, Z. G. Dai and X. Y. Wang for helpful suggestions and
discussion. This research was supported by a 2009 GRF grant of Hong
Kong Government (grants 701109), the National Natural Science
Foundation of China (grants 10625313), and the National Basic
Research Program of China (973 Program 2009CB824800).

redpajama_set_name: RedPajamaArXiv


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text:
export const REQUEST_PRODUCTS = 'REQUEST_PRODUCTS'
export const RECEIVE_PRODUCTS = 'RECEIVE_PRODUCTS'
export const REQUEST_PRODUCT = 'REQUEST_PRODUCT'
export const RECEIVE_PRODUCT = 'RECEIVE_PRODUCT'
export const TOGGLE_ACTIVE_PRODUCT = 'TOGGLE_ACTIVE_PRODUCT'
export const ENABLE_PRODUCT_SENDING = 'ENABLE_PRODUCT_SENDING'

redpajama_set_name: RedPajamaGithub


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text:
Watching Waters Rise Right Outside the Front Door
Home / Maritime Executive / Watching Waters Rise Right Outside the Front Door
By MarEx 2015-08-27 19:02:39
For the past two centuries, two trends have been steady and clear around the United States. Sea level has been rising, and more people have been moving closer to the coast.
As the ocean has warmed, polar ice has melted, and porous landmasses have subsided, global mean sea level has risen by 8 inches (20 centimeters) since 1870. The rate of sea level rise is faster now than at any time in the past 2,000 years, and that rate has doubled in the past two decades.
Tide gauges have been used to measure sea level for more than 130 years. Satellite measurements now complement the historical record. (NASA Earth Observatory image by Joshua Stevens, based on data from the Commonwealth Scientific and Industrial Research Organization and NOAA)
That has not stopped people from buying and building along the coast. About 55 to 60 percent of U.S. citizens live in counties touching the Atlantic or Pacific Ocean, the Gulf of Mexico, or the Great Lakes. A recent study by business and finance leaders found that $66 billion to $106 billion worth of coastal property is likely to sit below sea level by 2050.
The nation's problem is also NASA's problem, and not just because several satellites and hundreds of Earth scientists are monitoring the rising seas. Sea level rise hits especially close to home because half to two-thirds of NASA's infrastructure and assets stand within 16 feet (5 meters) of sea level. With at least $32 billion in laboratories, launch pads, airfields, testing facilities, data centers, and other infrastructure spread out across 330 square miles (850 square kilometers)—plus 60,000 employees—NASA has an awful lot of people and property in harm's way.
It is estimated that more than 50 percent of the United States population lives in coastal counties. (NASA Earth Observatory map by Joshua Stevens, using data from the NASA Socioeconomic Data Applications Center)
For NASA climatologist Cynthia Rosenzweig, the urgency of the problem was crystallized in the summer of 2009. As part of a climate change preparedness workshop, she joined other scientists, engineers, facility managers, and administrators on a tour of launch pads 39A and B at Kennedy Space Center. Since the Apollo-Saturn rocket days, and through 25 years of space shuttles, those two launch pads have been critical to NASA's mission.
But when Rosenzweig got off the bus and looked around, she could see that the shrinking dunes and damaged shoreline were just a stone's throw from the launch pads. "Every NASA center has its own set of vulnerabilities, and some are more at risk than others," Rosenzweig said. "But sea level rise is a very real challenge for all of the centers along the coast."
The Coast is the Place to Be
"NASA is on the coast because that's the right place to launch from," said Kim Toufectis, a facilities planner in NASA's Office of Strategic Infrastructure.
The U.S. government long ago made the choice to fly most of its rockets and experimental aircraft from the coast because failures happen, and they are less dangerous to the public when they happen over water than over land. But launching from the coast requires testing, storage, and spacecraft assembly facilities to be nearby. So if you are going into space from the United States, you are going to have to face down the challenge of rising seas.
The majority of NASA centers and facilities are on or very near the coast.
As at Kennedy, the launch pads and buildings at Wallops Flight Facility stand just a few hundred feet from the Atlantic Ocean. Langley Research Center is situated along the Back River, near the mouth of Chesapeake Bay. Ames Research Center is tucked into the south end of San Francisco Bay. Johnson Space Center sits on Clear Lake, an inlet off of Galveston Bay. Those centers all stand between 5 and 40 feet (2 and 12 meters) above mean sea level. The math is nearly upside down at Michoud Assembly Facility, which sits behind levees near the Mississippi River and Lake Pontchartrain.
In a review of the agency's vulnerability to sea level rise, NASA's Climate Adaptation Science Investigators (CASI) Working Group recently wrote:
Sea level rise of between 13 and 69 centimeters by the 2050s is projected for NASA's five coastal centers and facilities…Even under lower sea level rise scenarios, the coastal flood event that currently occurs on average once every 10 years is projected to occur approximately 50 percent more often by the 2050s in the Galveston/Johnson Space Center area; 2 to 3 times as often near Langley Research Center and Kennedy Space Center; and 10 times more frequently in the San Francisco Bay/Ames Research Center area. NASA coastal centers that are already at risk of flooding are virtually certain to become more vulnerable in the future.
The maps above show the amount of forecasted sea level rise at coastal NASA centers. The rings represent the relative amount of rise in each place, and do not show inundated areas. (NASA Earth Observatory maps by Joshua Stevens, using data from the Climate Adaptation Science Investigators (CASI) working group)
If you think about the height of the sea surface like the height of the water in a calm bathtub, then a rise of a few tens of centimeters over a few decades doesn't sound like much. But sea level doesn't rise evenly; it piles up more in some places because of natural wind and current patterns. And turbulence matters: Think about that bathtub with a child sloshing around in it. Waves can roll up one side and then the other, sometimes splashing over the brim. The higher the flat-water line, the greater the chance that the water will slosh out of the basin when it is stirred up by storms and winds.
Sea level also matters in a horizontal direction. An old rule of thumb is that one inch of vertical change in sea level translates into 100 inches of horizontal beach loss on a flat beach or marsh. In this way, a little bit of sea level rise can translate into a lot of water moving inland with storms or abnormally high tides.
"Sea level is important because it gradually moves the high-tide line farther up the beach and closer to buildable land," said John Jaeger, a coastal geologist from the University of Florida. "It also allows storm surges to penetrate farther inland."
Launching from a Sandbar
The high-tide line has been moving landward for some time at Kennedy Space Center on Florida's east coast. Located within the Merritt Island National Wildlife Refuge and adjacent to Cape Canaveral Air Force Station, NASA's most famous center covers more than 66 square miles (170 square kilometers) and holds about 20 percent of the agency's constructed assets. Most of it is built on coastal marshland about five to 10 feet above sea level.
Conservative climate models project that the seas off Kennedy will rise five to eight inches by the 2050s, and nine to 15 inches by the 2080s. If ice sheets in Greenland and Antarctica continue to melt as quickly as current measurements indicate, those numbers could become 21 to 24 inches by the 2050s and 43 to 49 inches by the 2080s.
"We consider sea-level rise and climate change to be urgent," said Nancy Bray, spaceport integration and services director for Kennedy.
Even as the space center was founded in 1961, management and scientists were aware that seas were rising and could someday pose a threat. But in that era, the challenge was to get to the Moon as soon as possible. There was an established Air Force station nearby with access to orbits that could not be obtained from anywhere else in the United States. The choice was easy, and it was right for the time.
But time has not been kind to this stretch of sand. Based on historical records and aerial photos, the beach in front of Kennedy has thinned and moved inland by as much as 200 feet (60 meters). The losses have been most acute and persistent along a stretch near the center's two most prized launch pads. Complex 39A was recently leased for 20 years to Space X, which intends to use it for its Falcon heavy lift rocket. NASA's new Space Launch System and Orion spacecraft are slotted for Complex 39B within the next decade. The Atlantic Ocean stands less than a quarter mile from both.
Crashing waves and sandy shoreline are not far from the launchpads at Kennedy Space Center. That distance is decreasing each year. (NASA Earth Observatory image by Joshua Stevens, using Landsat data from the U.S. Geological Survey)
In 2004, three hurricanes crossed the Florida peninsula. And while none made a direct hit on Cape Canaveral, they collectively caused $100 million in damage to the space center. Then a nor'easter in 2007 sat offshore for two weeks and battered the beach; Tropical Storm Fay then raked the beach again in 2008.
In response to the persistent storm damage, Kennedy facilities managers contracted to build a 15-foot-high, 725-foot-long dune as a proof of concept for a managed retreat. Center scientists and engineers also worked with the U.S. Geological Survey to map the shape of the beach (topography) with laser ranging and detection (LiDAR). Then they enlisted coastal geologists John Jaeger and Pete Adams of the University of Florida to figure out why sand dunes near launch Complexes 39A and B were so persistently being washed away.
For five years, Jaeger, Adams, and graduate students pulled GPS mapping gear up and down 6 miles of beach at least once a month—more often in the wake of storms. The goal was to build a three-dimensional model of the area. They found that the beaches were retreating due to the shape of the seafloor just offshore, where gaps between the sandbars channel wave energy toward certain areas. But they also found sand piling up (accreting) in other areas, mostly near Launch Complex 40. The beach is migrating south, even if NASA's infrastructure is not.
In 2012, Hurricane Sandy offered a glimpse of the new normal along the Atlantic coast. The storm passed 200 miles offshore from Kennedy, but it moved so slowly that the heavy surf scoured the beach for three or four high-tide cycles. By the time the skies cleared, the dunes along a 2-mile (3-kilometer) stretch near Complexes 39A and B had retreated as much as 65 feet (20 meters). Nearly 650 feet (200 meters) of railroad track in the vicinity of 39A were undermined by the storm surge. The high-tide line moved closer to a service road, under which lay some of the center's natural gas, communications, liquefied rocket fuel, and water lines. That road sits just 4 feet (1.2 meters) above sea level.
Hurricane Sandy had wind, wave, or water impacts on five NASA centers along the U.S. East Coast. (NASA Earth Observatory image by Jesse Allen, using Suomi NPP VIIRS data provided by NOAA CLASS)
Rising to Future Challenges
So what does NASA do as the seas rise around its facilities? Cynthia Rosenzweig has an answer: flexible adaptation pathways.
"What makes sense for us to do now? And what might we have to do later?" she said. "We have to consider and understand the risks, and then build something that can be adjusted."
Rosenzweig conducts her research at NASA's Goddard Institute for Space Studies and Columbia University, both of which stand on the Hurricane-Sandy-hardened streets of New York City. For years she worked with city and state leaders to assess the impacts of climate change and to develop risk reduction strategies. In 2009, she was asked to bring her experience to NASA's Climate Adaptation Science Investigators Working Group, an effort prompted by a presidential order to evaluate "risks and vulnerabilities" at every federal agency.
"It may be the first time NASA's scientists and managers have worked together to manage climate risks to our facilities and natural resources," Rosenzweig said. Together with state and local officials—as well as federal, military, commercial, and conservation partners—CASI has set out to brainstorm what kind of information is needed by facilities managers, as well as what kind of response might be required.
The CASI team translated international reports and projections—such as the Intergovernmental Panel on Climate Change (IPCC) or the U.S. National Climate Assessment—into practical, regional-scale advice for the NASA centers. They conducted environmental impact studies and modeling to project how much sea level could rise near each facility. They examined past and future land use changes around centers, even considering how sea level rise might affect the endangered and threatened species that find havens on NASA property.
"How do we fight Mother Nature for another fifty years?" said Kim Toufectis. His colleagues at each center and in the Office of Strategic Infrastructure—people with skills in civil and chemical engineering, urban planning, real estate, facilities construction and maintenance—must now weigh their options and develop long-range plans.
In some places, they will need to design smarter buildings; in others, they will retrofit and harden old infrastructure. If a facility must stay within sight of the water, then maybe the important laboratories, storage, or assembly rooms should not be on the ground floor. For the launch facilities, which must remain along the shore, beach replenishment, sea wall repair, and dune building may become part of routine maintenance.
But across the space agency, from lab manager to center director to NASA administrator, people will have to continually ask the question: is it time to abandon this place and move inland? It's a question everyone with coastal property in America will eventually have to answer.
By Michael Carlowicz
The opinions expressed herein are the author's and not necessarily those of The Maritime Executive.
This post was sourced from Maritime Executive: View original article here.
Filed Under: Maritime Executive


Darren Rhodes has been the director of YogaOasis studios in Tucson since 1999. Darren is featured in the yoga poster, Penchant for Practice. His book, The Yoga Resource Practice Manual, includes practice instructions for 360 poses. Darren is the founder of Yogahour® and was named one of Yoga Journal's "21 Talented Young Teachers Shaping the Future of Yoga." Darren is also a faculty member of Glo.


text:
Biodynamic Books
Our Connection with the Elemental World By Rudolf Steiner
The heart of this volume comprises Rudolf Steiner's commentary on the elemental forces responsible for our earthly nature as human beings―forces that influence us through our membership of a national or geographical group. When such elemental forces are not recognized and understood, he states, they cause conflict and chaos. However, Steiner indicates an important accompanying task that calls on all of us to develop individuality, emancipating ourselves from the earthly influences underlying national and racial groups.
These great themes are framed by Rudolf Steiner's pioneering research into the two major Northern folk poems―Kalevala and The Dream Song of Olaf Åsteson. The former tells of the elemental spirits who created the conditions for our earthly incarnation, whereas the Dream Song has to do with the drama of excarnation―the journey of the human soul after death. Linking these vast motifs is Steiner's unique description of the mission and tasks of the Russian people and the contrast of their destiny to the North American people (who, he says, are "dominating the Earth for a brief period of increasing splendor").
Steiner explains how elemental beings, responsible for the balance of land and sea, have created conditions whereby various peoples are enabled to develop their gifts and fulfill their destinies. Thus, he speaks of Finland as the ancient conscience of Europe, Russia as the future bearer of the Christ-imbued Spirit Self, and the differing but complementary environments of Germany and Britain. Strikingly, he states, "No souls on Earth love one another more than those living in Central Europe and those living in the British Isles."
Steiner also speaks of the necessary work of the luciferic and ahrimanic beings that collaborate to enable the solid spatial forms of our physical bodies. Likewise, they influence our etheric and astral bodies, facilitating thinking, feeling, and volition to be imbued with life and consciousness.


I love this ingenious combination of traditional paper origami, magnets, puppetry, and programmed electronics. The flock of dancing cranes is the creation of Japanese designer Ugoita T. The result is a whimsical whole that is more than the sum of the parts. I think there are a lot of other interesting things he could do with this concept.
Feeling inspired? Here is where you can get all kinds of Origami paper, kits, and instruction books. While your are at it, maybe you'll want some small strong magnets!


text:
The 1915–16 Colgate Raiders men's basketball team represented Colgate University during the 1915–16 college men's basketball season. The head coach was Walt Hammond, coaching the Raiders in his third season. The team had finished with a final record of 14–4. The team captain was Don Kennedy.

Schedule

|-

References

Colgate Raiders men's basketball seasons
Colgate
Colgate
Colgate

redpajama_set_name: RedPajamaWikipedia


6061 aluminum is a lightweight, general-purpose aluminum alloy that can easily be machined or welded. It has a high resistance to corrosion, and an excellent weight-to-strength ratio. The T6511 temperature also means it has been heat treated for additional strength (yield strength: 35, 000 psi). this 6061 aluminum meets ASTM B221 specifications.


text:
is a Japanese football player.

Club statistics
Updated to end of 2018 season.

References

External links
Profile at Kagoshima United FC

1991 births
Living people
Association football people from Yamanashi Prefecture
Japanese footballers
J1 League players
J2 League players
J3 League players
FC Tokyo players
Kataller Toyama players
Kagoshima United FC players
Suzuka Point Getters players
Association football defenders


text:
Storms down trees, cause power outages in parts of DC region
90s across DC region as heat wave continues; dangerous weekend heat as temps expected to soar
Report: DC's youth among most at-risk in the nation
Lawmaker introduces proposal in Fairfax County to ban panhandling at medians, intersections
Girl, 9, dies after being electrocuted by wire from pool light that was under repair
Lights! Camera! McCarthy!
Good Day DC Mug Giveaway
DC Lottery Tote Bag Giveaway
Zip Trip Acura Giveaway
Zip Trip Lafayette Federal Credit Union Giveaway
Avocados From Peru Contest
Universoul Circus Contest
FOX 5 Plus
Pocono Webcams
Actor Carol Channing performs during the Fourth Annual Actors' Fund of America gala, October 25, 2003 in the Luckman Fine Arts Complex at California State University in Los Angeles California. (Photo by Frederick M. Brown/Getty Images)
Posted Jan 15 2019 07:19AM EST
Updated Jan 15 2019 10:47AM EST
FOX NEWS - (AP) -- Carol Channing, the lanky, ebullient musical comedy star who delighted American audiences over almost 5,000 performances as the scheming Dolly Levi in "Hello, Dolly" on Broadway and beyond, has died. She was 97.
Publicist B. Harlan Boll said Channing died of natural causes at 12:31 a.m. Tuesday in Rancho Mirage, California. Boll says she had twice suffered strokes in the last year.
Besides "Hello, Dolly," Channing starred in other Broadway shows, but none with equal magnetism. She often appeared on television and in nightclubs, for a time partnering with George Burns in Las Vegas and a national tour.
Her outsized personality seemed too much for the screen, and she made only a few movies, notably "The First Traveling Saleslady" with Ginger Rogers and "Thoroughly Modern Millie" with Julie Andrews.
Over the years, Channing continued as Dolly in national tours, the last in 1996, when she was in her 70s. Tom Shales of The Washington Post called her "the ninth wonder of the world."
Messages of love and appreciation lit up Twitter early Tuesday, with the League of Professional Theatre Women saying Channing "was a gift of inspiration to so many." Fans who saw her work also took to social media, calling her a "firecracker" and saying she was "matchmaking for the angels now."
Channing was not the immediate choice to play Dolly, a matchmaker who receives her toughest challenge yet when a rich grump seeks a suitable wife. The show, which features a rousing score by Jerry Herman that's bursting with joy and tunes like "Put On Your Sunday Clothes," `'Before the Parade Passes By" and "It Only Takes a Moment," is a musical version of Thornton Wilder's play "The Matchmaker."
Theater producer David Merrick told her: "I don't want that silly grin with all those teeth that go back to your ears." Even though director Gower Champion had worked on her first Broadway hit, "Lend an Ear," he had doubts about Channing's casting.
She wowed them in an audition and was hired on the spot. At opening night on Jan. 16, 1964, when Channing appeared at the top of the stairs in a red gown with feathers in her hair and walked down the red carpet to the Harmonia Gardens restaurant, the New York audience went crazy. The critics followed suit. "Hello, Dolly" collected 10 Tony Awards, including one for Channing as best actress in a musical.
Channing was born Jan. 31, 1921, in Seattle, where her father, George Channing, was a newspaper editor. When his only child was 3 months old, he moved to San Francisco and worked as a writer for The Christian Science Monitor and as a lecturer. He later became editor-in-chief of Christian Science publications.
At the age of 7, Channing decided she wanted to become an entertainer. She credited her father with encouraging her: "He told me you can dedicate your life at 7 or 97. And the people who do that are happier people."
While majoring in drama and dance at Bennington College in Vermont, she was sent off to get experience in her chosen field. She found a job in a New York revue. The show lasted only two weeks, but a New Yorker magazine critic commented, "You will hear more about a satiric chanteuse named Carol Channing." She said later: "That was it. I said goodbye to trigonometry, zoology and English literature."
For several years she worked as an understudy, bit player and nightclub impressionist, taking jobs as a model, receptionist and sales clerk during lean times. Landing in Los Angeles, she auditioned for Marge Champion, wife and dance partner of Gower Champion who was putting together a revue, "Lend an Ear." Marge Champion recalled: "She certainly was awkward and odd-looking, but her warmth and wholesomeness came through."
Channing was the hit of "Lend an Ear" in a small Hollywood theater, and she captivated audiences and critics when the show moved to New York. As the innocent gold digger in the musical "Gentlemen Prefer Blondes," her stardom was assured. One reviewer reported she "hurls across the footlights in broad strokes of pantomime and bold, certain, exquisitely comical gestures." The show's hit song, "Diamonds Are a Girl's Best Friend," became her signature number.
Over and over again she returned to the surefire "Hello, Dolly," which earned her $5 million on one tour. She considered Dolly Levi "a role as deep as Lady Macbeth," but added that "the essence of her character was her unquenchable thirst for life." That description fit Carol Channing, who attributed her sunny optimism to her lifelong faith in Christian Science.
Others who have played the role include Pearl Bailey, Phyllis Diller, Betty Grable, Ethel Merman, Martha Raye, Ginger Rogers and Barbra Streisand, who played Dolly in a 1969 film version directed by Gene Kelly. Bette Midler won a Tony Award in the role in 2017.
Channing had two early marriages that ended in divorce -- to novelist Theodore Naidish and pro footballer Alexander Carson, father of her only child, Channing. Her son became a successful political cartoonist.
In 1956 she married a television producer, Charles Lowe, who seemed like the perfect mate for a major star. He adopted Channing's son and supervised every aspect of her business affairs and appearances. He reportedly viewed every one of her performances from out front, leading the applause.
After 41 years of marriage, she sued for divorce in 1998, alleging that he misappropriated her funds and humiliated her in public. She remarked that they only had sex twice in four decades.
"The only thing about control freak victims is that they don't know who they are," she told The Washington Post. "It's taken me 77 years to figure that out. I was miserable. I was unhappy. And I didn't realize it wasn't my fault. But I'm going to survive. I'm going to live. I'm free."
Lowe died after a stroke in 1999. Channing moved to Rancho Mirage near Palm Springs, California, in 2000 to write her memoirs. She called the book "Just Lucky, I Guess."
Channing remarried in 2003 to Harry Kullijian, her childhood sweetheart from 70 years before. He died in 2011.
In her book, Channing recounted an early story from her childhood that showed a budding audience-pleasing performer. She wrote that she came home from kindergarten and noted that all the little girls hit the little boys.
Her parents asked: "Do you?"
She responded: "Oh no, I pet them."
Associated Press writer Shawn Marsh in Trenton, New Jersey, contributed to this report.
Follow Mark Kennedy on Twitter at http://twitter.com/KennedyTwits
© 2019 The Associated Press. All rights reserved. This material may not be published, broadcast, rewritten or redistributed.
By fox5dc.com staff
The heat wave which has brought intense heat and humidity to the D.C. region over the last several days will continue Thursday with temperatures expected to soar to dangerous levels over the weekend.
Download the FOX 5 Weather App
FOX 5's Michelle Rotella says temperatures will drop slightly today giving us highs around 93 degrees but the heat index, which is what it feels like based on the temperature and humidity, could climb back up to around 105 degrees by later this afternoon.
A round of heavy storms that moved across the region Wednesday knocked out power and brought down trees in parts of the D.C. area.
FOX 5's Melania Alnwick was in Fairfax County where utility crews had been working overnight to restore power to impacted customers in the Fair Oaks neighborhood. Alnwick said that a transformer in a hard to access wooded area took a lightning strike and needed to be replaced.
Alnwick said some utility customers could expect service to be restore earlier in the day and other could be without power into the evening.
By Anne Cutler, FOX 5 DC
WASHINGTON (FOX 5 DC) — Washington, D.C. has more at-risk youth than almost every state in the nation, according to a new study looking at "idle and disconnected" youth across the U.S.
The report, which was released Wednesday by WalletHub , cites poverty and homelessness among other factors going into that number two ranking. It shows Louisiana is the only state with more at-risk youth than D.C.
The report ranked the District second in the nation in youth drug use, first in youth poverty, first in homeless youth and sixth for youth detainment and incarceration.
FOX 5 DC News App
DC Weather Radar and Alerts


New data from Synergy Research Group shows that just 20 metro areas account for 59% of worldwide retail and wholesale colocation revenues. Ranked by revenue generated in Q3 2017, the top five metros are Washington, New York, Tokyo, London, and Shanghai, with those five metros alone accounting for 26% of the worldwide market. The next 15 largest metro markets account for another third of the worldwide market. Those top 20 metros include ten in North America, four in the EMEA region and six in the APAC region. Across the 20 largest metros, retail colocation accounted for 72% of Q3 revenues and wholesale 28%. In Q3 Equinix was the market leader by revenue in eight of the top 20 metros and Digital Realty would be the leader in five more if a full quarter of the acquired DuPont Fabros operations were included in its numbers. Other colocation operators that featured heavily in the top 20 metros include 21Vianet, @Tokyo, China Telecom, CoreSite, CyrusOne, Global Switch, Interxion, KDDI, NTT, SingTel and QTS. Over the last four quarters colocation revenue growth in the top five metros outstripped growth in the rest of the world by two percentage points, so the worldwide market is slowly being concentrated more in those key metro areas. Top 20 metros with annualized growth rates of 15% or more (measured in local currencies) were Shanghai, Beijing, Hong Kong and Washington/Northern Virginia. All four saw strong growth in both the retail and wholesale segments of the market, though growth in wholesale tended to be higher. Chicago also saw very strong growth in wholesale revenues, though in this metro retail colocation growth was relatively weak.


The green IT track at Interop Las Vegas kicked off with a session from yours truly on "The evolution of green IT: Projects that cut cost, avoid risk, and grow revenues".
IT is the cornerstone to planning and executing organisation-wide green strategies. While C-level business execs in conjunction with the "environmental, health and safety" and "corporate social responsibility" departments might initiate organisation-wide green thinking, IT plays a critical role in planning and execution. Forrester finds that in 43% of organisations globally, "IT has a central role in both planning and executing" their organisation's environmental sustainability strategy. Because effective sustainability management requires information gathering and analysis across a broad range of company assets -- and then reporting to a range of internal and external stakeholders -- Forrester has long held that IT must be heavily involved. And this data indicates that IT practitioners at many companies agree.
The scope of green IT is broadening. While the industry's initial -- and even continued focus -- is on the datacentre, organisations are realising that they have bigger opportunities in distributed IT, and even more so outside of IT altogether. Why? While the datacentre is a significant consumer of energy, Forrester's survey data finds that more energy is actually consumed by distributed IT assets in aggregate (e.g., PCs, monitors, printers, phones) -- 55% across distributed IT vs. 45% in the datacentre. And even more, the IT industry is only responsible for 3% of the world's greenhouse gas emissions -- making the case very compelling to use technology to reduce environmental impacts across broader business operations (e.g., truck fleets, packaging, real estate energy management, supply chain). To describe this widening of the green IT agenda, Forrester uses the shorthand of green IT 1.0 ("green for IT") and green IT 2.0 ("IT for green").
The approach to green IT is expanding. While the traditional hardware-centric approach to green IT of sourcing more energy efficient equipment is still important, it should only be a component of how enterprise I&O professionals approach green IT. And as the economic downturn reduced CAPEX, IT organisations were forced to extend the lifecycle of hardware and pursue alternative approaches to green IT by consolidating and improving the utilisation and efficiency of IT equipment they already own. These additional approaches include software, services, processes and people.
Hardware: Enterprise Rent-A-Car's thin client draws 13.6 watts versus 77.1 watts from a desktop, saving $500K per year.
Software: Leading client management vendors and startups are offering PC power mgt software that can cut energy costs by $25-$75 per PC per year (ENERGY STAR).
Services: Emerson, Schneider Electric, HP, IBM, Dell, and others offer DC energy audits -- critical to spending time and money wisely.
Process: By increasing the temperature to 74°F degrees (from 69°F), KPMG noticed a 12.7% reduction in energy consumption.
People: Microsoft datacentre facility managers' bonuses are tied to year-over-year efficiency improvements.


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Daily variation at Concordia station (Antarctica) and its dependence on IMF conditions
L. Cafarella1, D. Di Mauro1, S. Lepidi1, A. Meloni1, M. Pietrolungo1, L. Santarelli1, and J. J. Schott2 L. Cafarella et al. L. Cafarella1, D. Di Mauro1, S. Lepidi1, A. Meloni1, M. Pietrolungo1, L. Santarelli1, and J. J. Schott2
1Istituto Nazionale di Geofisica e Vulcanologia, Roma, Italy
2Ecole et Observatoire des Science de la Terre, IPG, Strasbourg, France
Abstract. After some short test surveys, during the 2004–2005 summer expedition in Antarctica, a geomagnetic French-Italian observatory was installed on the plateau (geographic coordinates: 75.1° S, 123.4° E; corrected geomagnetic coordinates: 88.9° S, 54.3° E; UT=LT−8) very close to the geomagnetic pole. In this paper we present some peculiarities of the daily variation as observed at this polar cap observatory during the years 2005 and 2006, taking into account the different Loyd seasons and different interplanetary magnetic field conditions. Some interesting results emerge from the analysis, confirming the dependence of the daily variation (and of the associated polar current systems) on the IMF Bz and By components. In particular the analysis showed that different Bz conditions correspond to different contribution to daily variation of ionospheric and field aligned currents, while particular By conditions lead to a time shift of the diurnal variation, indicating an asymmetry with respect to the noon meridian.
How to cite: Cafarella, L., Di Mauro, D., Lepidi, S., Meloni, A., Pietrolungo, M., Santarelli, L., and Schott, J. J.: Daily variation at Concordia station (Antarctica) and its dependence on IMF conditions, Ann. Geophys., 25, 2045–2051, https://doi.org/10.5194/angeo-25-2045-2007, 2007.