text:
Invesco S&P 500 QVM UCITS ETF Dist
Fund Components
The Invesco S&P 500 QVM UCITS ETF Dist aims to provide investors with investment results which, before expenses, correspond to the price and yield performance of S&P 500 Quality, Value & Momentum Multi-factor Net Total Return Index (a multi-factor index) in US dollar terms by holding, as far as practicable, all of the Index's constituents in their respective weighting. The index constituent universe is reviewed twice a year, in June and December.
The S&P 500 Quality, Value & Momentum Multi-factor Net Total Return Index ("the Benchmark") aims to represent the performance of those companies within the S&P 500 Index which have the highest aggregate exposure to three investment factors: quality, value and momentum. To determine the components of the Benchmark, all companies included in the S&P 500 Index are assigned scores based on their performance against these three factors. These scores are then combined on an equal-weighted basis into a final factor composite. All companies are then ranked by their final factor composite with the top 100 companies being selected for inclusion in the Index, subject to a buffer rule which aims to reduce turnover. The weight for each component in the Benchmark will range between 0.05% and the lessor of 5.0% of the Benchmark or 20 times its market capitalisation weight. The weight of each sector is capped at 40% for the purposes of seeking to avoid sector concentration.
Information about the index & index sponsor - You can view further information by visiting the S&P Dow Jones Indices website. Please note that, by using this link, you will be leaving the Invesco website. Any views and opinions expressed subsequently are not those of Invesco.
Invesco S&P 500 QVM UCITS ETF - Factsheet DE
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Invesco S&P 500 QVM UCITS ETF Factsheet
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Invesco Markets III plc DK Country Supplement
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PowerShares dividend declaration 15-12-2017
PowerShares Dividendenausweis 16-03-2018 - CH
Bloomberg ticker PQVM LN
ISIN IE00BDZCKK11
Benchmark BBG ticker SPXQVMUN
Management fee 0.35%
NAV (17 Jan 2020) $34.66
AUM $6,931,517
Base currency USD
Shares of companies are generally considered high risk investments and may result in fluctuations in the value of the Fund due to external factors.
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Investors should be prepared to accept a higher degree of risk than for a fund that is geographically diversified.
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text:
Suk-Jun Kim
"I was in this land called Hasla. A far-off land in which everything seemed familiar and yet oddly alien; a place you have never traveled to and yet which in a strange way is similar to every city you've ever visited, which – no sooner did you arrive – you already left again. At least that's how I remember it. But how can I tell of a land that doesn't exist?"
Hasla consists of electroacoustic compositions that are inspired by a poetry of localization and spatialization of sound. Calmly and transparently, these sounds formulate questions whose answers are delayed, in a kind of tonal dream logic that lends the pieces their tension. Suk-Jun Kim (*1970 in Korea) studied in Canada, the USA and France, and was a guest of the Artists-in-Berlin Program of the DAAD in 2009 / 10.
Commissioning body
Berliner Künstlerprogramm des DAAD
Arts and Humanities(all)
Kim, S-J. (2011). Hasla. Heidelberg, Germany: Kehrer Verlag.
Hasla. / Kim, Suk-Jun.
Heidelberg, Germany : Kehrer Verlag, 2011. 88 p.
Kim, S-J 2011, Hasla. Kehrer Verlag, Heidelberg, Germany.
Kim S-J. Hasla. Heidelberg, Germany: Kehrer Verlag, 2011. 88 p.
Kim, Suk-Jun. / Hasla. Heidelberg, Germany : Kehrer Verlag, 2011. 88 p.
@book{69caddd4c2054fb48e08b586acba94da,
title = "Hasla",
abstract = "{"}I was in this land called Hasla. A far-off land in which everything seemed familiar and yet oddly alien; a place you have never traveled to and yet which in a strange way is similar to every city you've ever visited, which – no sooner did you arrive – you already left again. At least that's how I remember it. But how can I tell of a land that doesn't exist?{"} Hasla consists of electroacoustic compositions that are inspired by a poetry of localization and spatialization of sound. Calmly and transparently, these sounds formulate questions whose answers are delayed, in a kind of tonal dream logic that lends the pieces their tension. Suk-Jun Kim (*1970 in Korea) studied in Canada, the USA and France, and was a guest of the Artists-in-Berlin Program of the DAAD in 2009 / 10.",
author = "Suk-Jun Kim",
language = "Multiple languages",
isbn = "978-3-86828-162-0",
publisher = "Kehrer Verlag",
T1 - Hasla
AU - Kim, Suk-Jun
N2 - "I was in this land called Hasla. A far-off land in which everything seemed familiar and yet oddly alien; a place you have never traveled to and yet which in a strange way is similar to every city you've ever visited, which – no sooner did you arrive – you already left again. At least that's how I remember it. But how can I tell of a land that doesn't exist?" Hasla consists of electroacoustic compositions that are inspired by a poetry of localization and spatialization of sound. Calmly and transparently, these sounds formulate questions whose answers are delayed, in a kind of tonal dream logic that lends the pieces their tension. Suk-Jun Kim (*1970 in Korea) studied in Canada, the USA and France, and was a guest of the Artists-in-Berlin Program of the DAAD in 2009 / 10.
AB - "I was in this land called Hasla. A far-off land in which everything seemed familiar and yet oddly alien; a place you have never traveled to and yet which in a strange way is similar to every city you've ever visited, which – no sooner did you arrive – you already left again. At least that's how I remember it. But how can I tell of a land that doesn't exist?" Hasla consists of electroacoustic compositions that are inspired by a poetry of localization and spatialization of sound. Calmly and transparently, these sounds formulate questions whose answers are delayed, in a kind of tonal dream logic that lends the pieces their tension. Suk-Jun Kim (*1970 in Korea) studied in Canada, the USA and France, and was a guest of the Artists-in-Berlin Program of the DAAD in 2009 / 10.
M3 - Book
SN - 978-3-86828-162-0
BT - Hasla
PB - Kehrer Verlag
CY - Heidelberg, Germany
http://www.artbooksheidelberg.com/html/detail/en/suk-jun-kim-978-3-86828-162-0.html
Welcome to Hasla
Research output: Non-textual form › Composition
On the Way to Fwarrheu
Painting Nahhamu
A Travel Log: From Fwarrheu to Hejning
Research output: Non-textual form › Exhibition
One-Year Artists-in-Berlin Programme of the DAAD
Activity: Other › Types for public engagement, outreach and knowledge exchange - Other
Activity: Other › Types for public engagement, outreach and knowledge exchange - Festival/exhibition
In Tune, Out of Tune
Activity: Talk, presentation, public lecture, public engagement, outreach and knowledge exchange › Exhibition/Festival

redpajama_set_name: RedPajamaCommonCrawl


text:
Лъв V Арменец () е византийски император от 813 до смъртта си през 820.

Възкачване на престола
Той е началник на федератите по времето на Никифор I (802 – 811), но изпада в немилост, бичуван и принуден да се замонаши. Реабилитиран е при Михаил I Рангаве (811 – 813) и назначен за стратег на най-голямата по численост тема Анатоликон.

Лъв Арменец показва добри ръководни умения при сраженията с арабите през 812 г. и на него са възлагани надежди при войните срещу България по времето на хан Крум. Съвсем целенасочено Лъв изоставя император Михаил I в битката при Версиникия (22 юни 813 г.), а впоследствие използва поражението му като повод за военен преврат. Подкрепен от арменските войски Лъв принуждава Михаил I да абдикира и да се замонаши (11 юли 813 г.). Синовете на бившия император са скопени, за да нямат претенции за власт (според закона евнух не може да стане владетел).

Управление

Война с България

При хан Крум
След като идва на трона, Лъв трябва да се справя с обсаждащите Константинопол български войски. Ситуацията е много напрегната, тъй като българите търсят отмъщение за разорителното нахлуване на Никифор Геник. Тогава Лъв прави опит да убие чрез измама хан Крум при преговорите, но атентатът се оказва несполучлив и предизвиква яростната реакция на Крум, който опустошава околностите на Константинопол. Превзети и обезлюдени са Адрианопол (дн. Одрин) и Аркадиопол (дн. Люлебургаз). Ромеите нямат достатъчно военни сили за да спрат вилнеещите българи и само непревземаемите стени спасяват имперската столица.

При хан Омуртаг
През 815 г., след смъртта на Крум, Лъв Арменец сключва 30-годишен мирен договор с новия хан Омуртаг, с който се урежда границата между двете държави в Тракия, маркиращи териториалното статукво от управлението на хан Тервел. На преговорите императорът полага ритуална клетва съгласно българските обичаи, а пратениците на хана се заклеват според християнските правила. Мирът между двете страни е подновяван при следващите владетели и в общи линии продължава близо половин век.

Иконоборска политика

Лъв V е привърженик на иконоборството, макар че демонстрира обратното преди да дойде на власт. През 815 г. са осъдени решенията на Вселенския събор от Никея и е изказана защита на иконоборския събор от 754 година. Строгите репресивни мерки, които предприема спрямо павликяните и иконопочитателите, довеждат до непопулярността на императора сред духовниците и част от народа. Той конфискува имуществото на някои видни иконопочитатели, като Теодор Студит. Пикът на иконоборската му политика е избирането на нов константинополски патриарх – Лъв, верен нему човек. Връщането към иконоборството, вече в сравнително по-умерена форма, цели не толкова премахване на самите икони, колкото набавянето на необходимите за държавата средства, за сметка на богатото духовенство.

След като осуетява заговор, ръководен от неговия съратник Михаил Псел (бъдещият император Михаил II), Лъв хвърля Псел в затвора. Скоро след това е издебнат и посечен от приближени на Псел, предрешени като монаси, по време на Коледната литургия (25 декември 820 г.) в дворцовата катедрала "Св. Стефан".

След убийството на Лъв V Арменец четиримата му синове са кастрирани и замонашени, за да бъдат лишени от възможността да претендират за престола, тъй като според закона евнух не би могъл да бъде признат за законен император. Базирайки се на сведения от Константин Порфирогенет и Теофан Продължител арменският историк Никохайос Адонц изказва теорията, че Василий I Македонец е потомък на Лъв Арменец по женска линия, а не син на обикновени селяни.

Въпреки неговия принос за умиротворяването на империята, Лъв Арменец е оценяван негативно от византийските църковни хронисти, които критикуват иконоборството и безскрупулните му действия.

Външни препратки

 Продължителят на Теофан "Жизнеописание на византийските царе" (Книга I. Лъв V) ГИБИ I изд. БАН
 Leslie Brubaker, John F. Haldon: Byzantium in the Iconoclast era. c. 680 – 850. A History. Cambridge University Press, Cambridge u. a. 2011, ISBN 978-0-521-43093-7
 Warren Treadgold: The Byzantine Revival, 780 – 842. Stanford 1988

Византийски императори
Византийски императори от арменски произход
Православни монарси
Имперски римски консули

redpajama_set_name: RedPajamaWikipedia


text:
Q: DialogFragment does not close in AsyncTask I have a way to check the Internet connection every 15 seconds. If there is no internet connection, the method calls the dialogfragment. So far it works perfectly. I cannot close dialogFragment when internet connection is established. Logcat does not give an error.  "dialogfragment dissmis" not working and dialogfragment remains on the screen.
First I disconnect from the internet and the dialogFragment is called. Later  Internet connection is running and "Device is connected to internet." I see the text. But the dialogfragment does not disappear.
CheckInternetAsyncTask.class
public class CheckInternetAsyncTask extends AsyncTask<Void, Integer, Boolean> {

    Activity activity;
    private Context context;

    public CheckInternetAsyncTask(Activity activity) {
        this.context = activity.getApplicationContext();
        this.activity = activity;
    }

    @Override
    protected Boolean doInBackground(Void... params) {

        ConnectivityManager cm =
                (ConnectivityManager)context.getSystemService(Context.CONNECTIVITY_SERVICE);

        assert cm != null;
        NetworkInfo activeNetwork = cm.getActiveNetworkInfo();
        boolean isConnected = activeNetwork != null &&
                activeNetwork.isConnected();

        if (isConnected) {
            try {
                InetAddress ipAddr = InetAddress.getByName("google.com");
                //You can replace it with your name
                return !ipAddr.equals("");

            } catch (Exception e) {
                Log.e("TAG", "Error checking internet connection"+ e.getMessage());
                return false;
            }
        } else {
            //Log.d("TAG", "No network available!");
            return false;
        }
    }

    @Override
    protected void onPostExecute(Boolean result) {
        super.onPostExecute(result);
        //Log.d("TAG", "result" + result);

        if(result){
            // do ur code
            Toast.makeText(context,"Device is connected to internet.", Toast.LENGTH_LONG).show();
            EthernetControlFragment ethernetControlFragment = EthernetControlFragment.newInstance();

            if (ethernetControlFragment != null
                    && ethernetControlFragment.getDialog() != null
                    && ethernetControlFragment.getDialog().isShowing()
                    && !ethernetControlFragment.isRemoving()) {
                //dialog is showing so do something
                ethernetControlFragment.dismissAllowingStateLoss();
            } else {
                //dialog is not showing
            }

        }
        else {
            Toast.makeText(context,"Device is not connected to internet!",Toast.LENGTH_LONG).show();
            EthernetControlFragment ethernetControlFragment = EthernetControlFragment.newInstance();

            if (ethernetControlFragment != null
                    && ethernetControlFragment.getDialog() != null
                    && ethernetControlFragment.getDialog().isShowing()
                    && !ethernetControlFragment.isRemoving()) {
                //dialog is showing so do something
            } else {
                //dialog is not showing
                ethernetControlFragment.show(((FragmentActivity) activity).getSupportFragmentManager(), "ethernet");
                ethernetControlFragment.setCancelable(false);
            }
        }

    }
}

EthernetControlFragment
public class EthernetControlFragment extends DialogFragment {

Context context;

public static EthernetControlFragment newInstance(){
    return new EthernetControlFragment();
}

@Override
public void onCreate(@Nullable Bundle savedInstanceState) {
    super.onCreate(savedInstanceState);
    setStyle(DialogFragment.STYLE_NORMAL, R.style.dogum_haritasi_dialog);

}

@Nullable
@Override
public View onCreateView(@NonNull LayoutInflater inflater, @Nullable ViewGroup container, @Nullable Bundle savedInstanceState) {
    View view = inflater.inflate(R.layout.ethernet_controls,container,false);

    return view;
}}

A: Okay i'm gonna explain here in detail.
15 seconds ago you created a dialog using below line let's call it object1
EthernetControlFragment.newInstance()
Then after 15 seconds again you're creating a new dialog object2 using above line and when you're dismissing it you're dismissing this new dialog object2. Unfortunately you're not keeping reference of old Dialog dialog1 which is the real issue.
Solution would be to create only one object so create a global reference of EthernetControlFragment class and initialise this only if it's null. This way you'll have only one dialog.

A: I solved my problem. Call fragment like this:
    Fragment prev = ((FragmentActivity) activity).getSupportFragmentManager().findFragmentByTag("ethernet");
    if (prev == null) {
        ethernetControlFragment.show(((FragmentActivity) activity).getSupportFragmentManager(), "ethernet");
        ethernetControlFragment.setCancelable(false);
    }

And dissmis like this:
Fragment prev = ((FragmentActivity) activity).getSupportFragmentManager().findFragmentByTag("ethernet");
            if (prev != null) {
                EthernetControlFragment df = (EthernetControlFragment) prev;
                df.dismiss();
            }

I think these methods are the most reliable way to call and dissmis fragment.

redpajama_set_name: RedPajamaStackExchange


text:
Home > SWAROVSKI CRYSTALS
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Swarovski crystals are available in a myriad of amazing colors, effects, shapes, and sizes. The most popular are the flat back rhinestones.
Swarovski Products are no longer available for the RG Pros Customers, We are in the process of removing them from this site. Please move on to the Preciosa and RG Product lines.
Swarovski Rhinestones & Crystal Shapes Flat Backs
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text:
Hurricane Dorian: Prime Minister Addresses Nation
Prime Minister Dr Hubert Minnis, PLP Deputy Leader Chester Cooper, North Abaco MP Darren Henfield and Bahamas Christian Council President Rev Delton Fernander were among a delegation on a humanitarian trip to Green Turtle Cay, Coopers Town and North Abaco today to assess hurricane damage and deliver relief supplies.
As of Thursday, September 12, 2019
Discuss 10 comments, Blog about
THURSDAY'S UPDATES CAN BE READ HERE
9pm UPDATE: From Prime Minister Dr Hubert Minnis' national address tonight –
• Jack Thompson and Algernon Cargill have been appointed hurricane relief and redevelopment coordinators in Abaco while Senate President Kay Forbes Smith has been appointed coordinator for Grand Bahama.
• A national day of mourning is being planned and flags will be flown at half-mast on public buildings.
• On the government's action after the storm: "Right after the all-clear was given by the Met Department, we began mobilising our search, rescue and recovery efforts. We deployed security, food, water and other resources as quickly as was possible once the all-clear was given so that first respondents were not put at risk.
"Our search, rescue, and recovery efforts are one response with many parts. As soon as was possible, after the impact of the hurricane, the government deployed Bahamian rescue and security personnel, from the Royal Bahamas Defence Force and the Royal Bahamas Police Force.
"At the invitation of the government of the Bahamas, we asked the US Coast Guard to immediately go into action, using their helicopters and other resources."
• The government is working to set up and secure temporary housing and shelters on the affected islands for people who lost homes.
• The Prime Minister praised the United States, saying President Donald Trump has authorised the full support of the US government for this country and noted that disaster management experts from the US are in the country to provide their expertise. "One of our closest allies and neighbour is the United States of America," he said. "The president of the United States, Donald Trump, has proven to be a true friend to the Bahamas during this dark hour."
He added: "Because of their specialty equipment and resources, the US Coast Guard has been leading air rescuers and transport within the disaster zone. USAID is providing significant relief supplies. Members of the FBI are here too along with other US rescue, aid and security officials."
• The Prime Minister also thanked the United Kingdom, which has sent its Royal Navy; CARICOM, which has sent security forces and aid officials; the Canadian government and the Royal Dutch Navy.
• Dr Minnis called on residents to help. "Instead of criticising those who are trying their best, day after day, in government, charities, churches and volunteers' efforts, let us all join hands and hearts to focus on the needs of those who are suffering," he said. "Those whose lives are devastated need hope, love and generosity, not needless negativity.
"How can you help? Volunteer at a reputable charity. Make a donation. Take in those in need."
• The Prime Minister said incidents of looting and lawlessness post-hurricane will not be tolerated, adding law enforcement officials have secured Abaco.
• A private accounting firm will have oversight of storm relief donations to the government and will report on how the money is being spent.
6.20pm UPDATE: THE RFA Mounts Bay has completed its ten-day Hurricane Dorian aid mission - with more than 6,000 people helped by British sailors, soldiers, marines and fliers during the mission.
The HNLMS Johan de Witt has brought its first soldiers ashore using Cougar helicopters.
The Royal Navy vessel distributed all its stores - 3,000 ration packs, nearly 100 tonnes of water, more than 900 emergency shelter kits and 1,000 hygiene kits and is now moving to resupply in case of further disasters in the region.
Replacing the vessel in aid efforts is a Dutch vessel, the HNLMS Johan de Witt, which has already brought its first soldiers ashore using Cougar helicopters.
The Dutch ship reported it had "made contact with the advanced liaisons and local government" and were together making a plan to begin assistance.
12.50pm UPDATE: From today's NEMA press conference –
• The Department of Social Services is the agency managing the government register of missing people. You can register a missing person by calling the missing person hotline (numbers on NEMA's Facebook page) – you can also visit the Department of Rehabilitative Services and Welfare Services on University Boulevard. At this point there are approximately 2,500 individuals registered on the Bahamian government register.
This list has not yet been checked against government records of who is staying in shelters or who has been evacuated. The database processing is underway. Some individuals who evacuated from Abaco and Grand Bahama have not yet registered with social services and are encouraged to do so at the Department of Rehabilitative Services and Welfare Services.
Some of the government's list will have to be converted to a digital format to allow for effective cross checking. As NEMA is able to crosscheck they will be able to inform family members and reunite survivors with loved ones.
At the shelters, NEMA is facilitating those who are able to reach out directly to family and friends to let them know where they are. Over 5,500 individuals have been evacuated to New Providence – an update will come on the numbers who have travelled to the US.
• There is a significant reduction in those presenting themselves for evacuation flights. Commercial carriers will be allowed to resume flights starting today on a limited basis. Airlines should reach out to the director general of the Bahamas Civil Aviation Authority in order to gain approval. Organisations for humanitarian aid, repairs and search and recovery will continue to have priority.
Evacuations will continue in Freeport today.
• Parents and guardians of displaced students aged 4-19 can enroll them in a government school in New Providence or any of the unaffected islands.
The Ministry of Education will be registering students at the national stadium beginning Thursday (tomorrow) until Friday, October 11 from 9am-5pm.
Students will also be able to access services from the Ministry of Health, the Ministry of Social Services, the Ministry of Youth, Sports and Culture and the Royal Bahamas Police Force during this process. These include: Medical screening required for school enrollment; uniform and lunch assistance; referrals for counseling services and referrals for extra curricular activities.
Where available, parents and guardians are requested to provide documentation for their children including their immunisation cards – it is understood that some documents may have been lost.
Buses will be provided from shelters to the stadium and shelter managers will be informed of the registration schedule – which will be staggered to avoid long lines. All students from Abaco and Grand Bahama are expected to participate, whether or not they are in shelters. Those not in shelters should call the Ministry of Education on 502-3779 or 502-8319 to receive details on the scheduling.
• Marsh Harbour power station was completely destroyed. Power generation is still available in Wilson City and Sandypoint. The plan is to bring power back to the south of Abaco first – where the least damage is. This will be the staging ground for the recovery. 90 percent of the infrastructure is compromised from Marsh Harbour to Treasure Cay. Equipment has been dispatched to assist crews and there is sufficient manpower – but more equipment is needed.
• The US Embassy can facilitate appointments with hurricane survivors to apply for visas to the US. Hurricane survivors are welcome to visit other countries or temporarily live there while they get on their feet – this must be done with existing visa protocols. The Bahamian government is only providing service to survivors within the Bahamas.
Samaritan's Purse Field Hospital
Facility in Grand Bahama is now up and running.
10am UPDATE: From today's print edition –
• ON most days, Success Jean would wake up at 5am, check on his infant children and set off to do construction work at the Baker's Bay Golf & Ocean Club on Great Guana Cay. These days, the 37-year-old's life is confined to wandering a few miles around the Fox Hill Community Centre where he and his family have stayed since Hurricane Dorian made them storm evacuees - full story HERE
• ATTORNEY General Carl Bethel has confirmed the completion of draft legislation to allow for mandatory evacuations once parts of the country are under threat of natural disasters. According to Mr Bethel, once passed, the provision will allow the prime minister through the National Emergency Management Agency to declare a local disaster area and make the necessary orders for mandatory evacuation. The government is proposing to amend the Disaster Preparedness and Response Act – full story HERE
• CABINET ministers yesterday cautioned the public over the spread of erroneous information as officials continue to "meticulously" comb affected areas for deceased victims of Hurricane Dorian. National Security Minister Marvin Dames and Health Minister Dr Duane Sands sought yesterday to rebuff the wave of speculation regarding victims of the storm and to defend the government's process of officially declaring the death toll, which has been criticised as slow moving. Mr Dames maintained that due to the large areas that need to be searched, it could be weeks before the last body is recovered – full story HERE
• FROM the Associated Press: Hornets owner and six-time NBA champion Michael Jordan is pledging $1 million to organisations assisting with Hurricane Dorian relief efforts in the Bahamas.
Jordan said in a statement Tuesday on Twitter through his spokeswoman Estee Portnoy that he's "devastated" at the destruction in the Bahamas, adding "my heart goes out to everyone who is suffering and to those who have lost loved ones."
Jordan, who owns property and frequently visits the Bahamas, says as the recovery and relief efforts continue he will be tracking the situation closely and working to identify nonprofit agencies where the funds will have the most impact.
Jordan added that "the Bahamian people are strong and resilient and I hope that my donation will be of help as they work to recover from this catastrophic storm."
HURRICANE DORIAN: Death toll now stands at 50
HURRICANE DORIAN: Details for displaced students and school employees
HURRICANE DORIAN: Death toll rises to 30
HURRICANE DORIAN: Tropical storm warning for northwest Bahamas, Minnis hits back at former PMs
HURRICANE DORIAN UPDATES: Death toll now stands at 43
buddah17 1 year, 4 months ago
Personally I don't feel that the public is frustrated at the govenment and other agencies wanting to take their time in the recovery phase. But the problem is that the news is only "filtering" out regarding the victims... EG: The count was 5 for DAYS, then 20 for DAYS, then 43, and (now) 50 for DAYS... What is also important is that bodies are properly identified (picutres, DNA) so that nobody can do anything criminal with the information of that person..
TalRussell 1 year, 4 months ago
Every day since 1960's when comrades Sir Stafford and Wallace Groves signed the Hawksbill Creek Agreement, not much nothing positive has changed for thousands comrade Grand Bahamalanders who keeps plopping down their tired bodies on their mattresses at midnight, and after getting 7 hours of sleep only to wakes up at 5 am to face the harsh reality that there are two Grand Bahamaland's. There's FREE port, and then there is the rest of even more neglected Grand Bahamaland, yes, no .... now, the harsh cruelty left behind by Hurricane Dorian has left them mattress-less ....
Gotoutintime 1 year, 4 months ago
Tal---The HBC Act died in 1967!!
Ma Comrade GotOut, was on a Friday weekday of 1969, not 1967, when colony's comrade Lynden Oscar found a necessary need remind FREE port's foreign quasi government's that they better mend their apartheid plan to orchestrate Bahamalanders right out FREE port's master plan, yes, no.... no apology that their imported vicious German Shepard dogs upset colony's newly elected premier .... that members populaces of similar skin colour the colony's second premier, wasn't exactly warmly welcomed dine at Freeport's eatery establishments ....
Godson 1 year, 4 months ago
In all fairness to the present Government Administration, where is Fred Smith QC now in light of the disaster in 'The Mud' & 'Pigeon Peas' Shanty town communities?
Every voice that cries out 'to follow me' is not necessarily a voice to listen to.
Zakary 1 year, 4 months ago
There is also an online directory of missing persons that was very helpful for families during the aftermath of the hurricane at https://dorianpeoplesearch.com. Thank you whoever made that list. Words can't describe the absolutely horrific response of the Government.
killemwitdakno 1 year, 4 months ago
Is that commercial flights for Freeport or Abaco?
SP 1 year, 4 months ago
For the love of JESUS, please do not mention that clowns name and let sleeping idiots lie. Fred is the only person I wished Dorian would cause to disappear.
Bahamian tax payers are now burdened with the responsibility of the well being of 10's of 1000's of illegal Haitians and not one peep about any financial assistance from the Haitian government for their own people!
To add insult to injury, Haitians are the cause for strained U.S. relations resulting in Bahamians loosing the privilege of ease of travel to the U.S. `in our greatest tim e of need.
The Dominicans' did the right thing in deporting Illegal Haitians. Unfortunately, the PLP and FNM do not have what it takes to protect the Bahamas for Bahamians!!
mckenziecpa 1 year, 4 months ago
The Hiatian Embasy did offer support for their people in an earlier editorial
joeblow 1 year, 4 months ago
..... and offer of support is NOT support. Please tell what have they actually DONE!


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text:
Introduction and Allegro appassionato, Op. 92
Orchestration: 2 flutes, 2 oboes, 2 clarinets, 2 bassoons, 2 horns, 2 trumpets, timpani, strings, and solo piano
First Los Angeles Philharmonic performances
It is a shame that one of the legacies of the 19th century, despite its abundance of innovation, was a formalization of what we now think of as a standard concert formula. Audiences are trained to expect a short opening piece, usually an overture, followed by a substantial concerto featuring an instrumental soloist, then after intermission a symphony. The victims are the odd centaur-like pieces which don't fit easily into one of these categories. Pieces such as Schumann's entertaining Introduction and Allegro appassionato, Op. 92 for piano and orchestra get few chances to shine.
After the enormous success of the Piano Concerto in A minor, Op. 54 (a success for both the composer and his wife, the celebrated pianist Clara Schumann, who played the Concerto widely), four years would elapse before Schumann began composing again for the combination of piano and orchestra. The Introduction and Allegro was completed in September of 1849 and premiered by Clara. After mixed reviews it fell quickly into undeserved obscurity, perhaps already a victim of the clash between audience expectations and its novel form.
In barely 15 minutes, Schumann celebrates two of the great themes of the Romantic movement. The period's rapidly developing reverence for nature in the face of the mechanical regimentation of industrialization is heard in the vernal and fluid piano arpeggios and hushed orchestral melodies of the introduction. The joyful and somewhat martial swagger of the concluding allegro is an evocation of the individual as hero - Schumann's alter ego heading off to do battle with the Philistines.
- Annotator Grant Hiroshima is the executive director of a private foundation and the former director of Information Technology for the Los Angeles Philharmonic Association.


text:
Q: PayPal iOS sdk - Which calls should I make from Ruby sdk on my server after Single Payment from mobile? From mobile, I set intent to Sale and then sent the response to server.
From server, I used Payment.find() to get payer-id and then tried to execute the payment using Payment.execute() but I get this error: PAYMENT_STATE_INVALID.
Can anyone tell me what I am doing wrong?

A: I guess there was a confusion. When you set the intent to Sale and capture the payment from PayPal iOS sdk, the sdk does the execution for you. You don't have to do it again on your server.
The only thing you need to do on your server is to verify the payment.


text:
Q: php include works, jquery .load does not Why does this work:
<!DOCTYPE html PUBLIC "-//W3C//DTD XHTML 1.0 Transitional//EN" "http://www.w3.org/TR/xhtml1/DTD/xhtml1-transitional.dtd">

<meta http-equiv="Content-Type" content="text/html; charset=UTF-8" />
<title>Untitled Document</title>

<? include('sites/test.php') ?>

But this does not:
<!DOCTYPE html PUBLIC "-//W3C//DTD XHTML 1.0 Transitional//EN" "http://www.w3.org/TR/xhtml1/DTD/xhtml1-transitional.dtd">

<meta http-equiv="Content-Type" content="text/html; charset=UTF-8" />
<title>Untitled Document</title>

Here is test.php if required:
<link href="http://code.google.com/apis/maps/documentation/javascript/examples/default.css" rel="stylesheet" type="text/css" />

I really need to use jquery for a click event and can't understand why .load won't work.
MTIA!
EDIT - Apologies for the vagueness of "not working"! The initialize function does not seem to uhmmm... initialize. So the window.onload=initialize appears to work using include, but does not seem to work using .load.
I hope this is clearer.

A: window.onload=initialize;

that will execute on the browser triggering that event - as you load in via jquery that event has long passed. Simply change that line to:
initialize();

A: If you give your code another look, the .load is done after the documents loads.
Whereas the include is instantaneous.
This has many side-effects. I urge you to view the browser generated source for more details.
For one thing, you can't use <link/> tags in the body.
Another thing, if Google Maps API makes use of document.ready functionality, it won't work any more.

A: I'd say because the PHP script will look at its working path to include the path, whilst the JavaScript will look at the URL path.


text:
\section{Introduction}

There has been rising interest in studying the quasi-local energy (QLE)
inside the event horizon of the Schwarzschild geometry
\cite{Lundgren:2006fu,Blau:2007wj}. However, the absence of physical, static
observers on the interior, as exist on the exterior, has prevented a simple
passage of QLE across the horizon. The alternative is then to identify
families of non-static, non-geodesic and geodesic observers that can
actually penetrate the horizon smoothly and measure the QLE. This is the
main focus of the present work. It is hoped that this note can bring to the
ongoing discussion a somewhat different perspective.

It is well-known that the quasi-local energy is observer dependent
\cite{Brown:1992br}. Take the Brown-York QLE for example, a family of
prescribed observers -- interchangeably referred to as an observer field --
on a closed, orientable, space-like 2-surface, $S$, as embedded in a
space-like hypersurface $\Sigma$ in the space-time manifold $M$, set
up their frame fields and evaluate the trace of the mean curvature of
$S$ as embedded in $\Sigma$ at their respective locations. After
averaging over $S$ and calibrating against the Minkowski space
reference, the ultimate quantity is the measured QLE
associated with $S$. Among a sea of available observers in a
space-time, the most physically meaningful ones are the observer
fields that are static and those that are geodesic. In the
Schwarzschild space-time, no static observer fields can enter the
event horizon; on the other hand, there do exist geodesic observer
fields that can cross the event horizon. Hence, to use one observer
field as a probe to measure the QLE in the
Schwarzschild space-time, the best candidates would be a non-static,
observer field that penetrates the horizon or a geodesic observer
field.

The Brown-York QLE measured by the above two kinds of
observer fields in the Schwarzschild geometry are examined in this article.
Generalizations to other spherically symmetric space-times should be
straightforward. A simple observation regarding the dynamics of the
relative quasi-local momentum density in a geodesic observer field is also
presented.

A note about the Liu-Yau QLE \cite{Liu:2003} in the
Schwarzschild space-time is recorded here as a comparison. Since the
construction of the physical part of the Liu-Yau QLE employs a
co-dimension 2 embedding of $S$, it is independent, in the exterior of
the horizon, of the choice of observer field. However, the Liu-Yau
QLE becomes invalid in the interior since the mean curvature vector of
$S$ in $M$ becomes time-like, violating one of its defining
hypotheses.

The structure of this article is as follows. An expeditious review of the
fundamentals of the Schwarzschild and Kruskal space-times is given in
Sec.~\ref{review}. Static and non-static, non-geodesic observer fields are
used in the study in Sec.~\ref{nongeodesic}, whereas the case of a geodesic
observer field is presented in Sec.~\ref{geodesic}. Physical interpretations
of the results are summarized in Sec.~\ref{summary}.

\section{A Review of Definitions}
\label{review}

Collected here are some necessary definitions and facts that are frequently
referred to throughout the article. Hence, notations and terminology are
unified in a consistent fashion, at the outset. It should be duly
acknowledged that equivalent co-ordinate systems, such as those due to
Novikov, Painleve, and Eddington-Finklestein, may as well be adopted
for the problem at hand. The ones employed in the present work are an
impartial choice at the service of highlighting the geometric
nature. Details can be found in Ref.~\cite{SachsWu1977}, for example.

The Schwarzschild space-time $({\cal M}, g, D)$ consists of two connected
components ${\cal M}=N \cup B$, namely its exterior $N=P_{\rm I}\times_{\rm
  r} S^2$, where $P_{\rm   I}=p^{-1}({\mathds R}^1\times (2{\rm M},
+\infty))$, and its interior $B=P_{\rm II}\times_{\rm r} S^2$, where
$P_{\rm II}=p^{-1}({\mathds R}^1\times (0, 2{\rm M}))$, each, in the
form of warped product, equipped, in the Schwarzschild spherical
co-ordinate system $x=p \times s$, where $p=(t, r)$ on $P=P_{\rm I}
\cup P_{\rm II}$ and $s=(\vartheta, \varphi)$ on $S^2$, with the
metric $g=g_{\rm P} + r^2 g_{\rm S}$, where $g_{\rm P}=- h(r)dt\otimes
dt+ {dr \otimes dr}/{h(r)}$, $h(r)=1 - {2{\rm M}}/{r}$ ($M>0$), and
$g_{\rm S}$ the standard metric on $S^2$. $D$ is the Levi-Civita
connection of $g$.

It is also quoted here, for notational purposes, the very basics of
the Kruskal space-time that are referred to in the following
section. The Kruskal plane $Q$ is obtained by joining the two
connected components $P_{\rm I}$ and $P_{\rm II}$ via a diffeomorphism
$f: {\mathds R}^+ \longrightarrow (-{2 {\rm M}}/{e}, +\infty)$ by
$f(r)=(r-2{\rm M})e^{\frac{r}{2{\rm M}}-1}$, ${\rm M}>0$. In terms of
the Kruskal null co-ordinate functions $k=(u,v) \in {\mathfrak
  F}({\mathds R}^2, {\mathds R})$ on the $u-v$ plane,
$Q=k^{-1}\Big(\{(u,v) \in {\mathds R}^2: uv> -{2 {\rm
    M}}/{e}\}\Big)$. The Schwarzschild co-ordinate
functions $p=(t,r)$ on $Q$ become $t(u,v)=2{\rm M} {\rm log} |{v}/{u}
|$ on $Q-Q_{\rm H}$, where $Q_{\rm H}=k^{-1}(\{(u,v) \in k(Q):
uv=0\})$, and $r(u,v)=f^{-1}(uv)$ on $Q$. Thus, the metric on $Q$
reads $g_{\rm Q}=F(r) (du\otimes dv + dv \otimes du)$, where
$F(r)=\frac{8{\rm M}^2}{r}e^{1-\frac{r}{2 {\rm M}}}$, $\forall r \in
{\mathds R}^+$. The Kruskal space-time, which is inextendible and
incomplete, is the warped product $K=Q\times_{\rm r} S^2$, equipped with the
metric $g_{\rm K}=g_{\rm Q} + r^2 g_{\rm S}$. The four connected components,
$\{Q_{j}\}_{j={\rm I}}^{j={\rm IV}}$, of  $Q-Q_{\rm H}$ consisting of four
open quadrants in the Kruskal plane, when lifted to $K$, yield $K_{\rm III}
\approx K_{\rm I} \approx N$ and $K_{\rm IV} \approx K_{\rm II} \approx B$,
by virtue of the isometries that preserve the Schwarzschild functions $p$.
It is therefore sufficient to consider half of the Kruskal space-time.

The notions of a family of observers and an observer field (aka a reference
frame) are used interchangeably throughout, the definition of which is
adopted from Ref.~\cite{SachsWu1977}.  Namely, an {\it observer field} $Q$
on a space-time $ {\cal M}$ is a vector field each of whose integral curves is an
observer,  where an {\it observer} is a future-directed  time-like curve
$\gamma: \mathscr E \longrightarrow  {\cal M}$ with unit speed.

\section{Measurement by non-geodesic observers}
\label{nongeodesic}

\subsection{Static observer field}

The Schwarzschild exterior $N$, oriented by a nowhere-vanishing volume form
$\Omega$ and time-oriented by defining the time-like  Killing vector field
$\frac{\partial}{\partial t}$ to be future-directed, is static with respect
to the Schwarzschild observer field $U=\frac{1}{\sqrt{h(r)}}
\frac{\partial}{\partial t}$, where $h(r) \in (0, 1)$ on $N$. Since $D_{U}
U=\frac{{\rm M}}{r^2}\frac{\partial}{\partial r}$, $U$ is not geodesic. The
Schwarzschild  interior $B$, however, is not static with respect to any
observer field. Hence, Schwarzschild observers, i.e., integral curves of
$U$, exist only in $N$, as $U$ becomes space-like in $B$. What inhabits $B$,
nonetheless, is a geodesic observer field
$V=-\sqrt{-h(r)}\frac{\partial}{\partial r}$, which is proper-time
synchronizable since the dual frame field is $\theta^{\rm V}=-dg$, where
$g(r)=\int\limits_{r^\prime =r_0}^{r}\frac{dr^\prime}{\sqrt{-h(r^\prime)}}$,
for some $r_0 \in {\mathds R}^+$.

The Brown-York QLE measured by the Schwarzschild
observer field in $N$ is
\begin{equation}
{\rm QLE}(r) = r [1 - \sqrt{h(r)}].
\label{eqn:qleN}
\end{equation}
It is related to the ADM energy ${\rm M}$ for a
spherically symmetric matter distribution via \cite{Brown:1992br}
\begin{equation}
{\rm M} = {\rm QLE}(r_*) - \frac{{\rm QLE}^2(r_*)}{2 r_*},
\label{eqn:ADM}
\end{equation}
where $r_*$ is the outer boundary of the distribution and
${\rm M}=m(r_*)$. The negative energy term on the right-hand side is
interpreted in \cite{Brown:1992br} as the negative energy outside of
the matter distribution that equals the Newtonian gravitational
binding energy associated with building a spherically symmetric shell
with matter-energy ${\rm QLE}$ and radius $r_*$. In what follows, a
hypothetical quasi-equilibrium procedure of constructing a spherically
symmetric shell of gravitational mass ${\rm M}$ is described. The negative
of the work done by the static Schwarzschild observer field $U$
to build up such a shell is explicitly computed.

Initially, no mass distribution is present. The Schwarzschild observer
field $U$ starts moving from infinity, in a precisely spherically
symmetric manner, a dust-shell of gravitational mass $dm$ and of zero
thickness to a fixed radius $r_*$ which is outside of the horizon
radius. It is assumed that each step is within quasi-equilibrium in
the sense that staticity of the space-time is not sabotaged. It
appears also legitimate to require that $dm$ be small enough so that
the influence of the dust shell on $N$ is negligible. Moreover, the
accumulation of mass  on the shell at radius $r_*$ does not incur an
expansion in its  radius. Hence, no mechanism is provided to sustain
the shell at rest; eventually, the shell of total gravitational mass
${\rm M}$ serves as an equivalent description of a spherically symmetric relativistic
star of total gravitational mass ${\rm M}$ and radius $r_*$ seen from
outside. More precisely, each of the instantaneous observers at $z \in
N$ with co-ordinates $x(z)=(t, r,\vartheta, \varphi)$, carrying in
$T_zN$ an orthonormal frame $X=\{U, X_2, X_3, X_4\}$, is referred to
as $(z, X)$. The comoving dust-shell flow is modeled by its energy
stress \cite{SachsWu1977}  $T=\sigma \theta^{\rm U} \otimes
\theta^{\rm U}$, where the gravitational mass surface density $\sigma$
measured by $(z, X)$ takes the form, in the Schwarzschild spherical
co-ordinate system $x$,  $\sigma \circ x=\frac{dm}{4 \pi r^2
  \sqrt{h(r, m)}} \delta(x^1-r)$ and $\theta^{\rm U}$ is the dual of
$U$. Here, a more explicit notation $h(r, m)=1-\frac{2 m}{r}$ is
employed purely to emphasize the dependence on the mass parameter. The
use of the Dirac measure in the co-ordinate representation of $\sigma$
is but to indicate that  ${\rm supp}(\sigma\circ x)$ is the shell of
radius $r$ with zero thickness.

Before carrying out the computations, it seems worthwhile clarifying
here the meaning of ``work''. The absence of a globally defined
inertial reference frame in $N$ prohibits any definition of work in
the Newtonian fashion. However, the comoving feature of the dust-shell
described above facilitates the evaluation of the work done by the
observer field $U$ in the general relativistic context. An intuitive
physical picture of the hypothetical shell-building process resembles
very much a bucket brigade, where, by virtue of the spherical
symmetry, the observer field $U$ is regarded as a continuum of
radially lined up observers each exercising a certain amount of work
moving a bit of the gravitational mass of the shell infinitesimally at
their respective location. The total work, being a scalar, is
registered as the sum of the infinitesimal work from each
step. Precise calculations are as follows.

Suppose there exists already a spherical shell of gravitational mass
$m$ at radius $r_*$. In the instantaneous
inertial frame of each $(z, X)$, with $x^1(z)=r>r_*$, the measured
infinitesimal gravitational mass density $\sigma=T(U, U)$ gets moved
at the acceleration  $A=D_U U=\frac{m}{r^2 \sqrt{h(r, m)}} X_2$ by an
infinitesimal ``proper'' radial distance
$-\theta^2=-\frac{dr}{\sqrt{h(r, m)}}$. The infinitesimal work done in
each such step amounts, in the continuous limit, to the total work
done by the observer field $U$ throughout the entire moving process:
\begin{eqnarray}
&& W_U=\varint\limits_{0}^{{\rm M}} \varint\limits_{+\infty}^{r_*}
\varint\limits_{S^2} (\sigma\circ x)|_{x^1=r} g(A, X_2) \Omega_{S^2}
(-\theta^2) \cr && \qquad\qquad =-{\rm M}+r_*(1-\sqrt{h(r_*)}), \nonumber
\end{eqnarray}
where $\Omega_{S^2}$ is the standard volume form on $S^2$ and
$h(r_*)=1-\frac{2{\rm M}}{r_*} \in (0,1)$. Written in a more suggestive
form, the above relation, ${\rm M}={\rm QLE}(r_*)+ (-W_{\rm U})$, is
precisely Eq. (\ref{eqn:ADM}).

Recall the known inequality \cite{Bizon:1990nk} on the total
gravitational energy of a spherically symmetric distribution of matter
which is instantaneously at rest: ${\rm M} \leq {\rm M}_{\rm p} - E_{\rm B}$,
where ${\rm M}$ and ${\rm M}_{\rm p}$ are the total gravitational and the proper
mass of the distribution, respectively, and $E_{\rm B}$ is the binding
energy. The equality is achieved if and only if the general
relativistic configuration possesses the least binding energy, i.e., a
spherically symmetric shell as in the Newtonian limit. When ${\rm
  QLE}(r_*)$ is understood to be the proper energy within the radius
$r_*$ as in \cite{Brown:1992br}, $W_{\rm U}$ gives the least binding
energy required for the spherically symmetric shell configuration.

The geometry of the exterior of a spherically symmetric relativistic star is
known to be modeled by the Schwarzschild exterior $(N, g)$, provided that
the horizon is frozen inside the surface of the star. As another example,
the QLE of a spherically symmetric star is easily computed. For a mass
density $\rho(r)$, the gravitational  mass contained within a radius $r$ is
$m(r) = 4\pi \int dr\, r^2 \rho(r)$. Eq. (\ref{eqn:qleN}) indicates
that the slope of the QLE is discontinuous across the surface of the star.
Furthermore, based on the positivity of the mass density, the QLE is a
maximum at the surface of the star. Specifically, consider the case
of a constant density star of radius $r_*$ and gravitational mass ${\rm M}
\in (0, \frac{4}{9}r_*)$, with Schwarzschild radius $r_S = 2 {\rm M} <
r_*$. The QLE is
\begin{eqnarray}
{\rm QLE}&=& 2 {\rm M}\frac{r}{r_S} [1 - \sqrt{ h(r) } ]\cr
h(r) &=& 1 - \frac{r_S}{r}
\left(\left(\frac{r}{r_*}\right)^3\Theta(r_*-r) - \Theta(r-r_*)\right)
\label{eqn:star}
\end{eqnarray}
where $\Theta$ is the Heaviside function. The QLE grows inside the
star from the center to the surface, whereupon it decays to ${\rm M}$ at infinity
(see Figure~\ref{fig1}). The left (resp. right) radial derivative of the
QLE at $r_*$ tends to $+\infty$ (resp. $-\infty$) as $r_{\rm S}$
approaches $r_*$.

\begin{figure}[ht]
\includegraphics[scale=0.6]{fig1.eps}
\caption{The BY QLE for stationary, non-geodesic observers outside a constant
desity star of
mass $M$ and radius $r_*$ is shown. Four cases are shown
corresponding to $r_*/r_S=1$ (unstable, solid), and
$r_*/r_S=9/8,\, 3/2,\, 3$ (long-short-dashed, short-dashed, long-dashed
lines) where $r_S=2{\rm M}$ is the Schwarzschild radius of the star. In all
cases,
the slope of the QLE is discontinuous at the surface of the star.}
\label{fig1}
\end{figure}

\subsection{Non-static observer field}

It is natural to seek the QLE inside the horizon, in $B$ as well. The
investigation has been carried out recently in Ref.~\cite{Lundgren:2006fu},
wherein  an attempt has been made to continue the family of static,
non-geodesic Schwarzschild observers from $N$ into $B$. The result is that
the unit normal of $S^2$ as embedded in the space-like hypersurface $\Sigma$
is chosen to be time-like in $B$ (c.f. Eq.(16) in \cite{Lundgren:2006fu}),
thereby forcing the observer field to be space-like in $B$. This unphysical
choice for the observers seems incompatible with the construction of the
Brown-York QLE. The result in \cite{Lundgren:2006fu}, for
Schwarzschild space-time, is invoked in \cite{Blau:2007wj} to establish the
relationship between the Brown-York QLE measured by the
radial geodesic observers in $N \cup B$ and the effective potential of the
radial time-like geodesics. However, the observers used in
\cite{Lundgren:2006fu} are not geodesic and are valid in $N$ only, which
makes the analysis in \cite{Blau:2007wj} less justified. If instead
the geodesic observer field $V$ is employed in $B$, then the resulting
QLE is simply ${\rm QLE} = r$, which matches Eq. (\ref{eqn:qleN})
at the black hole horizon.
Similar calculations in more general
settings have been carried out in \cite{Booth:1998eh}, where the
``non-orthogonal'' boundaries are taken into account. The
non-orthogonality comes about by flowing the 2-dimensional closed
orientable space-like surface $S$ along an observer field $T$ that
differs from the unit time-like vector field $U$ that is orthogonal to
the 3-dimensional space-like hypersurface into which $S$ is
isometrically embedded. Such scenarios are of physical interest when
the so called ``boosted'' observer fields are considered. As a
consequence, a generalized reference embedding scheme has to be
devised to adapt the foliation of $S$ along the flow of $T$. In
particular, for the Schwarzschild space-time $N \cup B$, a natural
choice of $U$ in $N$ is the Schwarzschild static observer field, with
respect to which the observer field $T$ can be put in the form such as
Eq.(30) in Ref.~\cite{Booth:1998eh}. The different time orientation in
$B$, however, spoils the foliation by the privileged static observer
field and thus invalidates the choice of $T$ for $N$. Additional
comparison with the results in Ref.~\cite{Booth:1998eh} for  the
geodesic observer field in Schwarzschild geometry is given in
Sec.~\ref{geodesic}. In addition, so far as measurements are
concerned, it is always possible to associate to the observer field
2-dimensional closed orientable and space-like surfaces in the
orthogonal fashion as shown in what follows.

The crux of the matter is an observer field that can penetrate the
Schwarzschild horizon $r_S=2{\rm M}$. Such observer fields do exist. It is
perhaps more convenient to use the Kruskal space-time $K$. Note that the
radius function $r$ is well defined on all of $K$, whereas the time function
$t$ is defined only on $K-H$, where $H$ is the lift of $Q_{\rm H}$ and
represents the event horizon. By construction, $Y=\frac{1}{4 {\rm M}}
(v\frac{\partial}{\partial v}-u\frac{\partial}{\partial u})$ is a Killing
vector field on $K$ and equals $\frac{\partial}{\partial t}$ on $K-H$, but
$\frac{\partial}{\partial t}$ can be uniquely extended as a Killing field
over all of $K$. Hence, the Kruskal space-time can be time-oriented, in
accord with the physical interpretations on $N$, by requiring that
$\frac{\partial}{\partial t}$ be future-directed on $K_{\rm I}$.

Clearly, the observer field of interest here cannot be $Y$, which changes
its chronological signature in $K_{\rm II}$. It is, however, chosen, among
others, to be $X_1=\frac{1}{\sqrt{2 F(r)}} (-\frac{\partial}{\partial
u}+\frac{\partial}{\partial v})$, with its dual
$\theta^1=\sqrt{\frac{F(r)}{2}} d\xi$, where $\xi=-u+v$. Hence, $X_1$ is
synchronizable, i.e., there exists a unique space-like hypersurface
$\Sigma$ of $ {\cal M}$, the distribution on which is annihilated by
$\theta^1$, and thus completely integrable. Furthermore, the
co-ordinate function $\xi \circ \iota= \xi_0 ({\rm const.})$, where
$\iota: \Sigma \hookrightarrow  {\cal M}$. Given $X_1$, there exists
$X_2=\frac{1}{\sqrt{2 F(r)}} (\frac{\partial}{\partial
  u}+\frac{\partial}{\partial v})$, with its dual
$\theta^1=\sqrt{\frac{F(r)}{2}} d\rho$, where $\rho=u+v$, such that
$X_2$ is space-like and $\theta^1(X_2)=0$. Consequently, $X_2 \circ
\iota =X_2$ and in $\Sigma$, there exists a unique space-like
hypersurface $S$ of $\Sigma$, the distribution on which is annihilated
by $\theta^2$ and thus completely integrable. Similarly, the
co-ordinate function $\rho \circ \eta = \rho_0 ({\rm const.})$, where
$\eta: S \hookrightarrow \Sigma$. Thus, on $S$, $\xi=\xi_0$ and
$\rho=\rho_0$, and correspondingly, $t=t(\xi_0, \rho_0)={\rm const.}$ and
$r=r(\xi_0,\rho_0)={\rm const.}$, which implies that $(\iota \circ
\eta)^\ast g=r^2 g_{\rm S}$. That is, $S=S^2$. To complete the frame field
for the observer field, pick the usual orthonormal frame on $S^2$, namely,
$X_3=\frac{1}{r}\frac{\partial}{\partial \vartheta}$ and $X_4=\frac{1}{r
{\rm sin \vartheta}} \frac{\partial}{\partial \varphi}$, with their duals
$\theta^3=r d\vartheta$ and $\theta^4=r {\rm sin \vartheta} d\varphi$,
respectively.

The core of the calculation in Brown-York QLE is the mean
curvature of $S^2$ as embedded in $\Sigma$. However, substantial
simplifications are readily available in the current setting. Since $X_2 \in
\Gamma(\Sigma, T\Sigma)$, the induced connection ${\widetilde D}$ of $D$ on
$\Sigma$ coincides with the Levi-Civita connection $D^{\Sigma}$ of $\Sigma$,
thus, the second fundamental form of $S^2$ as embedded in $\Sigma$ with its
normal $X_2$ is given by
\begin{eqnarray}
\mathrm{I\!I}(X_l, X_l)&=&-\iota^\ast
g({\widetilde D}_{\eta_\ast X_l} X_2 \circ \iota, \eta_\ast X_l) \cr
&=& -g(D_{\eta_\ast X_l} \iota_\ast (X_2 \circ \iota), \eta_\ast X_l) \cr
&=&
\theta^2(D_{\eta_\ast X_l}\eta_\ast X_l), \nonumber
\end{eqnarray}
for $l=3, 4$. Standard Cartan calculus shows that $\mathrm{I\!I}(\theta^3,
X_3)=\mathrm{I\!I}(\theta^4, X_4)=\omega^2_3(\eta_\ast X_3)= -\frac{\sqrt{2 F(r)}}{8 M
r}(u+v)$, where $\omega$ is the connection 1-form on $M$. Hence, the trace
of the mean curvature is $k={\rm tr}\mathrm{I\!I}=-\frac{\sqrt{2 F(r)}}{4 {\rm M} r}
(u+v)$. On the other hand, the flat-space reference embedding $\eta^0: S^2
\hookrightarrow {\mathds R}^3$ yields $k^0={\rm tr} \mathrm{I\!I}^0=-\frac{2}{r}$.
Therefore, the Brown-York QLE is given by
\begin{eqnarray}
{\rm QLE}(t, r)&=&\frac{1}{8 \pi} \varint\limits_{S^2} (k-k^0)\Omega \cr
&=& r\Big[1-\frac{\sqrt{2 F(r)}}{8 {\rm M}}(u+v)\Big] \cr
&=& r\Big[1 - \delta \sqrt{h(r)} {\rm cosh} (\frac{t}{4 {\rm M}})\Big],
\nonumber
\end{eqnarray}
where $\Omega$ is the volume form of $S^2$ and $\delta= 1$ on
$K_{\rm I}$ (exterior) and $-1$ on $K_{\rm II}$ (interior).

\begin{figure}[ht]
\includegraphics[scale=0.6]{fig3.eps}
\caption{The Brown-York QLE for non-geodesic observers, $X_1$, outside a
black hole  of mass ${\rm M}$ is shown. Three cases are shown, corresponding to
maximum radius given by $r_{\rm max}/r_S =1, 3/2, 2$ (solid, short-dashed,
long-dashed lines). Note that QLE decreases smoothly as the observer crosses
the horizon.}
\label{fig3}
\end{figure}

The QLE measured by the observers $X_1$ on $S^2$ depends on
both Schwarzschild functions $t$ and $r$, subject to the conditions
$\xi\circ\iota={\rm const}.$ and $\rho\circ\eta={\rm const}.$. This result
differs from that measured by the Schwarzschild observers $U$ in $N$ because
$X_1$ and $U$ produce different foliations of the space-time manifold. The
key difference, though, is that $X_1$ is an observer field over all of $K$,
while $U$ is defined on $N \approx K_{\rm I}$ only.
The QLE is illustrated in Fig.~\ref{fig3}. In contrast to the case of
the static observer field, $D_{X_1}X_1=-\frac{1}{16{\rm
M}}(u+v)(\frac{1}{r(u,v)}+ \frac{1}{2{\rm M}})\sqrt{2 F}X_2$, the
work done by $X_1$ to build up the spherically symmetric shell of
gravitating mass ${\rm M}$ and radius $r_*$ is negative for $r_* \in {\rm
QLE}^{-1}({\mathds R}^-)$.

\section{Measurement by geodesic observers}
\label{geodesic}

A different type of observer field of physical interest is the geodesic
observer field in $N \cup B$, which crosses the event horizon. The
isometries of $S^2$ admit a system of the Schwarzschild spherical
co-ordinates with respect to which each of the geodesic observers, $\gamma:
{\mathscr E} \longrightarrow  {\cal M}$, is initially equatorial, i.e., $\vartheta
\circ \gamma \equiv \frac{\pi}{2}$, and thus, $X_1= {\dot
\gamma}=\frac{E}{h(r)}\frac{\partial}{\partial t} + \delta \sqrt{E^2 -
V(r)}\frac{\partial}{\partial r} + \frac{L}{r^2}\frac{\partial}{\partial
\varphi}$, depending upon whether the geodesic is ingoing ($\delta=-1$) or
outgoing ($\delta=+1$). Here the constants $L$, the angular momentum per
unit mass of the observer, and $E$, the energy per unit mass at infinity,
are related via the energy equation $E^2 =(\frac{d}{d\tau} (r \circ
\gamma))^2 + V(r)$, with $V(r)=(1+\frac{L^2}{r^2}) h(r)$ being the effective
potential. Of course, $X_1$, as a unit vector, is not defined on the horizon
$H$, in the Schwarzschild spherical co-ordinates, as usual; the energy
equation, nonetheless, holds by continuity.

For simplicity, only radial geodesics ($L=0$) are considered, in which case
two kinds of ordinary orbits are available: (1) the crash orbit ($E^2 \in
(0,1)$), where ingoing observers crash directly into the singularity at
$r=0$ and outgoing observers shoot out to a turning point $r_{\rm max}$
($E^2=h(r_{\rm max})$) and then back into crash; (2) the crash/escape orbit
($E^2 \in [1, +\infty)$), where ingoing observers crash while outgoing
observers escape to infinity. In $N \cup B$, the radial geodesic observer
field $X_1=\frac{\partial}{\partial \xi}$ is proper time synchronizable
since the dual frame $\theta^1=d\xi$, where
$\xi=Et-\int\limits_{r^\prime=r_0}^{r} \delta \frac{\sqrt{E^2 -
h(r^\prime)}}{h(r^\prime)}dr^\prime$. The rest of the construction follows
the same lines as in Sec.~\ref{nongeodesic}. There exists a space-like
$X_2=\frac{1}{\sqrt{E^2-h(r)}}\frac{\partial}{\partial \rho}$ chosen to be
consistent with the positive orientation of $\Sigma$ as embedded in $M$.
$X_2$ is synchronizable since $\theta^2=\sqrt{E^2-h(r)} d\rho$, where
$\rho=-\delta t + \int\limits_{r^\prime =r_0}^{r} \frac{E
dr^\prime}{h(r^\prime) \sqrt{E^2 - h(r^\prime)}}$. Hence, there exists a
co-dimension 1 embedding $\eta: S=S^2 \hookrightarrow \Sigma$ such that
$\rho \circ \eta=\rho_0 ({\rm const.})$. The mean curvature of $S^2$ as
embedded in $\Sigma$ with the unit normal $X_2=X_2 \circ \iota$ is given by
$k={\rm tr}\mathrm{I\!I}=- 2 \frac{E}{r}$, where $r=r(\xi_0, \rho_0)$, with the
reference part intact. Therefore, the Brown-York QLE measured
by the geodesic observer field in $N \cup B$, for crashing orbits, is ${\rm
QLE}(r)=r(1-E)$, where $r \in (0, r_{\rm max}]$. Note that $E(r)$ remains
valid at $r=2{\rm M}$ by continuity.

In contrast to the analysis in \cite{Blau:2007wj}, the QLE
measured by the geodesic observer field does not seem to be related to the
effective potential in a non-trivial fashion. It is, however, simply linear
in the radius function $r$. At the turning point $r_{\rm max}$ for crash
orbits, ${\rm QLE}(r_{\rm max})=\frac{2{\rm M}}{1+E}$. At the event horizon,
${\rm QLE}(r)$ remains valid by continuity, and  ${\rm QLE}(r=2{\rm
M})=2{\rm M} (1-E)$.  A critical  situation is when $E^2=1$ and each
observer in this geodesic observer field starts at rest from infinity. In
the course of freely falling towards the singularity, the QLE
measured by this family of geodesic observers vanishes identically.
Interestingly, when $E^2>1$, the QLE become negative. This
result follows from the definition of the Brown-York QLE, whose sign is
determined by that of the sectional curvature of the 3-dimensional
space-like hypersurface $\Sigma$ into which the 2-dimensional consistently
oriented, closed, space-like surface $S$ is isometrically embedded. For the
geodesic observer field $X_1$, the sectional curvature of $\Sigma$ is
$K(\Sigma)=\frac{1-E^2}{r^2}$, which is positive ($E^2 \in (0,1)$), zero
($E^2=1$), or negative ($E^2 \in (1, +\infty)$). When compared to the
reference term evaluated in ${\mathds R}^3$, the Brown-York QLE becomes
positive, zero, or negative, respectively. In Figure~\ref{fig2}, different
QLE measurements are plotted for illustrative purposes.

These results are different from those measured by the radially infalling
observers with $E=1$ considered in Ref.~\cite{Booth:1998eh}. As explained in
Sec.~\ref{nongeodesic}, the discrepancy arises from the generalized
embedding scheme  (c.f. Eq.(40)) in \cite{Booth:1998eh}, in accord with the
non-orthogonal boundaries. Should an $S^2$ that is orthogonal to $T$ be used
in \cite{Booth:1998eh}, the same QLE as given here follows immediately.

\begin{figure}[ht]
\includegraphics[scale=0.6]{fig2.eps}
\caption{The Brown-York QLE for geodesic observers outside a black hole of
mass $M$ is shown. Three cases are shown, corresponding to bound
trajectories with energy per unit mass $E = \sqrt{h(r_{\rm max})}$ starting
at a maximum radius given by $r_{\rm max}/r_S =1, 3/2, 3$ (solid,
short-dashed, long-dashed lines). Note that QLE decreases smoothly as the
observer crosses the horizon. In the case of an observer starting at $r_{\rm
max}/r_S \to \infty$, the QLE is zero.}
\label{fig2}
\end{figure}

It is curious to note that a star with mass density $\rho \propto r^{-2}$,
albeit unphysical due to the existence of a curvature singularity at the origin,
gives rise to a well-behaved QLE. In view of Eq.(\ref{eqn:star})
for observers $U$ in $N$, and observers $V$ in $B$,
${\rm QLE}= 2 {\rm M}\frac{r}{r_S}[1 - \sqrt{h(r)}]$ with $h(r)=1 -
\frac{r_S}{r_*}\Theta(r_*-r) - \frac{r_S}{r}\Theta(r-r_*)$. The
non-geodesic, stationary observer QLE curves in the limiting case $r_*/r_S\to 1$
and $r_*/r_S= 3/2,\, 3$ coincide with the curves for geodesic observers shown in Figure~\ref{fig2}.

The rest of this section is devoted to a discussion of the measurement
of the quasi-local momentum by a family of geodesic observers. Similar
analysis can be carried out, though more complicated, for non-geodesic
observers, as well.

Consider an orthonormal frame field $\{X_i\}_{i=1}^{i=4}$, in which $X_1$ is
time-like geodesic and (locally) synchronizable. $\forall p \in {\cal M}$, $T_p
 {\cal M}={\mathds R}X_1 \oplus {\rm R}_p  {\cal M}$, where  ${\rm R}_p  {\cal M}={\rm
span}_{\mathds R}\{X_i\}_{i=2}^{i=4}$. The Brown-York quasi-local momentum
density ${\mathscr J} \in R^\ast  {\cal M}$ is defined by \cite{Brown:1992br}
${\mathscr J}(Y_p)=-\frac{1}{8\pi}\Big(\Theta \iota^\ast g(Y_p, X_2) -
\mathrm{I\!I}^{X_1}(Y_p, X_2)\Big)$, $\forall (p, Y_p) \in R^\ast  {\cal M}$, where
$\Theta={\rm div} X_1$ is the expansion of the (local) flow of $X_1$ and
$\iota: \Sigma \hookrightarrow  {\cal M}$ is the (local) embedding induced by $X_1$.
When restricted to the 2-dimensional orientable closed space-like surface
$S$ embedded in $\Sigma$, whenever $\Sigma$ is completely integrable,
$\mathscr J$ is the quasi-local momentum surface density $j$, as originally
given in \cite{Brown:1992br}. It is clear from the definition that the
reference term for the quasi-local momentum vanishes identically when the
flat-space reference is employed. Hence, only the physical part is
considered in what follows.

Given a one-parameter family of time-like geodesics  $x: {\mathscr E} \times
(-\delta, +\delta) \longrightarrow  {\cal M}$ around the base, $\gamma:{\mathscr E}
\longrightarrow  {\cal M}$ given by  $\gamma u=x(u,0)$, where $\gamma_\ast
\frac{d}{du}=X_1$, the Fermi-Walker connection \cite{SachsWu1977} coincides
with the induced connection $\gamma^\ast D$ over $\gamma$. For economy of
notation, there is no differentiation among various connections whenever the
context is clear. Recall that a  {\it neighbor} of the base is given by a
Jacobi field,  $J \in \Gamma({\mathscr E}, R {\cal M})$, over $\gamma$, as those
Jacobi fields that are tangent to $\gamma$ are of scant importance. It is
then convenient to introduce the following natural decomposition: $J=J^\bot
+ J^\top$, where $J^\bot =\theta^2(J)$ and $J^\top =J-J^\bot$. Accordingly,
the 3-relative quasi-local momentum density measured by a neighboring
observer with respect to the base is  ${\mathscr J}(J)={\mathscr J}(J^\bot)
+ j(J^\top)$. Thus, the Brown-York quasi-local momentum surface density
$j(J^\top)$ measured by the neighbor is the component that is tangent to
$S$, the orthogonal complement being the normal stretch ${\mathscr
J}(J^\bot)$.

The relative quasi-local momentum density in the family of geodesic
observers is obtained with the help of the Raychaudhuri equation for
time-like geodesics. Further simplifications emerge as the space-time of
interest is Ricci-flat. Since $X_1$ is (locally) synchronizable, hence
irrotational \cite{SachsWu1977}, the Raychaudhuri equation becomes
$\frac{d}{du}\Theta=-\frac{1}{3} \Theta^2 -{\rm tr}(\sigma^2)$, where
$\sigma$ is the shear of $x$. Hence,  $\frac{d}{du}{\mathscr
J}(J)=-\frac{1}{8\pi}\Big[ \Theta {\mathscr J}(J) - (\Theta^2 + \mathrm{I\!I}^{X_1}
\cdot \mathrm{I\!I}^{X_1}) \iota^\ast g (J, X_2) - g(R_{J X_1}X_1, X_2)\Big]$, where
$\mathrm{I\!I}^{X_1} \cdot \mathrm{I\!I}^{X_1}=\sum\limits_{i=2}^{i=4} \sum\limits_{j=2}^{j=4}
\mathrm{I\!I}^{X_1}(\theta^i,\theta^j)\mathrm{I\!I}^{X_1}(X_i,X_j)$.  When restricted to $S$, it
yields
$$
8\pi \frac{d}{du} j(J^\top) + \Theta j(J^\top)=
g(R_{J^\top X_1}X_1, X_2),
$$
where $g(R_{J^\top X_1}X_1, X_2)$ is the tidal force exerted on the neighbor
tangent to $S$ in the $X_2$-direction.

It is hoped that the above analysis provides a slightly different
perspective towards understanding the dynamics of the quasi-local momemtum
measured by the family of geodesic observers.

\vspace*{0.2cm}
\section{Summary and discussion}
\label{summary}

The measurements of the Brown-York QLE in Schwarzschild space-time by a
non-static, non-geodesic observer field that penetrate  the event horizon
and by a geodesic observer field have been computed. It has been shown that
due to a different space-time foliation induced by the observer field, the
measurement of QLE by the non-static, non-geodesic observer field depends on
both the radius function $r$ and the time function $t$. The QLE measured by
a geodesic observer field is, however, linear in the radius function $r$, and
can be positive, zero, or negative, depending upon the energy parameter of
the geodesic observer field. These results differ significantly from the
measurement by a static observer field in the Schwarzschild exterior $N$,
which is previously known. On the other hand, the Liu-Yau QLE is independent
of the choice of observer field in $N$ and coincides with the Brown-York QLE
measured by the static observer field in $N$. However, the Liu-Yau QLE is
not defined in Schwarzshild interior $B$ because the mean curvature vector
of the co-dimension 2 isometric embedding of $S$ into $M$ becomes
time-like.

To explore more about the physical nature of QLE, a hypothetical process of
building a spherically symmetric massive shell by a static observer
field was considered. The gravitational mass of the spherically
symmetric shell is the QLE of the shell plus the negative
gravitational potential energy associated with the work exercised to
build the shell. The result holds for both the Brown-York and the
Liu-Yau QLE since they coincide in $N$ for the static observer
field. In addition, the QLE of a spherically symmetric star with
constant density in the interior is also calculated. The QLE grows
monotonically with respect to radial distance from the origin in the
interior and drops off in the exterior towards the ADM mass ${\rm M}$ at
infinity, with a cusp on the surface of the star. It seems to provide
certain physical justification for QLE as a viable measure of energy.

For a geodesic observer field in the Schwarzshild geometry, a dynamic
relation of the Brown-York quasi-local momentum density has been noted. It is
valid for any Ricci-flat space-time. When a family of geodesic observers are
assigned on $S$ to carry out physical measurements, this relation is
expected to describe their relative dynamics. Generalization to more
realistic Fermi-Walker observer fields is straightforward but more
complicated.

\begin{acknowledgments}
PPY wishes to thank Professor C. Sutton for useful discussions.
RRC was supported in part by NSF AST-0349213.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


text:
Q: preventDefault() is not working giving object does not support this property I want to set maximum length of a textbox to 7 and stop further keys entering and using preventDefault but its giving error
My Code is below
function crInputRK(ctrlid, ControlValue, size, clsName)                                    {

    var newTextBox = crE('input');
    newTextBox.type = 'text';
    newTextBox.style.fontSize = ".9em";
    newTextBox.style['width'] = size;
    newTextBox.style['height'] = '12px';
    newTextBox.style['float'] = 'none';
    newTextBox.style['margin'] = '0 0 0 10px';//added on 13feb2012
    //newTextBox.maxLength = '3';
    newTextBox.id = ctrlid;

    newTextBox.className = 'inputDate';

    //newTextBox.onchange = "javascript:return EnableButton();";

    //ControlValue = getControlValue(ctrlid);
    if (ControlValue != "")
        newTextBox.value = ControlValue;
    if (ControlValue == "Multiple")
        newTextBox.disabled = true;
      newTextBox.setAttribute("onkeypress", "javascript:SetMaxLength(event,this);");

    return newTextBox;
}

function SetMaxLength(e, txtbox)                                                           {

    var MaxLength = 7;
    if (_$(txtbox.id).value.length >= MaxLength) {
        e.preventDefault();

    }
}

A: Just an option:

var MaxLength = 7;
if (_$(txtbox.id).value.length >= MaxLength) {
  _$(txtbox.id).value = _$(txtbox.id).value.substring(0, MaxLength);
}

A: Input fields that require monitoring of keystrokes needs to be evaluated under the scope of 'on' (jQuery 1.7+) or 'live' (jQuery 1.4.2-1.7). If you don't, the input field will only be evaluated on page load. So you need to monitor the input doing something like...
function SetMaxLength(e,txtbox){
  var MaxLength = 7;
  $("#"+_$(txtbox.id)).live('keyup', function(e){
    if (_$(txtbox.id).value.length >= MaxLength) {
      e.preventDefault();
    }
  });
}

This will monitor your field for all actions, and if the length is greater than MaxLength it will not perform the default actions.

A: event.preventDefault isn't cross browser compatible if you need to support older Internet Explorer versions, try using events instead (assuming you have jQuery available):
jQuery(newTextBox).bind('keypress', SetMaxLength);

Your SetMaxLength function will then run in the scope of the text box rather than having it passed as an argument:
function SetMaxLength(e, txtbox) {
  var MaxLength = 7;
  if (this.value.length >= MaxLength) {
    return false; // or e.preventDefault();
  }
}

A: It is possible using .preventDefault();
 $("body").find("input[type=text]").each(function(k,v) {
     $(this).on('keypress', function(event) {
        limit = 7; //for example
        val = $(this).val();
        len = val.length;
        if(len > limit-1) { event.preventDefault(); }
             });
    });

Demo


text:
Nonea multicolor är en strävbladig växtart som beskrevs av G. Kunze. Nonea multicolor ingår i släktet nonneor, och familjen strävbladiga växter. Inga underarter finns listade i Catalogue of Life.

Källor

Nonneor
multicolor