I spent a good number of sleepless nights the past month trying to figure out time management, cutting down on work and prioritising my sanity. But, you know, when it rains, it pours. All my 'strategizing' has been gently kicked out the window with work days extending way into the late hours, mindboggling projects and so much paperwork that the kitchen adventures have had to take a bit of a backseat. And I have truly missed the kitchen.
So one night I decided to quit midweek and spend a laborious morning in the kitchen, with recipes that entail lengthy procedures whilst listening to some very good music, and sipping on cups of delicious coffee. I finally felt human all over again!
So this recipe is something rather unique – a spaghetti cake! This is perhaps a bit further from the usual kitchen therapy travails – it requires patience and quite some time, but I can assure you – it is all worth it!
The pasta is cooked, and divided between three sauces then layered into a well-oiled cake tin and the baked – with copious amount of cheeses!
While the recipe normally asks for spaghetti, I went for a packet of bucatini – a slightly thicker spaghetti with a hole running through it, that is traditionally used in the Italian meat sauce – amatriciana, based on guanciale, pecorino, tomatoes and chilli peppers. This type of pasta works very well with buttery sauces and maintains good shape for this pie. But feel free to use any sort of pasta and of course, instead of three kinds of sauces, you can go ahead and use just one – the choice is yours.
Place the beetroots, garlic, walnuts, salt and olive oil into a processer and grind down to a smooth mixture.
Transfer the mixture into a medium sauce pan and place on low heat. Let the sauce cook, stirring a few times.
Add the milk in and cook for another 6-7 minutes.
Place a medium pan on the low heat with olive oil, onions and garlic.
Cook until fragrant and then add the spinach with the herbs, chilli flakes and salt. Let the sauce cook for at least 10 minutes and then add the cream and stir.
Heat a pan with the olive oil and garlic.
Once the garlic has almost cooked, add the saffron and stir for a few minutes.
Then add the cream and salt and stir well. Let the sauce cook for a few more minutes before setting aside.
Divide the bucatini between the three sauces to coat each strand well.
Similarly divide the cheeses between the three sauces and mix well.
Grease a 9" cake tin well with olive oil.
Layer the beetroot sauce pasta first and press down well. Then layer the saffron sauce mix, followed by the spinach sauce pasta.
Add some cheese on top and drizzle a few drops of olive oil.
Bake in a preheated oven for 30 minutes at 180C.
Remove from oven and let cool for a few minutes before turning over onto serving dish.
Serve by slicing the 'cake' into slices.
What a wonderful idea! trying to make it at home tonight!!!


text:
How are filming permits issued for Altadena? How can I host a film shoot? Are there any limits on filming? Who should I contact if there's a problem with a production? www.altadenafilming.org is a resource for learning about filming in our community.
Notice: FilmLA, has updated and reorganized its website. In the process, many of our links to their site were broken. Most have been repaired by referencing archived copies stored at AltadenaFilming.org. Please let us know if you encounter a broken link. (1/6/20)
The new Altadenafilming listing service
Would you like to meet film location managers who are looking for filming locations in Altadena? If so perhaps you'll be interested to learn of a new service we're providing here AltadenaFilming.
We just started two new listing services:
(click on the following links for more information)
Community Members who would like to host a film shoot
Location Managers looking for Altadena locations
The "Community Members" list is intended for those Altadeneans who are interested in meeting film location managers who looking for new locations. The "Location Manager" list is intended for location managers interested in meeting members of the Altadena community who would like to host a film shoot.
It's part of an effort to broaden the benefit the wider Altadena community enjoys from film shoots by supporting Altadena nonprofit organizations. In other words, if you make a donation to an Altadena nonprofit, we would like to add your name to our list.
To date, Altadena Filming has made an arrangement for an information exchange with Altadena Heritage. If a Altadena community member makes a donation to Altadena Heritage, we can add your information to the list.
The Altadenafilming listing service is just getting underway. Both lists are presently empty. In time we hope the lists will grow and this service will stimulate donations to Altadena non-profits.
Note: Altadenafilming does not receive any benefit from your donation aside from the satisfaction of helping local non-profits.
Altadena Community Chest
It shouldn't go unsaid that the Altadena Community Chest also provides an excellent method for making filming-related contributions to our community non-profits. The Altadena Community Chest is associated with Home Shoot Home which provides location services for production companies wanting to shoot in our community.
The Altadena Community Chest has an impressive record of giving to our local non-profits. Both the Altadena Community Chest and Home Shoot Home are run by our fellow Altadenean, Russ Fega.
Posted by Kenny Meyer at 5:52 PM
AF Resources
Altadena Filming FAQ
Altadena Filming Map
Photos, footage and historical notes
Legalities and Analysis
Guidelines for Altadena Neighbors and Filmmakers
Filming data
Netflix's Bird Box: Map of filming locations
Cost of a film permit in Altadena. Is it cheap?
Jobs and Georgia on my mind
Filming history for Altadena locations now available on the Altadena Filming Map
The Data Chase (part 1): "Learning the ropes"
Disclaimmer: AltadenaFilming.org is a volunteer effort intended to provide a service to the community. The views expressed here are strictly our own. Postings may report on Altadena Filming Committee activities, but these reports should not be mistaken for the Committee's actual findings or recomendations. In addition, AltadenaFilming.org has no special affiliation with any organizations connected with the film industry. Your comments, suggestions, and corrections are welcome. Let us know if you have a topic of interest you would like to see posted. Please feel free to contact us at altadena.neighbors.4.ok.film@gmail.com
Annoucements (14)
FilmLA (13)
Altadena Filming Committee (12)
LACO Ordinance (10)
Helpful Suggestions (7)
FilmLA contract (5)
FilmLA policies (5)
Altadena Heritage
Altadena Historical Society
Altadena Special Filming Conditions
Altadena Town Council
Directors Guild of America
FilmLA
LA County Economic Development Corp.
Location Manager's Guild

redpajama_set_name: RedPajamaCommonCrawl


The main aim of REGTREND (Quantifying uncertainties in regional climate trends and its implications for adaptation decision-making) to revisit the uncertainties caused by natural variations in recent and future trends of user-relevant climate variables at regional scales, and assess how improved and more trustworthy information on uncertainties can be managed and reflected in decision-making processes.
Climate change will affect actors in all sectors of society. Thus it is imperative that authorities, municipalities, businesses and individual property owners all take action to adapt to the ongoing and future change. Municipalities and other local and regional actors are the ones that account for the bulk of the implementation of concrete measures and practical implementation of adaptation action.
Decision-makers do often only have access to a small part of the results from all existing climate model simulations as input for adaptation actions. At the regional scale, existing ensembles are generally too small to capture the full range of uncertainty caused by natural climate variability, which can have an overriding impact on the projected trends in time scales relevant for adaptation. This means that future changes can be foreseen to differ significantly from the information today´s decisions are based on.
To overcome this fundamental problem, REGTREND will analyze new, recently performed large ensemble simulations with global climate models. The available number of global model simulations is at least a factor of 10 higher than the number of regional model simulations, on which climate information to stakeholders are built today.
We aim to identify the regions where the uncertainty of future climate changes is particularly large or small. The main focus will be on Europe and Sweden.
The results from the global models will be compared to the existing simulations with regional models over Europe and Sweden. It is important to find out to which degree the regional model simulations cover the climate change uncertainties and if there are systematic differences in the climate change signals between regional and global model simulations. Combining the probabilistic information from the high number of global model simulations with the higher-resolved but case-specific information from the limited number of regional simulations will lead to more trustworthy regional information to decision-makers.
REGTREND also aims to advance the understanding of the physical processes, which might govern the variability of regional trends. Possible linkages between specific regional trends and potential large scale drivers as atmospheric circulation patterns or ocean currents and surface temperature distributions will be investigated.
In collaboration with decision-makers and planners at the local and regional level, REGTREND aims to assess how improved and more trustworthy information on uncertainties can be managed. This will be assessed for different approaches including: adaptive management (the selection of a strategy that can be modified to achieve better performance as one learns more about the issues at hand and how the future is unfolding), scenario planning (with consideration of multiple plausible outcomes to compare how well alternative policy decisions perform), and robust or resilient strategies (that will work reasonably well across the predicted range of future climate). We will also assess how more detailed information on uncertainties can be merged to already available information. In Sweden, this includes recently published reports with regional climate change assessments of a set of climate indexes based on RCP4.5 and RCP8.5 for each of Sweden´s 21 counties.
REGTREND will run from 2017-2019.
REGTREND is funded by FORMAS.
You will be sending an email to Torben Königk.


When patients obtain care outside of the primary care delivery system or physician network to which they are attributed, this out-of-network utilization can have tremendous impacts on the financial health of a provider organization — especially when that patient is part of a value-based contract.
Siloed data. Despite all the hype around interoperability and data, health industry stakeholders are not always able to share their data. That makes it difficult to manage patients who go to clinics or hospitals that are not connected.
Wasted resources. Costs increase as patients aren't as carefully managed. The results are often redundant services and/or services delivered by higher cost practitioners — with no increase in quality.
Disconnected care. Effectiveness of care coordination declines because clinicians can't easily communicate.
Poor results. Patient well-being and outcomes may become compromised.
The biggest impact patients going out of network can have is on the continuum of care. An in-network provider cannot manage the quality of care that a patient receives when they leave the system. How is a provider to know what a patient is seeing an outside physician for if a patient does not report the information, and what does that mean for the treatments they're receiving from in-network doctors?
NYUPN Clinically Integrated Network, a collaboration between the University Physician Network and NYU Langone Medical Center in Manhattan, New York, proactively analyzed its data and identified an issue with patients seeking care outside their care provider network. Within weeks, they applied data to help alleviate the issue.
New York City is home to many world-renowned health care organizations, all within a small geographic area. It's easy to see how patients seeking care with out-of-network physicians or facilities could become a problem. Group leaders knew they needed to influence patients to stay within NYUPN's network of clinicians and hospitals, and they determined the way to do so was to influence a critical patient gatekeeper: their physicians.
Using reports that allowed them to drill down to source data, NYUPN population health leaders aggressively educated physicians about how often their patients used out-of-network resources, and discussed the consequences that such usage had on quality of care and managing costs.
Their efforts worked. NYUPN increased its in-network utilization by 5 percent.
This entry was posted in OptumIQ. Bookmark the permalink.
← These boots were made for walking — on a treadmill!


text:
using System;
using System.Data;
using System.Data.SqlClient;
using Codeo.Data.Cache.Contract;
using Codeo.Data.Cache.Extension;
using Codeo.Data.Cache.Factory;
using Codeo.Data.Orm.Contract;
using Codeo.Data.Orm.Exception;

namespace Codeo.Data.Orm.Impl.SqlServer
{
    public class SqlDataContext : IDataContext
    {
        private readonly IMapper _mapper;
        private readonly ICacheService _cacheService;
        private readonly string _connectionString;
        private readonly int _connectionTimeout;

        public SqlDataContext()
        {

        }

        private SqlDataContext(IMapper mapper, ICacheServiceFactory cacheServiceFactory)
        {
            _mapper = mapper;
            _cacheService = cacheServiceFactory.Build(TimeSpan.FromMinutes(0));
        }

        public SqlDataContext(string connectionString, IMapper mapper, ICacheServiceFactory cacheServiceFactory) : this(mapper, cacheServiceFactory)
        {
            _connectionString = connectionString;
        }

        public SqlDataContext(string connectionString, int connectionTimeout, IMapper mapper, ICacheServiceFactory cacheServiceFactory) : this(connectionString, mapper, cacheServiceFactory)
        {
			_connectionString = connectionString;
			_connectionTimeout = connectionTimeout;
        }

        public void LockTable()
        {
            throw new NotImplementedException();
        }

        public IResult Execute(IStatementBuilder statement)
        {
            IResponse response = null;
            try
            {
                using (SqlConnection connection = new SqlConnection(_connectionString))
                {
                    connection.Open();
                    IDbCommand cmd = statement.Command;
                    cmd.Connection = connection;
                    cmd.CommandTimeout = _connectionTimeout;
                    switch (statement.Type)
                    {
                        case QueryType.Insert:
                            var sc = cmd.ExecuteScalar();
                            response = new SqlResponse(sc, statement.Type);
                            break;
                        case QueryType.Update:
                        case QueryType.Delete:
                            cmd.ExecuteNonQuery();
                            response = new SqlResponse(null, statement.Type);
                            break;
                        case QueryType.SelectSingleValue:
                            var sr = cmd.ExecuteScalar();
                            response = new SqlResponse(sr, QueryType.SelectSingleValue);
                            break;
                        case QueryType.SelectSingleRow:
                            var sdr = cmd.ExecuteReader(CommandBehavior.SingleRow);
                            response = new SqlResponse(sdr, QueryType.SelectSingleRow);
                            break;
                        case QueryType.SelectMultipleRows:
                            var mdr = cmd.ExecuteReader(CommandBehavior.Default);
                            response = new SqlResponse(mdr, QueryType.SelectMultipleRows);
                            break;
                    }
                    connection.Close();
                }
            }
            catch (SqlException)
            {
                throw;
            }
            catch (System.Exception e)
            {
                throw new MappingException(e.Message, e.InnerException);
            }
            return new SqlResult(_mapper, response);
        }

        public IResult CacheExecute(IStatementBuilder statement, Func<string, IResult, bool> expirationCallback)
        {
            if (statement.Type == QueryType.Delete || statement.Type == QueryType.Update || statement.Type == QueryType.Insert)
            {
                throw new System.Exception("Cache cannot be used with insert, update or delete query");
            }
            else
            {
                string cacheKey = statement.ToString();
                return _cacheService.Get(cacheKey, statement, expirationCallback, Execute);
            }
        }

        public IResult CacheExecute(IStatementBuilder statement, TimeSpan duration)
        {
            if (statement.Type == QueryType.Delete || statement.Type == QueryType.Update || statement.Type == QueryType.Insert)
            {
                throw new System.Exception("Cache cannot be used with insert, update or delete query");
            }
            else
            {
                string cacheKey = statement.ToString();
                return _cacheService.Get(cacheKey, statement, Execute, duration);
            }
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
The longstanding attempt to legislate Indigenous-Asian relations out of existence continues to cast its shadow today. Cathy Freeman is identified as Australia's most famous Indigenous sportswoman, but she is also of Chinese descent. In the late 19th century, her great-great grandfather moved from China to northern Queensland, where he worked on sugarcane farms. In 2001 Freeman supported Beijing's bid for the 2008 Olympic Games because of her Chinese heritage, but the English-language Australian media has entirely overlooked it. By contrast, in Chinese-language media inside and outside Australia, Freeman's multicultural heritage is celebrated; many Chinese-Australians even hoped Freeman would win gold in the Sydney Olympics because of her Chinese descent. Is the suppression of Freeman's heritage a sign that white Australia still wants to keep Asians and Aborigines apart?
Peta Stephenson, The Outsiders Within: Telling Australia's Indigenous-Asian Story, (Sydney: University of New South Wales Press, 2007), 2.
« The New Normal
Hapa, Amerasian, Euro-Asian, or 'Other' »
Richard Pryor's Daughter on Growing Up Biracial
WNYC Radio
WNYC News
Soterios Johnson
April 7, 2013 – Richard Pryor, one of the most influential comedians of all-time, gained pop star status in the 1970's with his incisive storytelling about issues including race. Now, his daughter Rain is sharing her take on growing up biracial in '70s and '80s Los Angeles, the child of the African-American comic genius and a Jewish go-go dancer.
In her one-woman show, "Fried Chicken and Latkes," Pryor brings to life the family members, societal pressures and personal experiences that forged her identity at a time when attitudes about race in the U.S. were rapidly changing.
"I really wanted to tell a story about me, so people would get to know who I am," Pryor said. "But at the same time really talk about things that were important to me. And, race was always such a big issue for me, and still is, especially in our country."…
Read the entire article here. Download the interview here.
Tags: Rain Pryor, Richard Pryor, WNYC, WNYC News, WNYC Radio
This entry was posted	on Friday, April 12th, 2013 at 20:00Z	and is filed under Articles, Audio, Autobiography, Interviews, Media Archive, United States, Women. You can follow any responses to this entry through the RSS 2.0 feed. Both comments and pings are currently closed.


Envirocare's Southampton depot were recently tasked to reinstate a fire break around a site perimeter and reduce the tree height.
Non of the staff there had ever used or worked on a MEWP (a Mobile Elevating Work Platform – a powered machine that offers a temporary work platform allowing work to be conducted safely at height).
All the Southampton staff were trained to use the MEWP as well as additional chainsaw training – meaning that the Southampton depot is now fully competent, trained and risk assessed for this difficult task.


text:
Global Partners Reports Third-Quarter 2012 Financial Results
- Net Income of $6.9 Million, or $0.24 per Unit
- Product Volume Increases 25% to Record 1.6 Billion Gallons
WALTHAM, Mass.--(BUSINESS WIRE)--Nov. 8, 2012-- Global Partners LP (NYSE: GLP) today reported financial results for the quarter ended September 30, 2012.
Third-Quarter 2012 Financial Summary
Net income for the third quarter of 2012 was $6.9 million, or $0.24 per diluted limited partner unit, compared with net income of $1.9 million, or $0.08 per diluted limited partner unit, for the third quarter of 2011.
Earnings before interest, taxes, depreciation and amortization (EBITDA) for the third quarter of 2012 were $29.5 million, compared with $18.7 million for the same period of 2011.
Distributable cash flow (DCF) for the third quarter of 2012 was $15.0 million, compared with $8.6 million for the third quarter of 2011.
EBITDA and DCF are non-GAAP (Generally Accepted Accounting Principles) financial measures, which are explained in greater detail below under "Use of Non-GAAP Financial Measures." Please refer to Financial Reconciliations included in this news release for reconciliations of these non-GAAP financial measures to their most directly comparable GAAP financial measures for the three months ended September 30, 2012 and 2011.
"Our year-over-year improvement reflects the success of our strategy, as we continue to strengthen our business through organic growth and strategic acquisitions," said Eric Slifka, the Partnership's President and Chief Executive Officer. "The combination of our Alliance Energy acquisition, which was completed in the first quarter of this year, our growing crude oil business and our fuel supply and services agreement with Getty Realty helped to drive our year-over-year results for Global Partners. In addition to volume of 1.6 billion gallons of petroleum products – the largest single quarter in our history – we generated record third-quarter net income, EBITDA and distributable cash flow."
"As we expected, our third quarter results did not match the performance we achieved in the second quarter due to the significant increase in gasoline prices from the end of June to the end of September, which adversely affected our margin results."
Slifka continued, "We recently signed a purchase agreement to acquire a 60% ownership interest in Basin Transload LLC, expanding our presence in the Bakken region as a hub for the gathering, storage, transportation and marketing of crude oil and associated petroleum products. We also completed the major rail expansion of our Albany, NY terminal, increasing its capacity to receive up to 160,000 barrels of products per day by rail. In addition, we recently signed an agreement to acquire six stations from Massachusetts-based Mutual Oil Company."
Sales for the third quarter of 2012 increased to $4.6 billion from $3.8 billion for the same period in 2011, driven primarily by the Alliance acquisition as well as the increasing crude oil business. Wholesale segment sales of $3.5 billion were up 11.6% from $3.1 billion in the third quarter of 2011 due to an increase in volume. Sales from the Gasoline Distribution and Station Operations segment more than doubled to $944.3 million compared with $416.3 million for the same period in 2011, reflecting the Alliance acquisition as well as the fuel supply and services agreement with Getty Realty. Commercial segment sales decreased 19.4% to $165.3 million from $205.1 million in the third quarter of 2011.
Wholesale segment volume was 1.2 billion gallons for the third quarter of 2012 compared with 1.1 billion gallons for the third quarter of 2011. Volume in the Gasoline Distribution and Station Operations segment was up 131% to a record 282.5 million gallons in the third quarter of 2012 from 122.1 million gallons in the comparable period of 2011. Commercial segment volume was 80.7 million, compared with 83.2 million gallons in the third quarter of 2011.
Combined gross profit increased to $82.6 million in the third quarter of 2012, compared with $49.3 million in the third quarter of 2011. Total wholesale net product margin grew to $34.9 million in the third quarter of 2012, compared with $25.4 million for the same period in 2011. In the Gasoline Distribution and Station Operations segment, net product margin increased 103% to $52.2 million from $25.7 million in the comparable period of 2011. Commercial segment net product margin increased to $4.8 million in the third quarter of 2012 compared with $4.3 million in the same period of 2011.
Global signed a purchase agreement to acquire a majority ownership interest in Basin Transload, which operates two transloading facilities in North Dakota with a combined rail loading capacity of 160,000 barrels per day. The total purchase price is approximately $80 million. Under the purchase agreement, Global will acquire a 60% ownership interest in Basin Transload, with the remaining 40% split evenly between current owners TGC, L.P. and MBI Holdings, LLC. This transaction is expected to close by year-end.
The Board of Directors of the Partnership's general partner, Global GP LLC, increased the Partnership's quarterly cash distribution to $0.5325 per unit ($2.13 per unit on an annualized basis) on all of its outstanding common units for the period from July 1 through September 30, 2012. The distribution will be paid on November 14, 2012 to unitholders of record as of the close of business November 5, 2012.
Global signed an agreement to acquire six New England gasoline stations from Massachusetts-based Mutual Oil Company. This transaction is expected to close by year-end.
"Strategic acquisitions and organic projects, including the expansion of our rail logistics business and the growth of our gasoline distribution and station operations, position the Partnership to capitalize on the many opportunities in the dynamic and rapidly changing energy market," Slifka said. "Based on our performance through the first nine months of 2012 and current market conditions, we are narrowing our full-year 2012 EBITDA guidance to a range of $115 million to $130 million." The Partnership's outlook is also based on assumptions regarding market conditions, including demand for petroleum products and renewable fuels, weather, credit markets and the forward product pricing curve, which will influence quarterly financial results.
Financial Results Conference Call
Management will review the Partnership's third-quarter 2012 financial results in a teleconference call for analysts and investors today.
Time: 10:00 a.m. ET
Dial-in numbers: (877) 709-8155 (U.S. and Canada)
The call also will be webcast live and archived on Global's website, www.globalp.com.
EBITDA is a non-GAAP financial measure used as a supplemental financial measure by management and external users of Global Partners' consolidated financial statements, such as investors, commercial banks and research analysts, to assess the Partnership's:
compliance with certain financial covenants included in its debt agreements;
financial performance without regard to financing methods, capital structure, income taxes or historical cost basis;
ability to generate cash sufficient to pay interest on its indebtedness and to make distributions to its partners;
operating performance and return on invested capital as compared to those of other companies in the wholesale, marketing, storing and distribution of refined petroleum products, renewable fuels and crude oil, without regard to financing methods and capital structure; and
viability of acquisitions and capital expenditure projects and the overall rates of return of alternative investment opportunities.
EBITDA should not be considered as an alternative to net income, operating income, cash flow from operating activities or any other measure of financial performance or liquidity presented in accordance with GAAP. EBITDA excludes some, but not all, items that affect net income, and this measure may vary among other companies. Therefore, EBITDA may not be comparable to similarly titled measures of other companies.
Distributable Cash Flow
Distributable cash flow is an important non-GAAP financial measure for Global Partners' limited partners since it serves as an indicator of the Partnership's success in providing a cash return on their investment. Distributable cash flow means the Partnership's net income plus depreciation and amortization minus maintenance capital expenditures, as well as adjustments to eliminate items approved by the audit committee of the Board of Directors of the Partnership's general partner that are extraordinary or non-recurring in nature and that would otherwise increase distributable cash flow. Specifically, this financial measure indicates to investors whether or not the Partnership has generated sufficient earnings on a current or historic level that can sustain or support an increase in its quarterly cash distribution. Distributable cash flow is a quantitative standard used by the investment community with respect to publicly traded partnerships. Distributable cash flow should not be considered as an alternative to net income, operating income, cash flow from operations, or any other measure of financial performance presented in accordance with GAAP. In addition, Global Partners' distributable cash flow may not be comparable to distributable cash flow or similarly titled measures of other companies.
Global Partners LP, a publicly traded master limited partnership based in Waltham, Massachusetts, owns, controls or has access to one of the largest terminal networks of refined petroleum products and renewable fuels in the Northeast. Global Partners is a leader in the logistics of transporting crude and other products from the mid-continent region of the U.S. and Canada to the East Coast. The Partnership is one of the largest wholesale distributors of gasoline (including blendstocks such as ethanol and naphtha), distillates (such as home heating oil, diesel and kerosene), residual oil and renewable fuels to wholesalers, retailers and commercial customers in the New England states and New York. In addition, the Partnership has a portfolio of approximately 1,000 gas stations in nine Northeastern states. The Partnership also is a distributor of natural gas. A FORTUNE 500® company, Global Partners trades on the New York Stock Exchange under the ticker symbol "GLP." For additional information, please visit www.globalp.com.
Some of the information contained in this news release may contain forward-looking statements. Forward-looking statements include, without limitation, any statement that may project, indicate or imply future results, events, performance or achievements, and may contain the words "may," "believe," "should," "could," "expect," "anticipate," "plan," "intend," "estimate," "continue," "will likely result," or other similar expressions. In addition, any statement made by Global Partners LP's management concerning future financial performance (including future revenues, earnings or growth rates), ongoing business strategies or prospects and possible actions by Global Partners LP or its subsidiaries are also forward-looking statements.
Although Global Partners LP believes these forward-looking statements are reasonable as and when made, there may be events in the future that Global Partners LP is not able to predict accurately or control, and there can be no assurance that future developments affecting Global Partners LP's business will be those that it anticipates. Estimates for Global Partners LP's future EBITDA are based on a number of assumptions regarding market conditions, including demand for petroleum products and renewable fuels, weather, credit markets and the forward product pricing curve. Therefore, Global Partners LP can give no assurance that its future EBITDA will be as estimated.
For additional information about risks and uncertainties that could cause actual results to differ materially from the expectations Global Partners LP describes in its forward-looking statements, please refer to Global Partners LP's Annual Report on Form 10-K for the year ended December 31, 2011 and subsequent filings the Partnership makes with the Securities and Exchange Commission.
Readers are cautioned not to place undue reliance on the forward-looking statements, which speak only as of the date on which they are made. Global Partners LP expressly disclaims any obligation or undertaking to update forward-looking statements to reflect any change in its expectations or beliefs or any change in events, conditions or circumstances on which any forward-looking statement is based.
CONSOLIDATED STATEMENTS OF INCOME
(In thousands, except per unit data)
Three Months Ended Nine Months Ended
September 30, September 30,
Sales $ 4,617,194 $ 3,765,765 $ 12,508,738 $ 10,728,985
Cost of sales 4,534,574 3,716,486 12,280,124 10,578,885
Gross profit 82,620 49,279 228,614 150,100
Costs and operating expenses:
Selling, general and administrative expenses 24,105 17,166 70,608 57,085
Operating expenses 40,196 19,373 100,692 54,932
Restructuring charges - 1,719 - 1,719
Amortization expense 1,511 1,216 5,373 3,583
Total costs and operating expenses 65,812 39,474 176,673 117,319
Operating income 16,808 9,805 51,941 32,781
Interest expense (9,237 ) (7,947 ) (27,705 ) (23,478 )
Income before income tax expense 7,571 1,858 24,236 9,303
Income tax expense (678 ) - (228 ) -
Net income 6,893 1,858 24,008 9,303
Less: General partner's interest in net income, including
incentive distribution rights (1)(2) (316 ) (142 ) (733 ) (455 )
Limited partners' interest in net income $ 6,577 $ 1,716 $ 23,275 $ 8,848
Basic net income per limited partner unit (3) $ 0.24 $ 0.08 $ 0.89 $ 0.42
Diluted net income per limited partner unit (3) $ 0.24 $ 0.08 $ 0.89 $ 0.41
Basic weighted average limited partner units outstanding 27,311 21,567 26,085 21,188
Diluted weighted average limited partner units outstanding 27,485 21,752 26,258 21,388
(1) Calculations for 2012 include the effect of the March 1, 2012 issuance of 5,850,000 common units in connection with the acquisition of Alliance Energy LLC. As a result, the general partner interest was reduced to 0.83% for the three months ended September 30, 2012 and, based on a weighted average, 0.87% for the nine months ended September 30, 2012.
(2) Calculations for 2011 include the effect of the November 2010 and February 2011 public offerings. As a result, the general partner interest was reduced to 1.06% for the three months ended September 30, 2011 and, based on a weighted average, 1.10% for the nine months ended September 30, 2011.
(3) Under the Partnership's partnership agreement, for any quarterly period, the incentive distribution rights ("IDRs") participate in net income only to the extent of the amount of cash distributions actually declared, thereby excluding the IDRs from participating in the Partnership's undistributed net income or losses. Accordingly, the Partnership's undistributed net income is assumed to be allocated to the limited partners' interest and to the General Partner's general partner interest. Limited partners' interest in net income is divided by the weighted average limited partner units outstanding in computing the net income per limited partner unit.
(In thousands)
Accounts receivable, net 680,438 621,670
Accounts receivable - affiliates 1,277 1,776
Inventories 593,727 664,144
Brokerage margin deposits 30,272 43,935
Fair value of forward fixed price contracts 30,138 15,450
Prepaid expenses and other current assets 62,031 61,561
Total current assets 1,398,956 1,412,864
Property and equipment, net 700,913 408,850
Goodwill 29,123 -
Intangible assets, net 64,623 36,710
Other assets 13,681 10,427
Liabilities and partners' equity
Accounts payable $ 704,459 $ 575,776
Working capital revolving credit facility - current portion 149,081 62,805
Environmental liabilities - current portion 4,373 2,936
Trustee taxes payable 78,977 76,523
Accrued expenses and other current liabilities 59,967 41,307
Obligations on forward fixed price contracts 945 11,707
Total current liabilities 997,802 771,054
Working capital revolving credit facility - less current portion 278,019 526,095
Revolving credit facility 422,000 205,000
Environmental liabilities - less current portion 46,422 27,303
Other long-term liabilities 33,438 24,110
Total liabilities 1,777,681 1,553,562
Partners' equity 429,615 315,289
Total liabilities and partners' equity $ 2,207,296 $ 1,868,851
FINANCIAL RECONCILIATIONS
Reconciliation of net income to EBITDA
Net income $ 6,893 $ 1,858 $ 24,008 $ 9,303
Depreciation and amortization and amortization of deferred financing fees 12,662 8,865 36,769 26,175
Interest expense 9,237 7,947 27,705 23,478
Income tax expense 678 - 228 -
EBITDA $ 29,470 $ 18,670 $ 88,710 $ 58,956
Reconciliation of net cash (used in) provided by operating activities to EBITDA
Net cash (used in) provided by operating activities $ (26,600 ) $ 52,505 $ 189,700 $ (6,779 )
Net changes in operating assets and liabilities and certain non-cash items 46,155 (41,782 ) (128,923 ) 42,257
Reconciliation of net income to distributable cash flow
Amortization of routine bank refinancings (960 ) (932 ) (2,878 ) (2,508 )
Maintenance capital expenditures (3,641 ) (1,193 ) (9,198 ) (2,681 )
Distributable cash flow $ 14,954 $ 8,598 $ 48,701 $ 30,289
Reconciliation of net cash (used in) provided by operating activities to distributable cash flow
Edward J. Faneuil, 781-894-8800


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Condition: New: A brand-new, unused, unopened and undamaged item in original retail packaging.
(6 HINGED DOORS AND 2 DRAWERS AT THE BOTTOM).
HOLDER WITH 3mm THICKNESS METALLIC TOP.
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This scenic view of what was once a glacier covered landscape was taken near the summit of Steens Mountain in southeastern Oregon. Steens Mountain is a 30 mile long (48 km) fault block mountain with an elevation of 9,773 ft (2,977 m). Sometimes mistaken for an entire mountain range the summit of this single mountain stands one mile above the desert below. The U-shaped valleys are caused by glacial erosion. Glaciers, which were present here in eons past, gouged out valleys, resulting in steepening, deepening and widening. The notch on the upper right is a hanging valley, formed by a tributary to the main valley glacier. In 2000 the Steens Mountain Cooperative Management and Protection Act was signed to protect the mountain and surrounding land. Photo taken On August 14, 2006.


text:
Cell | Movie review
Hannah Staunton
With Cell, it doesn't take long to get the gist of what the next hour and 38-minutes entails: within the first few scenes, you recognise the significance of a world where everyone is constantly on their mobile phones. With short, sharp cuts married with ominous music, this film suggests something more eerie, but there isn't much of a plot before the drama unravels, apart from the typical "busy American father can't make it to his son's baseball game" trope. Not long after Clay (John Cusack) ends a phone call with his estranged wife and son, a mysterious interference causes a zombie apocalypse, with everyone who was using their phone violently killing anyone in sight.
Clay escapes to a subway station to find a group of normal people terrifyingly hiding from the zombies – which we soon learn are called "phoners" – on a stationary train. Amongst the chaos strolls in Tom (Samuel L. Jackson, who acts in his usual calm demeanour, despite the current situation). Once again, he and Cusack are paired up for a Stephen King adaptation, following a similar plot to 2007's 1408. Both include cynical authors as the main protagonists whose books and graphic novels begin to bear real-life events.
The two leads make the decision to head out into the devastation, picking up a few stragglers on their way, as Clay is desperate to find his wife and son. There's a pause in action when the small group find a "no cell phone" area: a bar with a few "supposedly normal" people inside. A few drinks later and we see the remains of humanity coming closer together. The classic Hollywood calm before the storm – and it doesn't get much better than this.
Based on King's 2006 novel, Cell, perhaps ahead of its time, suggests the dehumanisation of a society ruled by mobile devices and technology alike. An interesting and thought-provoking concept to explore through literature, however, the film doesn't quite pull through as either.
It's difficult to define this as a horror film when none of the characters appear as terrified or concerned as they should be considering the circumstances. The predictability combined with the half-hearted acting makes Cell as unthreatening and tedious as watching a fifth re-run of Everybody Loves Raymond on a Tuesday morning.
Cell is released in cinemas on 26th August 2016.
Watch the trailer for Cell here:
Kids in Love | Movie review
The Game's Afoot at Madame Tussauds | Theatre review


We now shine the spotlight on a series of modern powder rooms that are magnificent in their own right. Stone is the material of choice in the bathroom below, which makes the Haven Stone Bathtub with Base from Apaiser an ideal choice for the space! Note how details such as a sculptural pendant light add layers of eye-catching design to this interior. Sometimes less is more, and when the powder room is all about the tub, it's not a bad idea to go bold. Next we see Apaiser's Haven Stone Bathtub (this time without the base), and if black isn't your tub color of choice, note that in true Apaiser tradition, the piece is available in a variety of finishes. Here's another modern black bathtub in a grey bathroom, and this time the tub is available through Modern Bathroom Vanities.
Now you're ready to give your small living space a personal touch. Adding some color, texture and interest to your basics will keep your apartment from looking like a furniture showroom. Layer textiles such as pillows and throws on your seating. Choose 20- or 22-inch-square pillows that can double as floor cushions. Add wall canvases and decor in bold tones. Finally, the right area rug will warm up your space while adding color and pattern. Below are some of our favorite accent pieces.


text:
\section{Introduction}

The mechanism for Type II supernovae (SNe) is triggered by the
collapse of massive stars (Burbidge et al. 1957).  As the stellar core
collapses its gravitational energy is released through the emission of
neutrinos (Colgate \& White 1966; Bethe 1990).
A small fraction of these neutrinos are absorbed and the heating
this provides drives the supernova explosion.  Prior to the appearance of
supernova 1987A, this mechanism, though well-developed, had no direct
observational validation.  The observation of neutrinos from SN 1987a at
both the IMB (Bionta et al. 1987) and Kamiokande (Hirata et al. 1987)
detectors provided the first such validation.
Both the $\sim 2$s duration of the
neutrino burst and the number flux of neutrinos agree well with the
predictions of the core-collapse model.  However, with all the reassurances
SN 1987A provides in support of the standard model, it also brings many
new puzzles.  One such unsolved mystery is the lack of detection of the
neutron star formed during the collapse.

Neutron stars formed in type II supernovae are thought to emit radiation as
pulsars, the Crab pulsar (Rickett \& Seiradakis 1982) being the canonical
example.  Even if the pulsar were not directed along our line of sight, its
radiation would heat the surrounding supernova remnant and add to its
bolometric luminosity.  At present, all of the luminosity of SN 1987A can
be accounted for by a radioactive decay model (with corrections for the
``freeze-out'' of the ionization state at late times) consistent with the
production of $0.075M_\odot$ of $^{56}$Ni (Kozma \& Fransson 1998).  The
current lack of evidence of any ``additional'' energy source places a limit
on any emission from the pulsar in SN 1987A at $\sim 10^{37}$erg s$^{-1}$
(Suntzeff et al. 1992, Kozma \& Fransson 1998), a factor of 50 times lower
than that of the Crab pulsar.

Where, then, is the neutron star formed by SN 1987a?  First, it may not be a
pulsar.  SN 1987A's remnant may have a magnetic field which is too weak, or
it may not be spinning sufficiently rapidly, to drive a strong pulsar like
that in the Crab.  Alternatively, the neutron star could obscured by
material which is falling back onto the neutron star.   Even so,
one would expect accretion to provide a sufficient energy source to have
been observed (Woosley, Hartman, \& Pinto 1989). Houck \& Chevalier (1991)
have shown that the ever-present fallback of matter onto the neutron star
(Woosley \& Weaver 1995) would produce a luminosity roughly equal to the
Compton Eddington Luminosity ($L_{\rm Edd,e^-}=4 \times 10^{38}$erg
s$^{-1}$), over an order of magnitude greater than the observed limit
of $10^{37}$erg s$^{-1}$.

It would seem we are forced to accept that the neutron star in SN 1987A
must have collapsed further into a black hole whose accretion luminosity
might be below the observational limits.  Although the duration of the
neutrino burst from 1987A precludes further collapse during the first $\sim
20$ seconds, the neutron star may have collapsed into a black hole at some
later time due either to the accretion of a sufficient fall-back mass and/or
to some change in its equation of state.

The late-time fallback calculated by Woosley \& Weaver (1995) could,
presumably, push the neutron star beyond the critical mass, forcing it to
collapse into a black hole.  However, their calculations estimate typical
fallback masses given the likely SN 1987A progenitors to be $\sim
0.2M_\odot$ and total neutron star remnant gravitational
masses $\lesssim 1.7 M_\odot$.  In fact, because
$0.07M_\odot$ of $^{56}$Ni was certainly ejected
from SN 1987a, the maximum mass of its compact remnant cannot be greater
than this value or it would have accreted all of the $^{56}$Ni production.
If this low-mass neutron star did indeed collapse into a black hole, many
of the current equations of state for dense matter must be incorrect.
Bethe \& Brown (1995) have used the collapse of the neutron star initially
formed in SN 1987A to argue for an equation of state softened by pion
condensates.  Such an exotic equation of state, or something akin to it, is
required to explain such a low stable mass for neutron stars.

The news of the demise of 1987A's neutron star may be premature, however.
In this paper, we study the characteristics of the fallback material to
question the high accretion luminosity derived by Houck \& Chevalier
(1992).  Their result is based on the assumption that the opacity of the
fallback material is comparable to Compton scattering.  We show in this paper
that for conditions appropriate to many fallback scenarios, the actual
opacity can be more than 3-4 orders of magnitude greater than that due to
Compton scattering alone, both in the first few days past explosion and for
many years thereafter.  The appropriate ``Eddington limit'' for the
accreting neutron star is thus over three orders of magnitude lower than that
employed by Houck \& Chevalier (1992) and
would likely remain undetectable in the
lightcurve of SN 1987A for centuries to come.  Indeed, in our simulations
the accreting material drives a photon wind which halts further accretion,
leaving a bare neutron star on timescales of less than a year.  If the
compact remnant of 1987A has not yet formed a strong pulsar, it may
still be a neutron star.

We first calculate the effect of this high opacity on the evolution of an
atmosphere formed by the fallback process.  In \S 2, we discuss the
nature and effects of the fallback which occurs during the supernova
explosion as the shock progresses through the hydrogen envelope,
sending a reverse shock back toward the nascent neutron star and
driving very rapid accretion $\dot{M}>10^4 M_\odot \, {\rm yr^{-1}}$
(Woosley \& Weaver 1995).  The structure of this atmosphere
is derived in \S 2.1 and compared (favorably) to the numerical calculations
in \S2.2.  Most of the atmosphere is accreted via neutrino emission
leaving an atmosphere which cools through photon diffusion.  However,
the opacity of the outer layers of this atmosphere is 3-4 orders
of magnitude higher than that of electron scattering and is
dominated by recombined heavy elements.  These outer ``blanket''
layers are blown off as a wind driven by the flux diffusing from the
inner, hotter (dissociated), and consequently lower-opacity
layers at the Compton Eddington rate(\S 2.3).
This energy flux, derived from the gravitational energy of the
accreting matter, goes primarily into reducing the gravitational binding
energy of the ejected matter and produces a photon flux nearly 3
orders of magnitude below the detection limit.  This process continues
until all the matter in the atmosphere is either accreted or ejected.

Although numerical considerations limit our calculations to only a
small fraction of the duration of this process, the
outcome of the process is not in doubt. In a relatively short time, hours
to weeks after neutrino cooling has shut down, the photon heat flow at
$L_{\rm Edd,e^-}$ at the base of the atmosphere is sufficient to
remove all the mass of the initial atmosphere.
Further accretion could occur at later times (say 10 years after
the supernova event) and understanding its fate and the luminosity
it produces requires a more detailed discussion of line driven
opacity, which we relegate to \S 3.  Here again, we find the
accretion luminosity to be much less than the Compton Eddington
rate.  Line-driven opacity dominates the opacity in all fallback
accretion scenarios, and the resultant luminosities are below
the current detection threshold.  A neutron star may yet
lurk in the ashes of SN 1987A.

\section{Supernova Fallback}

The first calculations of fallback in supernovae occurred soon after the
initial proposal of the neutrino-driven supernova mechanism (Colgate 1971,
Bisnovatyi-Kogan \& Lamzin 1984).  In these calculations, the fallback
results from the loss in pressure support of the expanding ejecta as the
material near the neutron star quickly cooled through neutrino emission.
Lacking pressure support, the matter falls back onto the neutron star
because of the strong gravitational field.  In this mechanism, material
began to fall back onto the neutron star almost immediately after the
launch of the supernova explosion.  Since this time, a new mechanism
causing fallback at later times ($10-10^4$s after the explosion) was
discovered through simulations of 1987A supernova explosions (Shigeyama
et al. 1988; Woosley 1989).  This fallback arises from a
deceleration of the inner layers of the explosion. As the initial
explosion shock encounters the massive envelope of the star, material piles
up behind it, sending a pressure wave (a shock in most simulations) back
toward the center and decelerating the inner layers, driving material back
onto the nascent neutron star (Herant \& Woosley 1994; Woosley \& Weaver
1995).

Figure 1 shows the rate of mass infall from fallback for three different
supernova models calculated from the simulations of Woosley \& Weaver
(1995).  Note that the bulk of the accretion occurs at very rapid infall
rates ($\gtrsim 10^4M_\odot\,$y$^{-1}$).  The fate of fallback material with these
infall rates has been studied in detail (Chevalier 1993, 1996; Houck \&
Chevalier 1992; Brown 1995; Fryer, Benz, \& Herant 1996).  Above a critical
infall rate $\sim 10^{-4}M_\odot\,$y$^{-1}$, this material cools quickly through
neutrino emission and accretes onto the neutron star.  Below this, photon
radiation dominates the cooling of the infalling material and the photon
Eddington limit becomes important.  All of these calculations, however,
assume a constant infall rate which is clearly not appropriate at later
times.

In this section we are interested in the structure of the atmosphere which
remains around the neutron star after neutrino cooling becomes inefficient
and, hence, must accrete through photon cooling.  This material is
comprised of the last bit of fallback onto the neutron star at times when
the infall rate is decreasing rapidly (see Figure 1).  We
derive the structure equations of the atmosphere for a variable infall
rate, ultimately deriving not only the density and temperature profiles but
also the amount of mass that piles on top of the neutron star.  We compare
these semi-analytic results to those of detailed hydrodynamical
simulations.

\subsection{Structure Equations}

The characteristics of an accretion shock for a constant  infall
rate are well known (e.g. Chevalier 1993).  In the  strong shock
limit for a radiation-pressure dominated  ($\gamma = 4/3$) gas,
the pressure ($P_{\rm sh}$), density  ($\rho_{\rm sh}$), and
hence, entropy ($S_{\rm sh}$) at the  shock are given by:
\begin{equation}
P_{\rm sh}=7/6 \rho_{\rm ff} V^2_{\rm ff},
\end{equation}
\begin{equation}
\rho_{\rm sh}=7 \rho_{\rm ff},
\end{equation}
and
\begin{equation}
S_{\rm sh}=P^{3/4}_{\rm sh}/\rho_{\rm sh},
\end{equation}
where $V_{\rm ff}= \sqrt{2 G M_{\rm NS}/R_{\rm
sh}}$ is the free-fall velocity, $\rho_{\rm ff}=\frac{\dot{M}} {4 \pi
R_{\rm sh}^2 V_{\rm ff}}$ is the density of the accreting matter, $G$ is
the gravitational constant, $M_{\rm NS}$ is the neutron star mass, and
$R_{\rm sh}$ is the shock radius.  We parameterize the variable accetion
rate as an exponential decrease in time, $\dot{M} \equiv \dot{M}_0
(t/t_0)^{-\alpha}$.  By setting $t=t_{\rm ff}$, we can write the infall
rate as a function of radius:
\begin{equation}
\dot{M}=\dot{M}_0 \left( \frac{2}{\pi} G^{1/2} M^{1/2}_{\rm NS}
t_0 \right)^{\alpha} R_{\rm sh}^{-3/2 \alpha}.
\end{equation}
Using these equations, we can express the entropy
of the shock as a function of radius:
\begin{equation}\label{eq:entr}
S_{\rm sh}=3.2 \times10^{-18} \dot{M}_0^{-1/4} M_{\rm NS}^{(7-\alpha)/8}
\left( \frac{6.1\times10^3}{t_0} \right)^{\alpha/4}
R_{\rm sh}^{3/8(\alpha-1)}=S_0  R_{\rm sh,6}^{3/8(\alpha-1)}
\end{equation}
where $\dot{M}_0,M_{\rm NS}$, and $t_0$ are all given in cgs units and
$R_{\rm sh,6}$ is the shock radius in units of $10^6$cm.  All previous work
assumed a constant accretion rate ($\alpha=0$) and the resulting atmosphere
was convectively unstable ($\partial S / \partial R = -\frac{3}{8} S_0
R_{sh}^{-11/8} < 0$).

Convection will strive to flatten a negative entropy  profile,
and for the cases where $\alpha < 1$,  the entropy of the
resulting accretion atmosphere (within the shock) is constant.
By assuming  pressure equilibrium for these constant entropy
atmospheres and a neutron star mass much greater  than the mass
of the surrounding atmosphere,  the pressure gradient is given by
(see, for  example, Colgate, Herant, \& Benz 1993):
\begin{equation}\label{eq:equi}
dP/dR=-g\rho=-M_{\rm NS} G \rho /R^2.
\end{equation}
Since the entropy is independent of radius, we can
integrate equation (\ref{eq:equi}) to obtain:
\begin{equation}
P=\left[ \frac{1}{4} M_{\rm NS} G S_{0}^{-1}
(1/R-1/R_{\rm out}) +  P_{\rm out}^{1/4} \right]^4,
\end{equation}
where $R_{\rm out}$ and $P_{\rm out}$ are the radius and pressure of the
outer boundary of the atmosphere.  Since we define the atmosphere as the
material within the accretion shock, $R_{\rm out}$ is equivalent to the
accretion shock radius and $P_{\rm out}$ is the pressure at that radius.
Using this relation for a radiation-dominated gas of pressure $P=1/3 a T^4$
and entropy $S=4/3 a T^3/ \rho$, one can derive the structure equations for
the atmosphere (Colgate, Herant, \& Benz 1993)\footnote{Our derivation
differs from the work of Colgate, Herant, \& Benz (1993) in that we assume
we can neglect the effects of electron-positron pairs.  For the
temperatures involved in this work, this assumption is valid.} including
the density and temperature profiles as well as the atmosphere mass.

For the fallback scenarios we consider, as the last bit of material falls
onto the neutron star, the fallback rate decreases dramatically: $\alpha >
1$ (see Figure 1).  Although convection will not flatten the entropy
profile for these systems, we can still derive the structure equations for
these atmospheres assuming that as the shock moves outward, the entropy
profile is maintained.  Then, again by assuming pressure equilibrium, we
can derive the pressure profile of the atmosphere:
\begin{equation}
P=\left[ \frac{1}{4}M_{\rm NS}G S_{0}^{-1}
\left(R^{-5/8-3\alpha/8}-R_{\rm out}^{-5/8-3\alpha/8}\right)
+ P_{\rm out}^{1/4}\right]^4.
\end{equation}
$R_{\rm out}$ is generally much beyond the regions that we
consider ($R_{\rm out} \approx R_{\rm Bondi-Hoyle}$) and hence it
and the outer pressure can be neglected.  The structure
equations then become:
\begin{equation}\label{eq:pres}
P=\left[\frac{1}{4}M_{\rm NS}G S_{0}^{-1} \right]^4 R^{-5/2-3\alpha/2}= P_0
R_6^{-5/2-3\alpha/2} \; {\rm g \, cm^{-1} \, s^{-2}},
\end{equation}
\begin{equation}\label{eq:temp}
T=\left(\frac{3}{a}\right)^{1/4}\left[\frac{1}{4}M_{\rm NS}
G S_{0}^{-1} \right]  R^{-5/8-3\alpha/8}=T_0
R_6^{-5/8-3\alpha/8}\; {\rm K},
\end{equation}
\begin{equation}\label{eq:dens}
\rho=S_0^{-1}\left[\frac{1}{4}M_{\rm NS}
G S_{0}^{-1} \right]^3  R^{-3/2(1+\alpha)}=\rho_0
R_6^{-3/2(1+\alpha)}\; {\rm g \, cm^{-3}},
\end{equation}
and
\begin{equation}\label{eq:mass}
M_{\rm encl}=\frac{4\pi}{3/2(1-\alpha)}
S_0^{-1}\left[\frac{1} {4}M_{\rm NS}G S_{0}^{-1}\right]^3
\left[R^{3/2(1-\alpha)}_{\rm NS}-
R^{3/2(1-\alpha)}_{\rm max}\right] M_{\odot},
\end{equation}
where $R_{\rm NS}$ is the radius of the neutron star and $R_{6}$ is the
radius in units of $10^6$cm. In next section, we compare this
analytic derivation of the atmosphere's structure to those calculated by
numerical simulation.  These analytic results will give us a basis from
which we can build our understanding of the evolution of these atmospheres.

\subsection{Comparison to Simulations and the Atmosphere Mass}

The structure equations do not uniquely define the atmosphere around the
neutron star. They depend both upon the parameter $\alpha$ and the initial
accretion rate $\dot{M}_0 t_0^{\alpha}$.  Although the uncertainty in
fallback rates allows relative freedom in the choice of $\alpha$, we can
constrain $\dot{M}_0 t_0^{\alpha}$ by insisting that we consider only the
mass of the atmosphere which is not cooled primarily by neutrinos.  The
neutrino cooling of the atmosphere at temperatures $\lesssim 1$ MeV is
dominated by electron capture on protons and can be approximated by (Bethe
1990):
\begin{equation}
L_{\nu}=\int_{r=R_{\rm NS}}^{\infty} 2 \times 10^{18} T^{6}_{\rm MeV}
\rho 4 \pi r^{2} dr \; {\rm erg/s}.
\end{equation}
By setting the neutrino luminosity equal to the Compton Eddington
luminosity ($L_{\rm Edd,e^-} \approx 4 \times 10^{38}$erg s$^{-1}$; the material is still
fully ionized), we estimate the temperature at the base of the atmosphere
to be $\sim 0.4$ MeV\footnote{This critical temperature depends upon
$\alpha$ and for each atmosphere we must calculate the exact critical base
temperature.  However, the strong dependence of the neutrino luminosity on
temperature prevents significant deviation from 0.4 MeV.}.  As the
temperature drops to $\sim 0.2$ MeV, the neutrino luminosity becomes
negligible ($< 10^{-3}L_{Edd,e^-}$).
Choosing a neutrino luminosity, we can then
iteratively derive the temperature at the surface of the neutron star
($T_{\rm NS}$) and the value of the initial accretion rate $\dot{M}_0
t_0^{\alpha}$ for a given $\alpha$.  Using this relation, we can derive
$\rho_0$, $P_0$, and $M_{\rm atm}$.  Hence, the structure of our
photon-cooling atmosphere is uniquely defined by a given $\alpha$.

Our simulations (see the appendix for a description) model both neutrino
emission and absorption as well as photon transport. We set up a range of
infall initial conditions by varying $\alpha$ and allowing the matter to
build an atmosphere around the neutron star. If the material begins to cool
significantly through neutrino emission, it compresses above a critical
density and we accrete it onto the neutron star, removing it from the
atmosphere.  The atmosphere which remains will persist until it can be
accreted via photon emission.  In this section, we will discuss the
structure of this remaining atmosphere.

Figure 2 shows the simulated fallback profiles (for $\alpha=1.5$, $\sim
30$s after the initial fallback) of density, temperature, pressure, and
entropy and the corresponding profiles of these quantities from equations
(\ref{eq:entr}, \ref{eq:pres}-\ref{eq:dens}).  The entropy gives the best
indication of the fit as it does not vary so dramatically with radius.
Figure 3 shows entropy profiles $\sim 30$s after the initial fallback for
a series of atmospheres varying $\alpha$.  Our analytic description of the
atmosphere agrees well with the simulations until the material becomes
sufficiently transparent to photons that the effects of photon diffusion
become important.

At this point in the simulations, the density and temperature structure of
the atmosphere near the base of the neutron star is well defined and we can
determine much of the internal structure of the atmosphere.  Table 1 gives
the derivations of $P_0$, $T_0$, and $\rho_0$ for a range of values for
$\alpha$ which, combined with equations (\ref{eq:pres}-\ref{eq:dens}),
defines the internal structure of the atmosphere.  We will use these
properties in \S 2.3 to discuss the the late-time evolution of the
atmospheres.  Table 1 lists both the analytic estimate of the total
enclosed mass for each atmosphere and that obtained through simulations.
For comparison with the simulations, we list simulation results when
$L_{\nu}=10^5 L_{Edd,e^-}$.  The table also includes the data for a
neutrino luminosity of $L_{Edd,e^-}$ for several values of $\alpha$.  The
accretion timescale ($t_{\rm acc}$),
\begin{equation}
t_{\rm acc}=\frac{G M_{\rm NS} M_{\rm atm}}{r_{\rm NS}
{\rm max} (L_{\nu},L_{Edd,e^-})},
\end{equation}
increases dramatically as the atmosphere cools and can be as high as $\sim
10^6$s when the neutrino luminosity equals the Compton Eddington luminosity.

Most of the material quickly cools and accretes via neutrino emission.
Although the cooling time is proportional to the binding energy, and
hence mass, of the atmosphere, the strong dependence of the neutrino
cooling on the temperature, $\propto T^9$, causes the last bit of
material to take the longest to accrete.  The temperature at the
base of the atmosphere $T_{0} \propto M_{0}^{1/4}$ (eqs. 10,12)
and neutrino cooling, then, is roughly proportional to $M_{0}^{9/4}$.
The mass at which $L_\nu = L_{\rm Edd,e^-}$ defines a sharp boundary between
rapid neutrino cooling above and constant cooling due to photons
below this condition.  Because the neutrino cooled phase is so rapid,
we can estimate the total accretion timescale to be equal
to the accretion timescale at this critical mass.

\subsection{Post-Fallback Evolution}

Returning to our discussion of the neutron star atmosphere, as the
temperature at the base of the atmosphere drops below $\sim 0.4$MeV, the
neutrino cooling becomes negligible.  At this point, the cooling of the
atmosphere depends almost entirely upon the photon heat transport.  If the
dominant opacity source were electron scattering, the luminosity of the
accreting neutron star would roughly equal the usual Compton
Eddington luminosity.  The strong dependence of the opacity on temperature
as the temperature drops below 0.2 keV creates a narrow transition region
from electron-scattering to an opacity dominated by recombined heavy
elements, especially those of the iron group (see Figure 4).
Thus, where the temperature drops below this value, there is a
narrow transition region within which
the Eddington limit falls dramatically.

Figure 5 shows the luminosity profile for a simulation with $\alpha=1.1$ as
a function of time.  The region whose opacity is dominated by
iron\footnote{In the regimes that are most important for our fallback
simulations, the results do not change significantly (30 \%) if the
fallback material were instead composed entirely of oxygen.} forms an
insulating blanket around the atmosphere, limiting its cooling rate.  At
this boundary, photon pressure halts the infall and eventually drives off
the fallback material in a wind. Almost all of the photon energy generated
below this opacity boundary, at the Compton $L_{\rm Edd,e^-}$,
goes into ejecting
mass, doing work against its gravitational binding; in other words, the
accretion flow bifurcates, the outer layers reversing direction and forming
a wind. Because the accretion rate (from larger radii) has fallen nearly to
zero by this time, this wind meets virtually no resistance and is driven
off to ``infinity''.

Figure 6 shows mass-point trajectories for a typical simulations
($\alpha=1.1$).  Much of the matter accretes onto the neutron star, while
the rest is driven off in a wind.  The atmosphere is removed over a cooling
timescale ($\lesssim 10$\,days -- see Table 1).  As the atmosphere expands
in response to the decreased pressure of its diminishing outer layers, the
temperature decreases in deeper layers. These layers then also
recombine and, in turn, are driven off.  This process continues
until the atmosphere either accretes onto the neutron star or is
blown off in the accretion-driven wind.

During this late phase, the observable luminosity of the accreting neutron
star is the fraction of the photon emission which escapes conversion into
kinetic energy in the ``blanket'' -- i.e. the iron-opacity Eddington limit.
Figure 7 shows the photon luminosity at infinity throughout the accretion
process; after about 500 seconds the luminosity is seen to fall by the
expected 3 to 4 orders of magnitude. Any subsequent accretion will continue
to produce a luminosity limited to $\lesssim 10^{-3}$ of the fully-ionized
Compton Eddington limit.

We have thus established that after a very brief interval, essentially none
of the original fallback is left to accrete onto the neutron star at later
times.

\section{Fallback Accretion 10 Years After}

We have shown in \S 2 that any of the ``late-time'' fallback
predicted by Woosley \& Weaver (1995) is removed within a
year of the supernova explosion.  But what about 10 years later
for the case of SN 1987A?  Present calculations of fallback
(e.g. Woosley \& Weaver 1995) can tell us little about very low
rates of accretion. The Compton Eddington accretion limit is only
$10^{-8}M_\odot\,$y$^{-1}$; such a small value is far below the resolution
limit of present-day hydrodynamic calculations (being much less than a single
zone per year in the current fallback simulations).
It is not at all unreasonable to expect that,
while the accretion rate declines rapidly to such small values,
it may remain at such values for periods of up to
many years.

For example, years after the explosion, the decay of $^{56}$Ni in the
supernova may decelerate some of the innermost material to the point
where it becomes once again gravitationally bound to the neutron star.
The energy available from radioactive decay of $^{56}$Ni
to $^{56}$Fe ($9.3\times 10^{16}$erg g$^{-1}$) corresponds to a
velocity increment of $4300$\,km\,s$^{-1}$ and this energy will both
accelerate the outer mass {\it and} decelerate the inner region of the
supernova ejecta.

By extrapolating the results from Woosley \& Weaver (1995), we can
estimate the accretion rate, and hence potential energy from
accretion released from fallback years after the supernova event.
If we take an arbitrary ejecta velocity of the inner
zone from the simulations by Woosley \& Weaver ($\sim 10^{-3} M_\odot$)
to be $100$km s$^{-1}$, after 1000 days its radius is $\sim 10^{15}$\,cm.
At these times, the density of this inner material has decreased to
$\sim 10^{-15}$g\,cm$^{-3}$.  Due to the homologous outflow which
characterizes supernova explosions, the outer material has
expanded at even higher velocities and the density decreases
sharply with radius.  If this inner zone were to decelerate
and become bound to the neutron star, it would accrete roughly
over a free fall time, and the accretion rate ($\dot{M}=
M_{\rm inner \; zone}/t_{\rm free \; fall}$) would be $\sim 10^{-13} M_\odot
{\rm s^{-1}}$.  The potential energy released during this time
yields a luminosity $\sim 3\times 10^{33} {\rm erg s^{-1}}$,
4 orders of magnitude below the detection threshold.

However, we can only make rough estimates given the current
resolution of the simulations and we can not preclude
accretion rates of $\sim 10^{-9} M_\odot {\rm s^{-1}}$.
Such small accretion rates, if all their accretion energy were
converted to photons, would be detectable above the standard decay
light curve of SN 1987A.  In this section, we direct our attention
to the possibility that accretion rates as high as
$\sim 10^{-9} M_\odot {\rm s^{-1}}$ might occur after 10 years.

Since the composition of this late-time fallback will still be
representative of the innermost layers of the ejecta, it will still have an
opacity which is dominated by heavy elements and thus have an Eddington
limit far below the Compton value.  Just as in \S 2 where the
iron opacity converted most of the potential energy of the
accreting material into kinetic energy of an accretion driven
wind, we find that even after 10 years, line-driven opacity
will limit the accretion rate.  However, we now move into regimes
where the SESAME opacity table is no longer accurate and must,
in this  section, discuss the fundamentals of line-driven opacity and
apply their consequences on the emission from this additional
fallback.

\subsection{Line-Driven Opacity}

The increase in mean opacity above the Thomson opacity is a
simple consequence of atomic physics.
The Thomas-Rieche-Kuhn sum rule requires that the sum over all the
oscillator strengths $f_{ij}$ of transitions arising from a given atomic
level equals the number of electrons which participate in giving rise to
the transitions from that level. Most often, this just means that the sum
of all the $f_{ij}$ over all transitions arising from a given level equals
unity.  Since the sum over all of the populations of all levels in an ion must
equal the density of the ion, the sum of all the oscillator
strength in an ion must be equal to the number of bound electrons. How,
then, does having a large number of transitions in the spectrum of an ion
increase the radiation force above that for Thomson scattering?

The answer is that the ``oscillator strength'' of a free electron is spread
out over (nearly) all energies, while the effect of atomic physics is to
concentrate the oscillator strength within a relatively narrow range of
energies, characteristically within a factor of ten of the ground-state
ionization threshold. If this range of energies coincides with that of the
radiation field (so that the Rosseland mean weights it most heavily), the
mean opacity can then be greatly increased.  Further, if the matter and
radiation temperatures are not too dissimilar, the dominant ionization
stages will always occur such that the peak of the radiation field is close to
the typical energy of the most important transitions.

Thus, as soon as the material in the atmosphere begins to recombine, it's
opacity rises sharply. This effect is strengthened at high densities by
pressure broadening.  The strong lines in the spectrum are nearly black
at their cores, and pressure broadening allows each line to absorb
a greater fraction of the spectral bandwidth.  At densities below
which pressure broadening has a significant effect, the opacity can
still be increased by the presence of a velocity gradient in the flow
-- the spread of co-moving frame energies ``seen'' by a photon with
fixed observer-frame energy again allows a single optically thick line
to absorb greater fraction of the total bandwidth.

The effect of pressure broadening is included in the high-density opacities
we have employed from the SESAME code (Magee 1993). At densities below
$\sim10^{-11}$g\,cm$^{-3}$ and temperatures below $\sim 1$eV these opacities
become unreliable due to incompleteness in the atomic physics
calculations. At significantly higher densities, the effects of a velocity
gradient, which are not included in the SESAME data, have already become
important. We therefore take the larger of the results from the SESAME
tables or the ``expansion opacity'' descibed in the following sections.

In the SESAME opacities employed above, for temperatures near 0.1 MeV
the main contribution arises from bound-free transitions and lines
significantly broadened by the high density. Further out in the flow, at
lower temperatures and densities, the ions become more recombined and lines
begin to dominate the opacity. Because of the density of lines in
iron-group elements, the opacity is strongly increased by a velocity
gradient -- the larger the velocity gradient ($\propto t^{-1}$ for
homologous expansion), the greater its opacity and the lower the Eddington
limit. Even for Fe II at nebular temperatures, the Eddington limit in the
inner layers of the ejecta is much reduced below the electron-scattering
value.  Thus, even for very cool material far from the neutron star,
matter is accelerated outward by a luminosity below observational limits.
We argue that any possible accretion rate is thus severly limited.

\subsection{Heating and Momentum Transfer}

There are two ways in which an increased opacity can affect an accretion
flow.  The first is by increasing the heating rate in the high-opacity
material. In the diffusion limit, if the flow is to sustain a given
luminosity it must achieve a sufficient temperature gradient to overcome
the effect of the opacity by heating the inner parts of the high-opacity
region.

As we have shown in \S 2, the entropy profile that develops for these
fallback atmospheres is convectively stable (see Figures 2,3).  As long as
the accretion rate falls off rapidly ($\alpha > 1$), the atmosphere will not
be convectively unstable. However, in the innermost parts of the
high-opacity region, the increased heating rate raises the entropy and
initiates convection.  In our simulations of the initial fallback,
this entropy gain was limited to the inner zone of the high-opacity
region and the resultant convective region would lie in a very
narrow radial space.

Even if the boundary between the high- and low-opacity regions is disrupted
by an instability, beyond the unstable region the radiation field can {\em
still} not be greater than the appropropriate Eddington limit.  The
accretion flow will be stopped by radiation pressure at the {\em largest}
radius at which the radiation force exceeds gravity. As one moves outward
in radius, the flow can be expected to become more uniform and the
radiation field more spherically symmetric, so that at such radii the usual
Eddington argument still applies. Thus, the detailed nature of the flow
near the neutron star seems not to be crucial to our argument.

\subsection{The Eddington Limit for a Line-Dominated Opacity}

An increased opacity can also increase the rate of momentum transport from
the radiation field to the gas.  The spherically-symmetric gas momentum
equation in the co-moving frame is, to $O(v/c)$,
\begin{equation}
\rho{{Dv}\over{Dt}} =
-{{G M(r) \rho}\over{r^2} } - {{\partial p}\over{\partial r}}
+ {1\over c}\int_0^\infty F_\nu \chi_\nu d\nu
\label{eq:radmom}
\end{equation}
The last term is the radiation force per unit volume (or momentum flux per
unit length), where $\chi_\nu$ is the the extinction coefficient (units:
length$^{-1}$).

In the usual treatment of the Eddington limit, the opacity is taken to be
due only to free electrons, $\chi_{e^-} = \rho N_A f
\sigma_e/\overline{A}$, where $f$ is the mean number of free electrons per
ion, $\bar{A}$ is the mean atomic weight of the material, and $\sigma_e$
is the Compton cross section at the flux-weighted mean energy of the
radiation field. Assuming a radially-streaming radiation field with total
flux $F$, we have the radiation force
\begin{equation}
\phi_{e^-} = {{F \rho N_A f \sigma_e}\over{c\overline{A}}}
\end{equation}
or $\phi_{e^-} = 1.3\times 10^{-11} \rho F f/\overline{A}$ in cgs units in
the low-energy (Thomson) limit.

If we set $F=L/4\pi r^2$ and ignore the gas pressure gradient, equation
(\ref{eq:radmom}) gives us the usual Eddington limit
\begin{equation}
L_{\rm Edd,e^{-}} = 1.25\times 10^{38} \left({{M}\over{M_\odot}}\right)
{{\overline{A}}\over{f}}{\rm erg s}^{-1}
\end{equation}

This limit is an absolute upper bound on the photon luminosity generated by
accretion in a steady state, spherically symmetric flow.
Above this limit the radiation force on the free electrons alone
exceeds gravity. Without neutrino cooling, accretion cannot take place at
rates much larger than this value. Even where neutrino cooling is
important, the excess photon luminosity above the Eddington limit will
drive mass outflow, and the photon luminosity at infinity will fall near or
below the limit.  For once-ionized material dominated by iron-goup elements,
as expected for the inner layers of the ejecta, we have $L_{\rm Edd,e^-}
\sim 7\times 10^{39} (M/M_\odot)$erg s$^{-1}$, or about $10^{40}$erg s$^{-1}$.

We have already discussed the increased opacity at high densities
immediately after fallback. In the supernova ejecta at late times the effective
opacity will also be much larger at nebular temperatures
and the Eddington limit will again be correspondingly much lower.
Eastman and Pinto (1993) give an expression for the opacity of a large
number of lines (the ``expansion opacity'') in the Sobolev limit as
\begin{equation}
\chi_\nu = \nu {\beta \over r}
{{\sum_j \int_0^1 (1+Q\mu^2)\left\{ 1 - e^{-\tau_j(\mu)}\right\}d\mu}\over
{\Delta\nu}},
\end{equation}
where for an outflow the sum extends over all lines in the interval
$[\nu,\nu+\Delta\nu]$. $\mu$ is the direction cosine from the radial
direction, and $\tau_j(\mu)$ is the Sobolev optical depth of line
$j$ in the direction $\mu$,
\begin{equation}
\tau_{lu}(\mu) = {h\over{4\pi}}{{n_l B_{lu} - n_u B_{ul}}\over{|\partial \beta/
\partial l|}},
\end{equation}
or, neglecting stimulated emission,
\begin{equation}
\tau_{lu}(\mu) = {{\pi e^2}\over{m_e c}} \nu_{lu}^{-1} f_{lu} n_l
\left|{{\partial \beta}\over{\partial l}}\right|^{-1},
\end{equation}
where $f_{lu}$ is the oscillator strength of the transition and the
directional derivative is
\begin{equation}
{{\partial \beta}\over{\partial l}} = {{\partial \beta}\over{\partial r}}
\left(1+Q\mu^2\right),
\end{equation}
with
\begin{equation}
Q = {{\partial ln\beta}\over{\partial ln\,r}} - 1.
\end{equation}
$Q$ is zero for homologous flow (throughout most of the ejecta in the
supernova), and takes on a value of -3/2 for free infall.

Following the discussion in Eastman \& Pinto (1993), the integral over
angle
\begin{equation}
I_j = \int_0^1 (1+Q\mu^2)\left\{ 1 - e^{-\tau_j(\mu)}\right\}d\mu
\end{equation}
has the limits $(1 + Q/3)$ for $\tau_j(\mu=0)>>1$ and $\tau(1+\tau Q/3)$ for
$\tau_j(\mu=0)<<1$. We will approximate the integral as
\begin{equation}
I_j = \tau^*\left( 1 + {{\tau^*_j Q}\over 3}\right)
\end{equation}
with $\tau^*_j = min(\tau_j(\mu=0),1)$. This gives us the opacity
\begin{equation}
\chi_\nu = \nu {\beta \over r}
{{\sum_j \tau^*\left( 1 + \tau^*_j Q/3\right)}\over{\Delta\nu}}.
\end{equation}

The value of this opacity clearly depends upon knowing the spectral density
of line transitions: the number of lines per unit frequency.  While line
lists are available from which we can determine the spectral density, most
such lists are seriously incomplete, especially in the context of
heavy-element-rich supernova ejecta.  As a purely illustrative example, we
have employed the line list of Kurucz (1991) which lists roughly 171,000
lines of Fe and Co with lower-level energies of $10^5$cm$^{-1}$ or less. The
true value of the opacity will be rather larger due to the incompleteness
of the list.

We have assumed an LTE equation of state at a temperature of 5000K.  Such a
temperature is typical of models for supernova ejecta at times later than a
few hundred days. The matter is assumed to be expanding homologously
($\partial v/\partial r = v/r = 1/t$) and has a density scaled from the
inner zones of hydrodynamic simulations. We have chosen a density range
with $\rho = 10^{-8} - 10^{-6}$g\,cm$^{-3}$
as being typical.  Figure 8 shows the
computed Eddington limits from this model. At present (10 years past
explosion), the Eddington limit is near if not below the observational
limit. Calculations, such as those of Woosley \& Weaver (1995), show a
density near $5\times 10^{-7}$g\,cm$^{-3}$
(scaled to one day) in their innermost
zones, but the density profile from these simulations falls off very
strongly with decreasing radius and the mass resolution of the
innermost zone only $\sim 10^{-3}M_\odot$ which makes it difficult
to determine the density profile. Unfortunately, without far more
detailed simulations of the dynamics of the innermost portion of the
ejecta, a firm prediction of whether the ejecta Eddington limit is
below the observed luminosity is impossible.

If the neutron star is given a significant impulse (``kick'') during the
explosion, it will find itself moving with the flow at the same velocity.
Thus, the material surrounding it will have zero velocity in its own frame.
Because the velocity gradient in homologous expansion is isotropic, the
flow will still be isotropically outward from the neutron star, and the
arguments of this section will remain valid.

\section{The remnant of SN 1987a}
We have shown that virtually all of the late-time fallback of material onto
a nascent neutron star which occurs in most supernova simulations (Woosley
\& Weaver 1995) accretes rapidly onto the neutron star.  However a small
remnant of this material ($\sim 10^{-11}-10^{-9}M_\odot$) remains on the
neutron star and cools due to photon emission.  Due to the high opacity of
recombined iron, the atmosphere emits at a rate much below Compton
Eddington ($\sim 10^{-3}L_{\rm Edd,e^-}$), with most of the photon energy
driving a wind from the neutron star.  The accretion times of the
atmospheres are $\lesssim 0.1$\,yr.  Any further fallback will be limited to
the iron-opacity Eddington accretion rate.  In the case of 1987a, this
means that, although we would not expect to see any luminosity from the
fallback.

If no mechanism drove further fallback onto the neutron star
(e.g. the decay of $^{56}$Ni), then the neutron star remnant of SN
1987A should now have no obscuring atmosphere.  If this did indeed
occur, and if the neutron star is rotating rapidly and has a
strong magnetic field (such as the Crab Pulsar), then we should
observe it as a pulsar.  Only when all of these ``ifs'' are satisfied
must we, as Bethe \& Brown (1995) have suggested, conclude that
the neutron star has indeed collapsed into a black hole.

\acknowledgements We acknowledge the early work of Kaiyou Chen, whose
unpublished research first recognized the importance of the opacity
of recombined iron.  We are grateful to Stan Woosley for access to fallback
models and for many discussions related to fallback and fallback rates.  We
would also like to thank Roger Chevalier, Adam Burrows and Willy Benz for
many useful discussions on this topic.  The work of C. Fryer was supported
by the NSF (AST 94-17161) and by NASA (NAG5 2843 and MIT SC A 292701) and
of P. Pinto by the NSF (CAREER grant AST9501634) and by NASA (NAG\,5-2798).
P. Pinto gratefully acknowledges support from the Research Corporation
though a Cottrell Scholarship.  S. Colgate acknowledges the support
of LDRD funds through DOE and UC.

redpajama_set_name: RedPajamaArXiv


text:
NHL roundup: Sergachev has 2 goals, 2 assists as Lightning beat Caps, 6-3
Mikhail Sergachev gets all his points in a four-goal first period for Tampa Bay.
Tampa Bay's Pierre-Edouard Bellemare, left, and Washington's Matt Irwin fight during the second period Sunday night in Tampa, Fla. Jason Behnken/Associated Press
TAMPA, Fla. — Mikhail Sergachev had two goals and two assists during a four-goal first period, and the Tampa Bay Lightning beat the Washington Capitals 6-3 on Sunday night.
Sergachev is the first NHL defenseman to have a four-point period since Toronto's Morgan Rielly on Oct. 15, 2019, He tied the team record for points in a period.
Nikita Kucherov, Nick Perbix Cole Koepke and Nick Paul also scored for the Lightning, and Andrei Vasilevskiy made 18 saves. Koepke's goal in the third was his first in the NHL, coming in his 13th game.
Steven Stamkos had his goal drought reach 10 straight games, but picked up two assists. The Lightning captain has 987 career points, moved past Dave Keon (986) into 98th place on the NHL list. His 499 assists moved him within one from joining Martin St. Louis (588) as the only Tampa Bay players to reach 500.
Washington star Alex Ovechkin was held without a goal for the third straight game and remains 13 away from tying Gordie Howe (801) for second all time. He received a double minor for high sticking Stamkos during the second.
Conor Sheary, Lars Eller and Garnet Hathaway scored for Washington. Darcy Kuemper, who beat the Lightning 5-1 Friday night, was pulled after allowing four goals on nine shots. Charlie Lindgren came and finished with 24 saves.
RANGERS 4, COYOTES 1: Barclay Goodrow and Adam Fox scored late in the second period as New York beat visiting Arizona.
Chris Kreider and Ryan Carpenter also scored and Igor Shesterkin made 31 saves for the Rangers, who snapped a three-game home losing streak. The Rangers are 13-1-2 in their last 16 games against the Coyotes, dating back to March 2014.
Clayton Keller scored for Arizona, which has lost consecutive games after winning the first three on their season-high 14-game trip. Connor Ingram had 23 saves.
Chris Kreider extended the lead to 3-0 with a power-play goal at 4:39 of the third for his seventh of the season. Mika Zibanejad and Fox had assists, stretching Fox's point streak to six games and giving Zibanejad a point in eight of his last nine.
Keller spoiled Shesterkin's shutout bid with his sixth of the season on the power play at 8:33 of the third, extending his point streak to five game and giving him a team-leading 17 points.
Carpenter made it 4-1 at 11:43 with his first goal since joining the Rangers in the offseason.
STARS 5, FLYERS 1: Joe Pavelski scored a goal and added two assists and Jake Oettinger made 37 saves as Dallas won at Philadelphia.
Matej Blumel, Esa Lindel, Luke Glendening and Jason Robertson all scored for Dallas, which snapped a two-game losing streak in the first game of a three-game Eastern Conference swing.
Travis Konecny scored his sixth goal of the season for Philadelphia, which lost its third game in a row and fifth in its last seven contests. Felix Sandstrom had 26 saves for the Flyers.
SHARKS 3, WILD 2: Alexander Barabanov scored in the fifth round of the shootout and visiting San Jose rallied to beat Minnesota, giving the Sharks consecutive wins for the first time this season.
Steven Lorentz and Nico Sturm scored in regulation and James Reimer made 28 saves for San Jose, which was coming off a 5-4 win at Dallas on Friday night.
Tied at 1 after four shooters apiece, Barbanov's wrist shot from low in the left circle beat Filip Gustavsson between the pads. Nick Bonino also scored in the shootout, the first San Jose has won in four attempts this season.
Kirill Kaprizov scored in the shootout for Minnesota, which got regulation goals from Freddy Gaudreau and Connor Dewar. Gustavsson finished with 35 saves.
Gallery: Soccer all-stars face off in Maine Soccer Coaches Senior Bowl
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CARTER v. BALDWIN COUNTY BD. OF EDUC., 532 So.2d 1017 (Ala.Civ.App. 1988)
LexRoll.com > LexRoll (AL) > Alabama Case Law > CARTER v. BALDWIN COUNTY BD. OF EDUC., 532 So.2d 1017 (Ala.Civ.App. 1988)
532 So.2d 1017
Annie Loree CARTER, et al. v. BALDWIN COUNTY BOARD OF EDUCATION.
Civ. 6415.Court of Civil Appeals of Alabama.
July 13, 1988.Rehearing Denied August 19, 1988.Page 1018
Appeal from the Circuit Court, Baldwin County, Thomas B. Norton, Jr., J.
Gregory B. Stein of Stein and Brewster, Mobile, for appellants.
Norborne C. Stone, Jr. of Stone, Granade, Crosby Blackburn, Bay Minette, for appellee.
BRADLEY, Presiding Judge.
This is an employee termination case.
Employees filed an action against the Baldwin County Board of Education (Board) claiming violations pursuant to the Fair Dismissal Act, ?? 36-26-100 through -108, Code 1975 (1987 Cum.Supp.) (Act). Following an ore tenus proceeding the Circuit Court of Baldwin County ruled in favor of the Board. The employees appeal. We reverse.
The pertinent facts are that the Board, having been advised of the opinion in Garcia v. San Antonio Metropolitan TransitAuthority, 469 U.S. 528, 105 S.Ct. 1005, 83 L.Ed.2d 1016
(1985), which subjected certain Board personnel to the requirements of the Fair Labor Standards Act of 1938, 29 U.S.C.A., ?? 201 through 209 (FLSA), instructed the superintendent to reduce to forty the number of hours worked per week by the employees. The appellants (employees) were all classified, nonprobationary employees of the Board, each having dual duties including cafeteria work, custodial work, teachers' aides, and driving buses.
The trial court made a finding of fact of the "working hours" per week for each of the employees. The "working hours" for employee Carter equaled 44.5 "working hours" per week, for employee Powell equaled 44.5 "working hours" per week (although the correct computation should equal 45), for employee Cruz equaled 44.5 "working hours" per week, for employee Hileman equaled 42.5 "working hours" per week, and for employee Akins equaled 43.5 "working hours" per week. The trial court further stated that the Board reduced the employees' total "working hours." The hours in each case were reduced to forty hours per week so as to comply with the provisions of the FLSA and dispense with the need for overtime compensation. The employees were not given written notice of the reduction, nor were they afforded a hearing.
The employees sought a declaratory judgment, writ of mandamus, and injunctions against the Board, alleging a violation of the Act which required notice and hearing procedures. The employees requested a stay of the proceedings pending a ruling from the Alabama Supreme Court in Ledbetter v.Jackson County Board of Education, 508 So.2d 244 (Ala. 1987). After the ruling in Ledbetter the stay was dissolved and a bench trial was held. The trial court held that the employees had a propertyPage 1019
interest only in a "normal working week" but not in "overtime" hours.
The employees appeal from this decision, contending that the trial court erred in not following the ruling in Ledbetter. We agree.
The Act itself requires notice of a termination or transfer and provides for a hearing if the employee wishes to contest the termination or transfer. In Ledbetter, a cafeteria worker's hours were reduced from thirty-five to thirty hours per week. The dispositive issue in Ledbetter was whether the reduction in hours constituted a termination so as to require the observance of the procedural safeguards of the Act. The court ruled that the employee had a property interest in the "whole" of her employment and any reduction of the "working hours" was a partial termination which triggered the rights to written notice and a hearing under the provisions of the Act.
The dispositive question in the instant case is whether the reduction of "regularly scheduled working hours" in excess of forty per week is considered a partial termination which would require notice and a hearing. We are not cited to any authority nor has our research revealed any authority to answer this issue with the exception of Ledbetter. We read Ledbetter as including any reduction in regularly scheduled hours as a partial termination since these scheduled hours constituted the employee's employment as a whole.
The trial court made a finding of fact that a reduction of the employee's working hours existed. Once this finding was made, the trial court was obligated to assign the case for an administrative hearing in accordance with the provisions of the Fair Dismissal Act. Such a procedure is in keeping with the supreme court's decision in Ledbetter. As stated by the supreme court in Ledbetter:
"By holding that Mrs. Ledbetter was not entitled to a hearing or any review of the board's reduction in her hours of employment, the trial court has allowed the state to deprive her of a property interest given by the statute without due process of law. . . . [W]hen Mrs. Ledbetter followed the procedures of the Fair Dismissal Act to challenge the reduction, she was entitled to present her position before the neutral decision-making body for which the Act provides."
Employees also contend for the first time on appeal that the provisions of the Alabama Litigation Accountability Act, ??12-19-270 through -276, Code 1975 (1987 Cum.Supp.), should be applied to the instant case in that the Board continued to litigate after the ruling in Ledbetter. After a careful review of the record and the language of Ledbetter, we cannot apply the Litigation Accountability Act to the facts of the present case. The existence of factual distinctions between a case being litigated and existing appellate decisions ordinarily relieves a party from the application of the Litigation Accountability Act. Moreover, it is within the province of the courts to interpret statutes and apply appellate opinions. Disagreement between trial courts and appellate courts in the interpretation of statutes and the application of appellate decisions does not necessarily give rise to the sanctions authorized by the Litigation Accountability Act. Thus, we conclude that the trial court properly declined to apply the Litigation Accountability Act to the case at bar.
REVERSED AND REMANDED WITH DIRECTIONS.
HOLMES and INGRAM, JJ., concur.