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Questioning Prepetition Bankruptcy Bans
Debra Felder Chief Practice Officer - Finance, Restructuring, Bankruptcy Litigation
Transactions Sector
Finance Sector
Debra Felder Chief Practice Officer - Finance Restructuring, Bankruptcy Litigation
Debbie Felder, a senior associate in the Washington, D.C., office, is a member of the Restructuring group. Debbie has 19 years of extensive experience in the areas of bankruptcy, insolvency and creditors' rights.
Debbie represents secured and unsecured creditors, investors, lenders, asset purchasers, financial institutions, preference defendants, debtors and other parties in a wide variety of bankruptcy and restructuring matters, as well as in related litigation throughout the United States. In 2020 and 2021, Chambers USA named Debbie an Associate to Watch in the District of Columbia's Bankruptcy/Restructuring category, and clients praised her as "extremely knowledgeable" and providing "very business-minded, practical advice in the most efficient manner possible."
Debbie is currently the lead restructuring associate representing the court-appointed representative for future asbestos personal injury claimants in a complex Chapter 11 pending.
Debbie was the lead restructuring associate representing Toyota in the $30 billion bankruptcy of Takata Corporation. Takata and several of its subsidiaries filed for Chapter 11 bankruptcy in the United States and sought bankruptcy protection in Japan and several other jurisdictions in the aftermath of a worldwide problem involving faulty airbag inflators that led to numerous deaths and the recall of millions of vehicles. Toyota was one of the largest creditors in the proceedings, with claims of over $7 billion. Orrick's work in the Takata bankruptcy and restructuring matter – which included the sale of all of Takata's assets except for the inflator business to the Chinese-owned, Michigan-based Key Safety Systems – was awarded the "2019 Cross Border Turnaround of the Year / Large" by Global M&A Network.
Debbie was also the lead restructuring associate in the representation of the Conflicts Committee of Seadrill Partners (SDLP) in the $14 billion Chapter 11 bankruptcy and associated restructuring proceedings of Seadrill Limited, SDLP's parent company. This bankruptcy and related restructuring was awarded "2019 Cross Border Turnaround of the Year / Mega" by Global M&A Network.
Other recent notable engagements include representing counsel to a borrower in the restructuring of a toll road, representing financial institutions and others in the global Lehman insolvency proceedings, representing a lender in the restructuring of a performing arts center, representing a purchaser in a section 363 bankruptcy sale and representing a defendant in a preference and fraudulent transfer litigation.
Debbie is active in pro bono matters including advising distressed clients in corporate dissolution proceedings pursuant to state statutes. She recently drafted a white paper on "Pay for Success" (PFS) programs – a social services funding mechanism in which non-governmental investors fund social programs and receive returns on their investments from the government only if the programs are successful – which explores the feasibility of using PFS programs to provide civil legal aid to vulnerable populations. She also represents proposed guardians and adoptive parents in connection with guardianship and adoption proceedings involving abused or neglected children in the Superior Court for the District of Columbia.
In addition, Debbie serves as Orrick's Risk Management Counsel where she advises the Firm's management and more than 1,300 Orrick lawyers across the world on issues related to professional responsibility, risk management, and legal issues involving the Firm.
Debbie regularly presents CLE training programs to clients on bankruptcy-related topics, including best practices for creditors.
Prior to joining Orrick, Debbie was an associate at Swidler Berlin LLP. As an undergraduate, she spent four summers as an intern in the Clerk's Office of the United States Supreme Court. During her time at the United States Supreme Court, Debbie researched and wrote a paper on the U.S. Attorneys General, which she presented to the U.S. Solicitor General.


Short Description: Have you ever thought about a career in addiction counseling? Addiction counseling professionals treat individuals who are in need of substance abuse counseling as well as offer peace of mind to the families of persons who are in need of drug addiction counseling. In this program, we will first provide an introduction to psychology. The Introduction to Psychology course takes students through the basic concepts, theories, research methods, and contributions to the understanding of human behavior taking students through the various complexities of human development, the motivations for our thoughts, feelings and behavior as well as the role of sexuality, gender, heredity and genetics as applied to human behavior overall. Students will have the opportunity to analyze various psychological disorders, "normal" behaviors and the basis of the psychology behind learning, memory and experience. Drug and Alcohol Counseling – Level 1 reflects the explosion of information regarding the understanding, identification, and treatment of addictive disorders. It examines the use and abuse of alcohol, tobacco, barbiturates, amphetamines, cocaine, opiates, and hallucinogens, as well as chemicals -- such as aerosols, steroids, and over-the-counter analgesics. Additionally, the course investigates solid strategies for working with clients, the differences between abusers and addicts; drug effects on children, teenagers, and pregnant and nursing women; and children of alcoholics. Drug and Alcohol Counseling Level 2 is a comprehensive course for people who want to work with the chemically dependent and addicted in a variety of treatment settings. This course shows the student how to use the best evidence-based treatments available, including motivational enhancement, cognitive behavioral therapy, skills training, medication and 12 step facilitation. Guiding the student step-by-step through treatment, this course presents state-of-the-art tools, and forms and tests necessary to deliver outstanding treatment and to meet the highest standards demanded by accrediting bodies.
Certification: Upon successful completion of our Drug and Alcohol Counseling Level 1 and Level 2 courses, students may be prepared, in part, to sit for licensing and credentialing exams. Each state has its own regulations, and each state may have additional licensing requirements, so be sure to research your states requirements for employment by visiting your states occupation board.
•	The Growth of New "Addictions"


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How Stalin's Favorite Executioner Vasily Blokhin Personally Killed 7,000 Poles During The Katyn Massacre
By Morgan Dunn | Edited By Kaleena Fraga
As Joseph Stalin's chief executioner of the NKVD, Vasily Blokhin is believed to have ended tens of thousands of lives.
Wikimedia CommonsMajor General Vasily Mikhailovich Blokhin killed tens of thousands of people at Stalin's command.
For decades, citizens of the Soviet Union lived in constant fear of secret police organizations empowered to dole out punishment. Beyond the threat of imprisonment or exile, the dreaded elite executioners posed a terrifying threat. Of these professional mass murderers, Vasily Blokhin boasted the highest body count.
Rising to prominence within the shadowy ranks of the secret police, Blokhin became an instrument of death in Joseph Stalin's numerous purges and in the brutal repression which lay at the foundation of the Soviet empire. Though his killing spree began in the 1920s, Blokhin's most gruesome achievement came during World War II.
Over just 28 days in the spring of 1940, he was personally charged with planning the execution of over 20,000 Polish prisoners of war. Blokhin shot as many as 7,000 prisoners personally, one by one, cementing himself as one of the most prolific individual killers in world history.
This is the chilling story of Vasily Blokhin, the Soviet Union's bloodiest executioner.
Vasily Blokhin's Murky Beginnings
Little is known about Vasily Blokhin's early years. Born in 1895 to peasants in the countryside near the city of Vladimir, he went to work as a shepherd at the age of ten before moving to Moscow to become a bricklayer.
By June 1915, the Russian Empire was deeply entangled in World War I. Blokhin joined the Imperial Russian Army and likely saw combat in Belarus. Eventually, he rose to a senior noncommissioned officer rank.
Wikimedia CommonsRussian troops marching to the front, circa 1917.
In 1917, conditions at home took an unexpected turn. Tsar Nicholas II was toppled in the February Revolution, sending shockwaves throughout the army and the Russian Empire. A provisional government that supported free speech rights and other liberal beliefs led by lawyer Alexander Kerensky was briefly installed in the Romanov Tsar's place.
However, that fall the Bolsheviks, a Communist faction, seized power in St. Petersburg. Their control of the country was nowhere near total, and in order to respond to both peaceful political dissent and violent opposition from the monarchist White movement, the newly-formed government decided that a police force with almost unlimited powers would be needed.
Blokhin, wounded in 1918, returned home to work on his father's farm. He waited to see which faction would emerge as the victor.
In May 1921, Blokhin made his political choice: after joining the Communist Party, he was immediately appointed to the ranks of the already-feared "All-Russian Extraordinary Commission," better known as the Cheka — the first of many iterations of the secret police in the Soviet Union.
Blokhin's Role In Cheka, The Secret Police
Wikimedia CommonsMarshal Mikhail Tukhachevsky (bottom right), was one of Blokhin's highest-profile victims during the Great Purge of the 1930s.
Chekists were entrusted with ensuring discipline in the new Red Army, protecting shipments of food and supplies, and disrupting opposing political groups through violence and infiltration.
Blokhin took an active part in the Cheka mission, quickly gaining the attention of his superiors. He steadily climbed the ranks and in 1926 was appointed "Commissioner of the Special Department of the OGPU" — in other words, chief executioner.
His ascendancy dovetailed with that of Joseph Stalin, who became increasingly powerful in the 1920s, as well as the Union of Soviet Socialist Republics (USSR) which came into being between 1917 and 1922.
Blokhin was tasked with carrying out and supervising executions in the Lubyanka building in Moscow, which held prisoners on its top floor with Cheka offices below.
Wikimedia CommonsThe Lubyanka was a symbol of dread for Soviet citizens. Here, Blokhin and his fellow executioners killed thousands.
The preferred method of execution at the Lubyanka was crude. The condemned was ordered to kneel. Then, the executioner fired a bullet into the back of their skull. The body was then moved to a crematorium of Blokhin's own design, inaugurated in October 1927 to commemorate the Bolshevik Revolution's tenth anniversary.
During Stalin's Great Purge which took place between 1936 and 1938, some 750,000 people were executed as dissenters. Blokhin personally shot the victims of the great show trials, as well as several of his fellow executioners when they fell under suspicion.
Blokhin's abilities won him the personal favor of Stalin. When bureaucrats accused Blokhin of conspiring against the state in 1939, Stalin refused to sign a warrant for his execution, calling the "black work" Blokhin did invaluable.
The purges had largely ended by the time Nazi Germany and the USSR cooperatively invaded Poland in September 1939. But for the Soviets, angered by their defeat in the Polish-Soviet War of 1919-20 and eager to smash any resistance to their power in Eastern Europe, the invasion was only the beginning.
The instrument of their violent goals was to be the Cheka, now renamed the NKVD.
The Massacre At Katyn
The capture of eastern Poland delivered thousands of Polish soldiers, officers, officials, and intellectuals to the Red Army — all of whom were distrusted by Lavrentiy Beria, the new head of the NKVD.
Beria had come to power after toppling his predecessor Nikolai Yezhov, who may have been personally shot by Vasily Blokhin. To Beria, every Polish officer was a potential threat to the Soviets, and the solution he proposed to Stalin was as brutal as it was simple: execute every officer who couldn't be convinced to join them. Stalin quickly green-lit the bloody plan.
Universal History Archive/Getty Images
Photo from the 1943 exhumation of a mass grave of Polish officers.
In the spring of 1940, over 22,000 soldiers, writers, bureaucrats, police officers, and politicians were shipped to sites in western Russia, including the Katyn forest near the city of Smolensk, for execution.
In charge of the organization, Blokhin and two colleagues traveled to the outskirts of the town of Ostashkov to take part, outfitting a soundproof hut and setting themselves a quota of 300 executions a night.
Victims would first be taken to an antechamber of the hut that had been painted red and dubbed "the Lenin room" for identification. Then, they were handcuffed and taken to the execution room where Blokhin was waiting with his gun. On the very first night of the massacre, Blokhin and his colleagues shot 343 victims, a grisly accomplishment for three men working only with pistols.
Years later, ex-NKVD officer Dmitry Tokarev described how Blokhin, who'd brought a suitcase of reliable German Walther PP pistols to carry out his task instead of the standard-issue Soviet TT-30 which he found unreliable. He dressed in a butcher's leather apron with arm-length gloves, a long leather coat, and a leather cap to protect his uniform from bloodstains.
But perhaps the eeriest thing about Blokhin was his calm, cheery demeanor. Top Soviet executioners lived under a kind of mental torture themselves. They rarely saw their families and often drowned the trauma of killing with alcohol.
Blokhin, by contrast, was a strict teetotaller, preferring hot sweet tea even on the killing fields of Katyn, and his cheerful attitude in all situations and settings made him universally popular among his fellow black work operatives.
Wikimedia CommonsThe bound hands of one of the 22,000 victims of the Katyn massacre.
"An experienced executioner shoots in the neck, holding the barrel obliquely upwards," Blokhin stated matter-of-factly. "Then there is a chance that the bullet will come out through the eye or mouth. If you kill 250 people a day, then cleaning the premises becomes a serious problem."
At the end of 28 days, all but a few hundred of the captives had been shot and buried in mass graves. Blokhin himself claimed to have personally shot as many as 7,000. As a reward, he received a small raise, a gramophone, and the Order of the Red Banner, one of the highest military awards in the USSR.
Before taking a month's vacation, he and his fellow executioners held a banquet behind a train station just down the road from the site where they'd carried out their brutal task.
The Nazis — no strangers to horrifying violence themselves — uncovered the mass graves from the Katyn massacre when Germany invaded the Soviet Union in late 1941.
An examination of exhumed soldiers in 1943.
Rumors of a massacre near Smolensk led German troops to the graves in Katyn, and Nazi Minister of Propaganda Joseph Goebbels knew he'd uncovered something he could use against the Soviets. In April 1943, he organized a media circus around the exhumation of the bodies, including a Red Cross delegation, a forensics team, radio coverage, and even journalists from occupied nations, who were released from detention to report the discovery.
However, the Soviets claimed that the Germans were responsible for the mass killings at Katyn. Soviets pointed to the fact that the victims in the mass graves had been shot with German guns to support their story. Other Allied leaders were somewhat skeptical of this narrative, but to avoid rocking the boat with Stalin they accepted the Soviet version of events.
The Most Prolific Killer In History?
Wikimedia CommonsThe ashes of countless people killed by Blokhin are buried in this common grave, just a short walk from Blokhin's own in Moscow's Donskoye Cemetery.
Even among the notoriously violent NKVD members of Stalin's day, Blokhin stands out, with as many as 20,000 deaths credited to him. Over the course of a quarter of a century, he'd personally shot notable army generals, artists, and old revolutionaries.
Because of the secrecy of most Soviet executions, his true death toll may never be known — but Blokhin certainly has one of the highest victim counts for any executioner in history. According to his claim, he killed twice as many as runner-up Peter Maggo — another Soviet executioner who's believed to have killed more than 10,000 people.
The deaths of Stalin and Beria in 1953 signaled Blokhin's downfall. Stripped of his rank and honors, he sank into alcoholism before dying by suicide in 1955. His name was forgotten by much of the world until 2010 when the Russian government finally admitted guilt in the Katyn massacre.
That same year, Blokhin was named as the Guinness World Record holder for the most prolific executioner as his role in the Katyn massacre had finally come to light.
Even in death, Blokhin can't escape his brutal past. Just a short walk away from his grave in Moscow's Donskoye Cemetery lies Common Grave Number 1. This morbid pit was the NKVD's preferred dumping ground for the cremated remains of Blokhin's victims after passing through his special crematorium.
After learning the terrifying truth behind the Soviet Union's bloodiest killer, take a closer look at what life was like inside the Gulag in these tragic photos. Then, explore Russia's forbidden closed cities that were built to hide the Soviet nuclear program.
Morgan Dunn
Morgan Dunn is a freelance writer who holds a bachelor's degree in fine art and art history from Goldsmiths, University of London. His areas of interest include the Soviet Union, China, and the far-reaching effects of colonialism.
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redpajama_set_name: RedPajamaCommonCrawl


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Medical Assistance to Self-settled Refugees (Tropical Institute Antwerp, 1998)
3. The refugee-crisis: between self-reliance and pragmatic assistance
Settlement patterns of refugees
The number and distribution of refugees*
'Integration' of urban refugees
Rural refugees: between 'integration' and 'segregation'
'Refugees live in camps'
One third of the refugees, mainly Mandingo, settled in the major urban centres: N'ZkorGuu and Macenta. The Mandingo, whether 'refugees', 'returnees' or 'citizens', dominated trade in the cities. Their arrival from Liberia transformed the cities of the Forest Region. Since 1990, the number of cars in the cities at least tripled or quadrupled. The refugees brought many of these cars, but often had to sell them when their resource basis dwindled.
These refugees were integrated in the economic life of the cities. The sudden increase of Mandingo further marginalised the forest tribes - Mano, KpellLoma and Kissi - economically. It also exacerbated pre-existing ethnic tensions. The forest tribes were loyal to NPFL that had persecuted the Mandingo in Liberia. In June 1991, ethnic tensions between Kpellnd Mandingo escalated in N'Zkornd resulted in clashes which caused some 200 deaths. Also in Macenta, tensions between the Mandingo, locally known as Tomamania, and the Loma increased. Several hundreds of people were killed. At the same time, political liberalisation made the forest tribes more vocal and their domination of certain city councils, namely in N'Zkorstrengthened their political position.
In the cities, there were serious problems with over-registration of refugees. Many merchants and local authorities acquired ration cards, in certain cases for many groups of 50 beneficiaries. The urban Mandingo refugees were the most outspoken and politically aware section of the refugee population. When food distributions became irregular, the urban refugees staged protests at the UNHCR offices. When food aid only trickled in, as was the case throughout 1995, there was political pressure to favour distributions to the urban refugees to avoid tensions in the cities. Most urban refugees managed relatively well, at least economically. Still, they lost a lot through their forced migration to Guinea. Many Mandingo were killed in Liberia, and part of their property was looted or destroyed. Some became destitute, lost their social network and became pauperised urban dwellers.


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Home Hugh Morton Collection of Photographs and Films "Ghost Town in the Sky," Maggie Valley
"Ghost Town in the Sky," Maggie Valley
Entrance to "Ghost Town in the Sky" amusement park in Maggie Valley, NC.  Incline railway in background.
Title "Ghost Town in the Sky" Maggie Valley
Description Entrance to "Ghost Town in the Sky" amusement park in Maggie Valley, NC. Incline railway in background.
filename P081_PTCS4_006164.tif
Date 1960s-early 1970s
Search by Decade 1960-1969
Subject (tgm) Amusement parks
Railroad cars
Subject Geographic Ghost Town in the Sky (Maggie Valley, N.C.)
Maggie Valley (N.C.)
Haywood County (N.C.)
Subseries 1.1.38
Creator Morton, Hugh M.
Resource Type Image
Form General Photographs
Form Specific Color sheet film transparency
Size of Original 4 x 5 in. (101.6 x 127 mm)
Collection in Repository Hugh Morton Photographs and Films (P081); Finding Aid: https://finding-aids.lib.unc.edu/P0081/
Local Identifier P081
Digital Collection Hugh Morton Collection of Photographs and Films
Repository University of North Carolina at Chapel Hill, Wilson Library, North Carolina Collection Photographic Archives
Usage Rights Copyright North Carolina Collection, University of North Carolina at Chapel Hill Library. The images in this collection are made available for use in research, private study, and teaching. Prior permission from the North Carolina Collection is required for any commercial use.
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Photo taken of the damage to a section of Highway 11, and shared to social media on Nov. 15 by Abbotsford Police.
Highway 11 reopens between Abbotsford and Mission
Busy transit route has been closed since Nov. 15; single lane in both directions now open
Patrick Penner
Dec. 6, 2021 10:35 a.m.
Highway 11, the busy transit route connecting Mission to Abbotsford, has finally been re-opened.
The highway was opened on Dec. 6 and can now be used by passenger vehicles, municipal service vehicles and emergency service vehicles, according to the Ministry of Transportation and Infrastructure.
A single lane in each direction in the southbound lanes between Hazelwood Avenue and Clayburn Road are being utilized, while the northbound lanes remain closed as further repairs are done, according to the ministry, noting there is no left turn onto Highway 11 from Valley Road.
Delays are still expected.
The busy transit route has been cut off in both directions between Hazelwood Avenue and Townshipline Road since Nov. 15, after the flooding caused extensive damage that required extensive assessments.
Traffic was re-routed to Downes Road, but congestion became a problem as there was a no-left turn on Gladwin Road due to construction.
Abbotsford's rural, single-lane back roads became clogged on a daily basis, with commercial-transport vehicles and commuters attempting to navigate roads unsuitable for the heavy traffic.
The restrictions on travel along Highway 7 between Mission and Hope have also been officially been lifted.
In a Monday (Dec. 6) evening news release, the Ministry of Transportation and Infrastructure announced travellers can use Highway 7 for daily activities once more, including commuting to work, driving students to school or attending appointments.
The ministry advises motorists to continue to expect congestion with the restrictions being lifted.
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Tired of searching the internet for a collection of recipes to serve at your holiday dinner this year? Look no further! I have compiled the perfect Thanksgiving menu for you, all in one place.
Thanksgiving is literally right around the corner. So, let's take care of the biggest item on the menu — turkey. And boy do I have the easiest, best and juiciest roast turkey ever for you! It cooks faster than using a traditional method and it requires NO brining! Winning!
Thanksgiving is not the same without thick and delicious, classic homemade turkey gravy made using leftover drippings and homemade turkey stock. The leftover drippings come from the turkey recipe above and the homemade turkey stock will require the turkey neck and giblets. There is seriously no need for powdered gravy if you are already making a roast turkey dinner!!
Finally, a recipe that you can make days before Thanksgiving! Easy make-ahead cranberry sauce. You literally have no excuse to serve cranberry sauce out of a can when it only takes 15 minutes and 4 ingredients to make. This recipe will just take the stress out of the holidays!
I love combining sweet and savory flavours, and this stuffing is the perfect example of why it works so well. Cranberry walnut bread paired with sautéed apples, onions, and rosemary is exactly what your holiday table needs! Hello cranberry walnut apple stuffing!
This delicious and easy roasted butternut squash soup brings all the taste of the holidays in one spoon. Rosemary, sage and thyme, need I say more? This soup is just all around comfort food… without the guilt! That's right, this soup is super healthy. It's vegan, gluten-free and whole 3o compliant. Which also means that there is no cream, no milk, no butter!! Yet this soup has a very creamy and smooth texture from the butternut squash. You really can't get any healthier than that!
A handful of ingredients and a few simple steps makes creamy cauliflower and garlic soup one of the easiest and tastiest soups ever. Carmelized cauliflower, garlic and onion in this soup not only enhances the flavour, but it also gives the soup a gorgeous, golden colour.
Another killer butternut squash and apple soup with toasted croutons to share. It's got sweetness from apple and carrots, a kick from onions and curry powder, and it's just all around comfort food… also without the guilt!
Have an apple today and keep the doctor away with this fresh, fall favourite — apple walnut salad with homemade balsamic vinaigrette. Throw together crisp apples, crunchy walnuts, and sweet cranberries to beautifully decorate your dinner table with a taste of the holidays.
This roasted brussels sprouts salad with creamy potatoes, crispy string beans, and dijon vinaigrette makes for a delicious whole30 compliant and vegan meal this season!
Winter kale salad with apples, goat cheese and spiced pecans tossed in apple cider vinaigrette can be on your holiday table from start to finish in under 10 minutes. Take that, Thanksgiving stress!
Pick one item from the following categories (or more, depending on how big your party is).
Say good-bye to lumpy, bland and dry mashed potatoes this year!! I introduce the best and creamiest mashed potatoes. These potatoes are so velvety and so smooth. Your holiday table has never looked better! Seriously. You can also prepare these mashed potatoes the day before. Just make it without the butter, store in the refrigerator, and reheat the next day adding in the butter.
Crispy on the outside and soft and tender on the inside, these flavourful, herb-roasted sweet potatoes are the perfect side dish on your holiday table. It's another one of my go-to's since it is super easy, taking only about 10 minutes of prep time. Your oven basically does all the work.
Hasselback potatoes are perfectly crispy on the outside and tender and buttery on the inside. The ah-mazing garlic herb butter is basically just that, butter infused with garlic and rosemary. You can also serve it with a sprinkle of Parmesan cheese on top for maximum flavour.
One of my favourite dishes to serve on Thanksgiving are tender and caramelized, easy roasted brussels sprouts tossed in balsamic vinegar and honey. Now that's a mouthful of yum! It is also another super easy dish that takes only 10 minutes to prep and then you let the oven do the rest of the work while you can relax and kick your feet up!
If you are hosting the big event this year, this recipe has just made your life a little easier. The key to stress-free holiday entertaining is to prepare some dishes that take no time and no effort to make. I am talking about dishes that take under 30-minutes to make or dishes that can be made in one pan. How about both? That's where one-pan maple roasted brussels sprouts and butternut squash comes in play.
Here's another super easy, one-pan vegetable dish to make your holiday prep so much easier. I am talking about sweet and flavourful easy garlic and herb roasted carrots. Plus, these veggies are roasted which brings out their flavour and intensifies it, making them sweeter and more flavourful. Carrots will never taste the same!
Imagine having a nice big serving of mashed potatoes but with a quarter of the calories. Now you can with creamy garlic mashed cauliflower! That's right, cauliflower. You might just fool your guests into thinking this is mashed potatoes, yet saving them tons of calories!
Why settle for steamed corn when it is too cold to grill your corn on the cob? You can get that perfect balance of perfectly juicy inside and charred on the outside, without a grill. It's called buttery, oven-roasted corn on the cob with garlic butter! This corn turns out perfect every time. The garlic butter gives it a perfect subtle flavour and keep the corn juicy. But for extra juiciness, add even more butter on top. YUM!
Creamy, cheesy, classic mac and cheese with a crunchy topping always finds a way to my holiday table. Yes, I know this isn't particularly the most healthy dish, but at least it is made from scratch. If you have grown accustomed to those boxes of mac and cheese, you don't know what you are missing!! Throw away that orange, powdered cheese and try fresh, grated cheeses. Trust me, once you try the real stuff, you will never go back!!
These garlic cheddar biscuits are packed with flavour and can be prepped and in the oven in less than 15 minutes! They also make a great leftover breakfast so go ahead and make a big batch of this stuff, you won't regret it!
These fluffy, quick and easy dinner rolls will melt in your mouth, making them the only bread recipe you'll need to complement any meal! And don't run away at the thought of baking bread. It may have been that putting freshly baked bread on the table used to be something that only our grandmothers used to do. Nowadays, we feel like we just don't have the time. But guess what? What used to take hours to make can now be put on the table in less than an hour, while you preparing the rest of the dishes for your holiday dinner! It can't get any easier!!
Easy cornbread muffins just made your holiday dinner a whole lot easier and tastier! They take literally 10 minutes to prepare and 20 minutes to bake. It's so easy that even the kids can help you make this! So add these moist and fluffy muffins (made with cornmeal, cooked corn kernels, and sweetened with honey) to your holiday table.
Classic pecan pie is an essential Thanksgiving dessert. Try this easy to follow recipe to get that flaky crust, smooth custard filling and pecan topping. For such a complicated looking pie, it is actually embarrassingly easy to make. You can also make this a day in advance or at least a few hours before your Thanksgiving dinner to allow the filling to set.
Give traditional pecan pie a twist this holiday season by using finely chopped pecans to create a smooth topping on this chopped pecan pie! This pie is also ridiculously easy to make. You prepare the pie crust, prepare the pie filling, put them together and bake. The entire preparation process takes less than 20 minutes which gives you time to do the other hundred items on your to do list during the busy holiday season. So basically it's time to change things up this Thanksgiving and say good bye to store-bought pies and hello to irresistible homemade!
Individual apple crisp are served in ramekins so that you and your guests can enjoy single-sized servings meaning you will get the crunchy corners of crumble all to yourselves! Add a big scoop of ice cream on top for maximum happiness.
Celebrate fall this year with think and dense, yet surprisingly light, pumpkin pie bundt cake with cream cheese glaze. Can you think of a more perfect pair? The beauty of this cake is that it is thick and dense, but also surprisingly light! It's warm from the mixture of pumpkin and pumpkin pie spice blend, and absolutely benefits from a hearty drizzle of cream cheese glaze. Can you think of a more perfect pair?!
Move over pumpkin, there is a new loaf in town! Butternut squash "pumpkin" bread is moist and flavourful, and brings the pumpkin spice season to your home. This loaf can be made with butternut squash puree or pumpkin puree.
Warm, fresh-from-the-oven, soft and chewy white chocolate cranberry walnut cookies make the perfect holiday treat. They are beyond simple to prepare, and even easier to watch disappear! You've got sweetness from the white chocolate, a slightly crunch from the walnuts, and the perfect tangy bite from the dried cranberries. I don't know anyone who doesn't love these.
What is better than classic, soft and chewy peanut butter cookies? Umm… not a whole lot comes to mind. Get ready to fall in love with a cookie. A puffy, thick circular pile of goodness. It takes 10 minutes to prepare (basically while the oven is preheating anyways) and 8 minutes to bake. Yup, 8 minutes. When you are craving a delicious treat, nothing else is on your mind than taking that first bite. The amount of time it takes really matters!!
Soft, buttery, melt-in-your mouth jam-filled thumbprint cookies with almond glaze are the cutest, festive treat to make. Plus, it comes together with just a handful of ingredients and less than 20 minutes of prep time.
Tired of searching for a collection of recipes to serve at your holiday dinner this year? Look no further! Here's the perfect Thanksgiving menu for you, all in one place.
Creamy mashed potato and creamy garlic mashed cauliflower reheat well on the stove or microwave.
Garlic cheddar biscuits and easy cornbread muffins reheat well in the microwave or oven.
Classic baked macaroni and cheese reheats well in the oven.
Classic old fashioned pecan pie, chopped pecan pie, pumpkin pie bundt cake with cream cheese glaze, butternut squash "pumpkin" bread, soft and chewy white chocolate cranberry walnut cookies, soft and chewy peanut butter cookies, and jam-filled thumbprint cookies with almond glaze can be stored at room temperature overnight.
Roast turkey and classic homemade turkey gravy.
Cranberry walnut apple stuffing is best served from the oven.
Hasselback potatoes and herb-roasted sweet potatoes are best and crispiest when served from the oven.
Easy roasted brussels sprouts, maple roasted brussels sprouts and butternut squash, easy garlic and herb roasted carrots, and oven-roasted corn on the cob with garlic butter are best served from the oven.
Quick and easy dinner rolls are best served from the oven.
Individual apple crisp is best served from the oven.
This is such a feast! I can't believe you can pull it out by yourself! We have 8 people and still take all day to finish cooking dinner! I really love pecan pie, but am embarrassed to say that I have never made a pecan pie. And, I have never made pie crust and always got the store bought pie crusts. Since you make it look easy to make pie crust, I may just have to try this. Thanking you for shared this post!
What a great looking thanksgiving collection, we don't celebrate Thanksgiving here in the UK, but these recipes are perfect for Christmas too!
What a terrific list of Thanksgiving meals. Thanks for sharing them.
Wow I LOVE this menu. It's so rich and so FESTIVE! I wish I get the invite to your party with all these delicious food served. I honestly drooling over avery one of these recipe. Can't decide what to try first!
I love that you laid out a whole menu! We're hosting this year so I'll definitely be referring back to this for the dishes I'm responsible for.
What a great plan! You just saved me massive amounts of time AND made sure I don't forget anything!
So glad to help!! Hope you and your loved ones have a Happy Thanksgiving!
I'm not gonna lie, I am ALL OVER those dinner rolls!
I lOVE this post! I'm sending this to my daughter and saving for me. This is very helpful so thank you for doing this. And as always, your pictures are gorgeous:) Happy Thanksgiving.
Fantastic collection of Thanksgiving meals! I will pick most of my holiday dishes from here, so useful!
Ahhh. A refreshing list of everything I need to cook. Sans hunting down each recipe individually. Thanks for the inspiration!
This is a wonderful menu!! Everything goes together so well! I'm going to give the skillet rolls a try!
Thanks for sharing this! I will be saving this for next week when I start planning my menu.
What a glorious roundup of Thanksgiving or holiday fair!! Everything looks delicious and that pecan pie looks out of this world. The only problem I see is which recipe to start with!


text:
Franz Keller (* 19 de mayo de 1913 - †  12 de septiembre de 1991) fue un psicólogo católico, periodista marxista y consultor conyugal y de pareja, miembro del Partido Socialista Suizo.

Vida

Keller estudió la psicología, la filosofía y la historia de la literatura en las universidades de Zúrich, Berna, Múnich, Viena y París. En 1938 comenzó a trabajar como psicólogo y grafólogo en Ascona y Zúrich. Durante la década de 1950 estuvo varias veces en Alemania Oriental, donde conoció su segunda esposa, Marianne, una cantante de ópera. Fue miembro de la Asociación Suiza - Unión Soviética, de la Asociación Suiza - República Democrática Alemana, del Movimiento Suizo por la Paz y del Consejo Mundial de la Paz y publicó regularmente artículos en las revistas suizas Profil, Zeitdienst y Vorwärts (órgano de la izquierda política suiza).

Obra

La obra de Keller se caracteriza por reunir catolicismo y marxismo, dos polos ideológicos aparentemente contradictorios. Entre sus obras las más importantes se encuentran:
 Psychologische Zeitlupe: Die jüngste Vergangenheit im Vergrößerungsglas eines Psychologen.  ("La cámara lenta psicológica: el pasado reciente bajo la lupa de un psicólogo.") 1941
 Wie sich finden? ("¿Cómo encontrarse a sí mismo?") 1944
 Vom seelischen Gleichgewicht. ("Sobre el equilibrio del alma.") 1945
 Wie bereitet man eine Heirat vor? ("¿Cómo preparar un matrimonio?") 1948
 Frei werden von Hemmungen. ("Vencer las inhibiciones.") 1954
 Die moderne Ehe. ("El matrimonio moderno.") 1954
 Das Schicksal der abendländischen Kultur. ("El destino de la cultura occidental.") Manuscrito inédito de 70 páginas.

Otra fuente

 Verena Keller: Silvester in der Milchbar: Erinnerungen einer Schweizer Schauspielerin an die DDR und ein großes Abenteuer. Berlín: Vergangenheitsverlag, 2012. ISBN 978-3864080623

Enlaces externos

 Keller, Franz (1913 - 1991) en los HelveticArchives de la Biblioteca Nacional Suiza

Referencias

Católicos de Suiza
Activistas de Suiza
Psicólogos de Suiza
Socialistas de Suiza
Grafólogos
Nacidos en Soleura

redpajama_set_name: RedPajamaWikipedia


Commuting to work might have surpassed baseball as America's pastime. It's favorite pastime? Not so much, and the amount of hours we spend everyday trekking to and from work adds to up to some truly astronomical numbers.
According to the Bureau of Transportation Statistics, if you live in New York and commute to work then you are one of a whopping 9,024,559 workers who do this every day, compared to New Jersey's 4,166,286. And according to the New York Post, the average round-trip commute time for NYC goers is 57.92 minutes, fourth longest just behind DC (60.42 minutes), San Francisco (59.2 minutes) and Chicago (58.5 minutes). These are staggering numbers.
With employees taking all of this wasted time out of their busy day to travel, more and more businesses are choosing to operate out of shared workspaces due to their close proximity to residential areas and many convenient locations. Employers understand the simple fact that less travel time equals more work time which equals more dollars in their pockets.
From the employee's standpoint, it's just as lucrative. All that time spent on planes, trains and automobiles add up to time spent unpaid, leading companies to now offer to pay for commute costs. Sean Coughlan, a BBC News education and family correspondent, believe that emails while commuting should count as work. She is not alone in this thought.
But it isn't just about dollars and cents, commuting is known as "the stress that doesn't pay". Quality of life drops when you are a part of a system which collectively spent 5.5 billion hours traveling to work in 2011. Today's workers are leaving their jobs in record numbers and a large contributing factor is how long their commute is. A survey showed that 23% of those leaving their jobs attribute it to their commute. It's the unpredictability and the sudden loss of control of the situation which stresses people out.
The lack of commute is just one of the many reasons why businesses are switching from traditional commercial real estate to shared workspaces. PrimeWork Somerset offers the outstanding facilities and magnificent views of big-city coworking with small-town charm and convenience.
This new year, give yourself the gift of a shorter commute – and less stress. Join us at PrimeWork Somerset. We'd love to show you around!


Gwent Police have contacted the family of missing teenager Nida Ul-Naseer after a body was discovered in wetland today.
The 19-year-old from Pill went missing from her home while allegedly taking out the rubbish on December 28.
Officers were called to Gwent Wetland Site in West Nash Road at 10am this morning, after a body was found by a member of the public.
The body is not being linked to the search for the missing teenager at this stage, police said.
"We have made Nida's family aware of the situation because of the ongoing investigation but the body has not been found as a consequence of searching for Nida," a spokesman said.
"The body has yet to be identified. We continue to give the family support during this distressing time."
Ul-Naseer was an asylum seeker from Pakistan who had wanted to attend university to become a marketing or finance manager. But she had become upset after being unable to continue with her higher education.
Her sister Shamyla Ul-Naseer said: "She wanted to go to university. It was not a dispute - she just wanted to go to university.
"Because we are asylum seekers we are not allowed to go to university. She was angry about that. She was very sad. She was very angry about her future."


text:
Q: Sorting order in SQLite In the following query in SQLite
SELECT cfpref FROM cfprefs ORDER BY cfpref

I expect the output to be sorted in ASCII order. However, the output contains
GLAIC_TLC
GLAICSPW

in this order, even though underscore (_) in ASCII table is located after uppercase letters. Is it intentional, or is it a bug?

A: Do you, by any chance, use COLLATE NOCASE on cfpref?
Here is a SQLFiddle demo
When you use the default BINARY collation you will get your expected order
Here is a SQLFiddle demo

redpajama_set_name: RedPajamaStackExchange


Dual Channel or Single Memory?
In reality how much performance difference is there between dual channel and single channel? Is it worth it? If dual is better which applications would it be better in? I need some new Ram for my 8RDA+ and need to make the decision.
Definitely, but you need good RAN!
I take that as its worth it then? I'm looking at the OCZ PC3500EL.
I'm running an ADXA1700DLT3C week 0319 at 220x11.5 right now. It should help then?
But many report not being able to go beyond 200 in duel channel mode. Those I listen to recommend the DDR set up.
I would go for Single-Channel if you are to look for high FSB overclocking.
I had some OCZ PC3500EL on my 8RDA3+ and couldn't pass 185fsb in dual channel. Do yourself a favour and avoid these OCZ's. Even tho they are squarely aimed at dual channel, in reality, they are awful at it.
For example, I bought some Twinmos £100 cheaper, and they can post up to 235fsb! Thats a big difference, and also in dual channel. They are completely stable at 215fsb, and Prime for days. However, I need to OVP mod to my board to get higher I think.
Good luck anyway, and keep us informed!


There are eight categories of Songs on the Junior Cert Music course, they're all listed below. Some of them have very long titles and have been shortened to fit here.
Art Songs Songs from Operas, Operettas..
note any important features of that type of song that are in your set or choice song.
Songs from Operas, Operettas.. - Spring from "Ottone"


Search "aloe" 12 results have been found.
Extra-Soothing Water Cream (50ml - 1.7 fl oz) - Face&Body Line. With zinc oxide it has extra emollient, restorative and protective effects on the skin.
Face Cream "Francy" (50ml - 1.7 fl oz) - Ebe Line. Its natural and organic components moisturize and nourish the skin all day long. Its silky and light texture glides beautifully without greasing.


One day an aeroplane cleaner was cleaning the pilots' cockpit when he saw a book entitled "How to fly an aeroplane for beginners. Volume One".
He opened the first page which said, "To start the engine, press the 🔴red button.". He did so and the airplane engine started.
He did so and the aeroplane started moving at an amazing speed.
He did this and the plane started to fly.
After 20 minutes of flying, he was satisfied and wanted to land so he decided to go to the fourth page.
He fainted after reading the instruction..
The fourth page read, "To learn how to land, please purchase Volume Two at the nearest bookshop!!!!


Emerald ash borer has been confirmed for the first time in Wood County, less than a month after the destructive pest was discovered in Portage County. The Department of Agriculture, Trade and Consumer Protection(DATCP) says the insect was collected from a boulevard tree, and sent to the U.S. Department of Agriculture, which gave confirmation this week that it was the emerald ash borer. Both counties are now under quarantine. Property owners are urged to watch their ash trees for signs of infestation, which include thinning of the canopy, D-shaped holes in the bark, cracked bark, and woodpeckers pulling at the bark to get to the insect larvae beneath it.


text:
English, 05.02.2020 10:50 kenyaa63
What satirical statement does washington irving make about tom walker and society in this excerpt from "the devil and tom walker"? a. he insisted that the money found through his means should be employed in his service. b. he proposed, therefore, that tom should employ it in the black traffic; that is to say, that he should fit out a slave ship. c. this, however, tom resolutely refused: he was bad enough in all conscience, but the devil himself could not tempt him to turn slave-trader.
Answer from: andrespacheco5888
"He insisted that the money found through his means should be employed in his service" is the satirical statement among the choices given in the question that Washington Irving make about Tom Walker and society in this excerpt from "The Devil and Tom Walker". The correct option among the options given is option "A".
im not
Sorry i can't you here.
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text:
Saïd Benrahma misses out on Player of the Month award
Birmingham City's Che Adams takes Sky Bet Championship prize for February
Despite scoring four goals, and contributing as many assists, in five games, Saïd Benrahma has missed out on February's Sky Bet Championship Player of the Month prize.
The Algerian winger was beaten to the prize by Birmingham City's Che Adams after Blues striker netted six goals in five matches last month.
The four goals he set up took Saïd's to the top of the second tier's assist charts with 11. The 23-year-old has now been involved in 20 goals this term, the joint ninth-most in the Championship.
It's the second time in as many months that we have been beaten to a Sky Bet Championship prize after Thomas Frank was nominated for January's Manager of the Month prize.
Saïd Benrahma


Our D'Organica Garden Shoppee sponsored 10 sets (each four plants) cancer curing plants for auction to Sankalp Beautiful world. Thanks to each and everyone who have supported for this great cause. Special thanks to Ammu madam for this fabulous opportunity.
D' Organica Garden Shoppee has been invited to set up a stall in the Expo hosted by Greater Chennai Corporation. The expo has created awareness on eco plastic free society and pollution less living in the society.
Invitation from the US Consulate to attend Global Entrepreneurship Summit at IIT. Great learning experience and immense motivation from the meet.
D'Organica budding women entrepreneurs participated in our COWE founder's day celebrations forum. They had a great opportunity to meet people from different sectors and develop their business network.
Glad to be a part of the Green Temple inaugural function. Their mission is to reduce the city's landfill by converting organic and bio degradable waste into useful compost.
Had a wonderful opportunity to create awareness about Seed Stem activities like Organic Gardening, Junk art, Waste management program etc. at their inaugural function.
Thanks to Mrs.Vaijayanthi for the lovely opportunity.
Judge for Inter College competitions held @ Ethiraj College.
Guest Lecture presented by Jayasri Krishnan about Women Empowerment and Entrepreneurship on March 8th 2017.
Special lecture given by Jayasri Krishnan about Opportunities and Challenges for Women Entrepreneurship in India.
Motivational Talk by Jayasri Krishnan to create awareness about entrepreneurship in organic field.


text:
Hiding evidence just as bad as crime itself: campaigner
By Natasha Wallace
July 26, 2013 — 3.00am
Priests should be jailed for concealing evidence of sex abuse because they are effectively aiding and abetting a crime, a child protection campaigner has said.
The executive director of advocacy group Bravehearts, Hetty Johnston, was responding to testimony by high-ranking Catholic priest Father Brian Lucas that he did not take notes while interviewing about 35 priests from 1990-1996 who were accused of sex abuse, nor did he refer the matters to police. ''He should be jailed. That just aids and abets offenders to continue to offend and it is just as bad a crime, in my view, than committing the crimes itself,'' Ms Johnston said.
"I don't understand how you could do that": Bravehearts executive director Hetty Johnston. Credit:Michelle Smith
''The person didn't only not do their job but their moral obligation. It is absolutely the most appalling, atrocious response.''
Father Lucas is the general secretary of the Australian Catholic Bishops Conference, which oversees the National Committee for Professional Standards responsible for procedures in dealing with abuse complaints. Retired psychologist Stephen Paull, who has 25 years of experience in child protection in the NSW education department, said it was ''absolutely grossly negligent'' both legally and morally not to take notes at such meetings.
Mr Paull has been attending the inquiry in the public gallery.
''I don't understand how you could do that and have a clear conscious as a priest,'' Mr Paull said.
A spokeswoman for the bishops' conference conceded on Thursday the Church's policy document Towards Healing, established in 1996 in response to its poor handling of sex-abuse complaints, did not compel priests to take notes during meetings with alleged offenders.
''That just happened to be Father Lucas's legal practice but, with that said, we're not willing to speculate any more than that. We'll just leave it to the inquiry and its findings,'' she said.
The heads of the bishops' conference were in a meeting all day on Thursday and could not be contacted, she said.


To escape the holiday induced cabin fever, we picked up one of K's friends and headed to the movies. This was part of the conversation on the way home.
K: "How are you going to get to Disney World? Are you gonna fly?"
M: "I'm gonna eat 20 pounds of beans and fly there on fart power!"
Oh, I am soooooooo glad I have girls!


text:
SN 1997ep – supernowa typu Ia odkryta 28 grudnia 1997 roku w galaktyce A045748-0342. W momencie odkrycia miała maksymalną jasność 22,40.

Przypisy

Supernowe zaobserwowane w 1997 roku


text:
ByMovienewz	 August 5, 2011 January 5, 2015
Movie Trailer for Pariah. Adepero Oduye, Pernell Walker and Kim Wayans star in the feature-length expansion of writer/director Dee Rees' award-winning 2007 short film. See the movie trailer for 'Pariah'. A Brooklyn teenager juggles with conflicting identities and risks friendship, heartbreak, and family in a desperate search for sexual expression.
Release Date: December 28, 2011 (NY/LA/SF)
Release Date: April 24, 2012 (Blu-ray, DVD)
Studio: Focus Features
Director: Dee Rees
Screenwriter: Dee Rees
Official Website: PariahMovie.com
Starring: Adepero Oduye, Pernell Walker, Kim Wayans, Charles Parnell, Sahra Mellesse, Aasha Davis
MPAA Rating: (R) for sexual content and language.
Buy New: $17.99 (Save 40%)
Adepero Oduye portrays Alike (pronounced "ah-lee-kay"), a 17-year-old African-American woman who lives with her parents (Kim Wayans and Charles Parnell) and younger sister (Sahra Mellesse) in Brooklyn's Fort Greene neighborhood. Alike is quietly but firmly embracing her identity as a lesbian. With the support of her best friend Laura (Pernell Walker), she is especially eager to find a girlfriend. Wondering how much she can confide in her family, Alike strives to get through adolescence with grace, humor, and tenacity — sometimes succeeding, sometimes not, but always moving forward.
DVD and Blu-ray Special Features:
Dee Rees: A Director's Style
A Walk in Brooklyn
Trying Out Identity: Pariah's Wardrobe
Pariah – Movie Trailer
Post Tags:	#Adepero Oduye#Drama#Kim Wayans#Pariah#Pernell Walker#Urban
California Crumbles in the New San Andreas Trailer
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text:
\section{The Rare Light Elements}

The trio of light elements, Li, Be, and B, offer a special opportunity to
discern the structure and processes occurring beneath the surfaces of stars.
The three are destroyed by fusion reactions at a few million K.  The isotope
of $^7$Li fuses with a proton at $T$ $\sim$2.5 x 10$^6$ K and higher which
corresponds to the inner 97.5\% (by mass) of the solar model.  For $^9$Be the
temperature is $\sim$3.5 x 10$^6$ K and higher, or 95\% (by mass).  The
relevant figures for the B isotopes ($^{10}$B and $^{11}$B) are near 5 x
10$^6$ K and 18-20\% (by mass).  Thus the surface zones in which each element
is preserved have different dimensions; the amount of each element remaining
on the stellar surface indicates how deep the mixing has been.  And since the
depletion in F and G dwarfs is apparently due to slow mixing, the depletion is
a function of the age of a star.

Due to the low abundances of these rare light elements in stellar atmospheres,
they are primarily observed in their respective resonance lines.  For F and G
stars these are 6707.74 and 6707.89 \AA\ of Li I, 3130.42 and 3131.06 \AA\
of Be II, and 2496.77 \AA\ of B I.  The Li I resonance doublet occurs in a
relatively clean part of the spectrum, but both the Be II and B I features are
in spectral regions crowded with other lines.  Extracting the abundances
requires the use of spectrum synthesis methods.  Examples of synthesized
spectra of all three elements can be found in Boesgaard et al.~(2004c).

\subsection{The Li and Be Dips in mid-F Dwarfs}

The discovery of the Li dip in the Hyades by Boesgaard \& Tripicco (1986) was
followed by a series of papers searching for such a dip in other open clusters
(e.g. Pilachowski, Booth \& Hobbs (1987), Boesgaard, Budge \& Ramsay (1988),
Hobbs \& Pilachowski (1988), Soderblom et al.~(1993), and more recently,
Steinhauer (2003).)  A search for a Be dip in the Hyades was done by Boesgaard
\& Budge (1989) with the tantalizing hint of such a dip.  It has been possible
with the Keck telescope and HIRES (Vogt et al.~1994) to re-examine the Hyades
and to extend the search for a Be dip to other clusters.  One cautionary note,
however, is that many of the young stars with mid-F spectral types (near the
center of the dip) are rotating sufficiently to affect the reliability of the
Be abundance determination.  Therefore we observed stars with $v$ sin $i$ $<$
20 km s$^{-1}$.

Boesgaard \& King (2002) found compelling evidence of a Be dip in the Hyades
which is $\sim$700 Myr old; this is shown in the left panel of Figure 1.  The
comparison of the Li and Be abundance is shown in the right panel of Figure 1.
The abundances are on the same scale and are normalized to the meteoritic
values of A(Li) = 3.30 and A(Be) = 1.42 (Grevesse \& Sauval 1998).  (We define
A(element) = log N(element)/N(H) + 12.00.)  There are two major differences in
the abundance-temperature profile between the two elements.  1) The Be dip in
the mid-F stars is not as deep as the Li dip.  2) There is no apparent
depletion of Be in the G stars in spite of the large (a factor of 100)
depletion of Li.  These results are not unexpected as the Be atoms need to be
mixed down deeper to higher temperatures within the star to be destroyed.  The
volume of the region where Be is preserved is larger than that where Li is
preserved indicating a larger number of surviving Be atoms initially.

\begin{figure}[!ht]
\plottwo{betc4.ps}{belit4c.ps}
\caption{Left: The Be dip in the Hyades.  Abundances of Be are shown as a
function of temperature.  The horizontal line corresponds to A(Be) in
meteorites of 1.42.  Right: A display of both Li and Be in the Hyades on the
same scale with A(Be) on the left y-axis and A(Li) on the right y-axis.  The
Li results are shown as hexagons and the Be results as encircled plus signs.
The two elements are normalized to their respective meteoritic abundances of
1.42 for Be and 3.30 for Li, shown by the horizontal line.  ApJ, 565, 587.}
\end{figure}

\begin{figure}[!ht]
\plottwo{belicppn.ps}{becoumerrc2.ps}
\caption{Left: Li and Be abundances in the Pleiades and $\alpha$ Per samples.
The Pleiades Li results are shown as hexagons and the Be results as encircled
plus signs and the $\alpha$ Per results as triangle for Li and circled x signs
for Be.  ApJ 582, 410.  Right: Abundances of Be in the Coma and UMa clusters
compared with the Hyades (small dots).  The Coma results are shown as
encircled plus signs and Uma as circled x signs.  ApJ, 583, 955.}
\end{figure}

Other young and intermediate age clusters have been investigated for the
presence of a Be dip and to check Be in the G dwarfs.  Boesgaard, Armengaud \&
King (2003a) looked at the younger Pleiades and $\alpha$ Per clusters.  The
left panel of Figure 2 shows the scaled Li and Be abundances in those two
clusters.  There is no evidence of a Be dip in these clusters which are
$\sim$50 - 70 Myr old.  This indicates that the Li-Be dip is a phenomenon that
occurs on the main sequence, not during pre-main sequence evolution, after an
age of 100 Myr or so.

Other young clusters have been studied for Be including Coma and the UMa
moving group which are slightly younger than the Hyades at 300 - 500 Myr.
Boesgaard, Armengaud \& King (2003b) found evidence of Be dip in the Coma
cluster which can be seen in the right panel of Figure 2.  It is shown in
comparison with the Hyades Be dip and is on the same scale as the left panel
of Figure 1.  The pattern is similar to the Hyades with perhaps more
(intrinsic?) spread in A(Be).  The Praesepe cluster was also studied by
Boesgaard, Armengaud \& King (2004a).  They found depleted Be in the Li dip
region in Praesepe stars and summarized the results for five young to
intermediate age clusters.  The correlation between Li and Be in the cluster
stars was presented for stars in the temperature range from 5900 - 6650 K.
(This is discussed below in $\S$1.3.)

\subsection{Beryllium in Field Stars}

In addition to the Be studies in cluster stars Boesgaard et al.~(2004b) have
determined Li and Be in an array of F and G field dwarfs with high S/N spectra
primarily from Keck/HIRES (Be) and the UH 2.2-m coud\'e spectrograph (Li).
They have compiled the results from that and other studies, including the
cluster work, into plots showing the range and trends of A(Be) with both
effective temperature and metallicity.  Those results are shown in Figure 3.

It can be seen that there are stars at or near the meteoritic abundance at all
temperatures (left), but only at the higher metallicity values, near solar
[Fe/H] (right).  The field stars can show large Be depletions (two orders of
magnitude and more), but the (young) cluster stars in the Be dip region have
depletions of no more than a factor of 10.  For the cooler stars ($T$ $<$ 5700
K) field stars show depletions of up to a factor of 4, but the relatively
younger cluster stars have little or no Be depletion.  The field stars in the
Be dip may have no Be depletion while others have depletions larger than a
factor of 100.  The highly Be-depleted stars may be the older ones or those
with higher initial angular momentum.

The right panel of Figure 3 shows that the full range of A(Be) is seen at
solar metallicity, [Fe/H] = 0.0 $\pm$ 0.2.  The full range extends out to
stars with metallicities a factor of two less than solar ([Fe/H] = $-$0.3).
It appears that there is an upper envelope of A(Be) as a function of [Fe/H];
that is, the initial amount of Be in stars is correlated with its [Fe/H].
This appears to be the case for halo stars as well (e.g.~Duncan et al.~1998).

\begin{figure}[!ht]
\plottwo{betallexoc.ps}{befeallexoc.ps}
\caption{Left: Values of A(Be) as a function of temperature.  This compilation
is from several sources; the crosses are field stars from Boesgaard et
al.~(2004b), Deliyannis et al.~(1998) and Boesgaard et al.~(2001).  The
inverted triangles represent upper limits on A(Be) from those papers.  The
open circles are cluster stars from Hyades (Boesgaard \& King 2002, Boesgaard
et al.~2004a) the Pleiades and $\alpha$ Per (Boesgaard, Armengaud \& King
2003a), Coma and UMa (Boesgaard, Armengaud \& King 2003b) and Praesepe
(Boesgaard, Armengaud \& King 2004a).  The plus signs are the stars with
exoplanets from Santos et al. (2002).  Right: Values of A(Be) in F and G
dwarfs as a function of [Fe/H].  The symbols are the same as in the left
panel.  ApJ, 613, 1202.}
\end{figure}

\subsection{The Correlation of Li and Be}

The cluster and field star data on Li and Be can be assembled to investigate
the correlation between the abundances of these elements.  Boesgaard et
al.~(2004b) have done this and have found correlations for the 88 field and
cluster stars between 5900 - 6650 K.  They have divided this into two
temperatures ranges corresponding to the cool side of the Li-Be dip, 6300 -
6650 K, where Li and Be are increasing as the temperature decreases and the
cooler group of early G stars near the Hyades Li peak, 5900 - 6300 K.  The
correlations for these two groups are shown in Figure 4, along with the best
fit slope for each group.  A light line with the slope for the other group is
also shown to illustrate differences between the two temperature groups.

\begin{figure}[!ht]
\plottwo{tall6366c.ps}{tall5963c.ps}
\caption{Left: The Li and Be abundances in the hotter stars which corresponds
to the cool side of the Li-Be dip, 6300 - 6650 K.  The dot-dashed line
represents the best-fit least-squares slope of 0.43 $\pm$0.04.  The faint
dotted line is the slope for the stars in the right panel.  The horizontal and
vertical dashed lines correspond to the meteoritic Be and Li abundances
respectively.  Right: The Li and Be abundances in the cooler stars, 5900 -
6300 K.  The dot-dashed line represents the best-fit least-squares slope of
0.34 $\pm$0.03.  The faint dotted line is the slope for the stars in the left
panel.  ApJ, 613, 1202.}
\end{figure}

For the 35 stars with $T$ = 6300 - 6650 K the least squares fit gives the
relationship: A(Be) = 0.433 ($\pm$0.036) A(Li) $-$ 0.071 ($\pm$0.094)

For the 54 stars with $T$ = 5900 - 6300 K the least squares fit gives the
relationship: A(Be) = 0.337 ($\pm$0.031) A(Li) + 0.248 ($\pm$0.078)

The 88 stars in the total sample from $T$ = 5900 - 6650 K are shown in the
left panel of Figure 5.  The least squares solution for this line is:

A(Be) = 0.382($\pm$0.030) A(Li) + 0.105 ($\pm$0.078)

\begin{figure}[!ht]
\plottwo{5966noc.ps}{rotmodels2.ps}
\caption{Left: The Li and Be abundances in the full sample of 88 cluster and
field stars with $T$ = 5900 - 6650 K.  A typical error bar is in the lower
right.  The horizontal and vertical dashed lines represent the meteoritic Be
and Li abundances respectively.  Right: Models - see text.  ApJ, 613, 1202.}
\end{figure}

Calculations of Li and Be depletion due to rotationally-induced slow-mixing
have been made by Deliyannis \& Pinsonneault (1997) for dwarf stars of
selected ages (0.1, 1.7, and 4 Gyr), initial rotation (10 and 30 km s$^{-1}$)
and specific temperatures (see their Figure 2).  Examples of these depletions
at the three ages and the two initial velocities are shown in Figure 5, right
panel, for specific temperatures between 5900 and 6300 K.  The observed slope
is shown as the dot-dashed line from Figure 4, right panel.  For this
comparison the initial A(Be) is taken as 1.28, which corresponds to the mean
of the high values in Figure 4, left panel.  The observations and predictions
are in remarkably good agreement and very supportive of the conclusion that
the light element depletion is due to rotationally-induced mixing.  Deliyannis
\& Pinsonneault (1997) argue persuasively against mass loss and diffusion as
the source of the depletion.

\subsection{Boron in Field Stars}

In order to study B in the Galactic disk, Boesgaard et al.~(2004c) used HST +
STIS to obtain spectra of the B I line at 2497 \AA\ in 20 stars which had no
depletion of Be.  The stars are from the upper envelope of Figure 3, right
panel, and cover a range in [Fe/H].  Since the Be abundance is undiminished in
these stars, the B abundances would be unaffected by depletion also.

\begin{figure}[!ht]
\plottwo{bsyn.ps}{ndisk.ps}
\caption{Left: An example of the spectrum synthesis of the B I line.  The
upper star is a high resolution spectrum, $R$ = 114,000, while the lower star
is at medium resolution, $R$ = 30,000.  The dots are the observed points, the
solid line is the best fit, and the dashed lines are a factor of two in A(B)
above and below the best fit.  Right: The B and Be abundances in the sampl of
stars with undepleted Be.  There is a slope to the relationship with [Fe/H] of
about 0.40 for both Be and B.  ApJ, 606, 306.}
\end{figure}

Figure 6, left panel, shows and example of the spectrum synthesis for B I.
The results of the research to determine the initial values for B and Be in
Galactic disk stars are shown in Figure 6, right panel.  Both B and Be increase
slowly with Fe such that as Fe increases by a factor of 4, Be and B increase
by a factor of $\sim$1.7.

Those relationships are:

A(Be) = 0.382 ($\pm$0.135) [Fe/H] + 1.218 ($\pm$0.037)

A(B)$_{NLTE}$ = 0.402 ($\pm$0.117) [Fe/H] + 2.371 ($\pm$0.032)

The ratio of B/Be for the 20 stars was found to be 15, with no trend with
[Fe/H].  This ratio is consistent with the predictions of spallation reactions
as the source of Galactic Be and B.

\subsection{The Correlation of Be and B}

Another HST/STIS study of B focussed on stars with large Be depletions to
try to find stars that were depleted in B.  In this work Boesgaard, Deliyannis
\& Steinhauer (2005) looked at 13 F and G stars with large Be depletions and
at five Be-normal stars.  The result was the discovery of a correlation
between Be and B as shown in Figure 7.  The left panel showns the Be and B
abundances in our sample of 18 stars and has a slope of 0.20 $\pm$0.05.  Those
values have been corrected for the differences in the initial values of B and
Be that result from the relations seen in Figure 6, right panel.  Other Li-
and Be-normal stars have been added from the work described in the previous
section; those results are seen in Figure 7, right panel, where the slope is
0.18 $\pm$0.06.  Predictions for B depletion have not yet been made, but it
seems likely that rotational mixing will be a key ingredient in the small B
depletions.

\begin{figure}[!ht]
\plottwo{mixbbe.ps}{tmixrallbbe.ps}
\caption{Left: The correlation of B and Be.  Three stars with upper limits on
A(Be) are shown with left-directed arrows.  Right: The normalized values of
A(Be) and A(B) to correct for different initial values depending on [Fe/H], as
seen in Figure 6, right.  Additional Li-normal and Be-normal stars are
included.}
\end{figure}

\section{Li, Be, B Summary}

We have presented an amalgamation of several research projects on light
elements from spectra obtained primarily with the Keck telescope and HIRES and
HST with STIS.  In addition to the Li dip in several intermediate age
clusters, we have now discovered a Be dip in those clusters.  The Be dip is
not as deep as the Li dip, that is, Be is not as depleted as Li.  Neither Li
nor Be is measureably depleted in the younger open clusters, e.g.~Pleiades.
The depletion of these elements occurs during main-sequence evolution, after
an age of $\sim$100 Myr.  Although Li is depleted in cooler stars, and the
depletion increases with decreasing surface temperature, there is little or no
Be depletion in stars cooler than 5900 K.

Many stars in clusters and the field show depleted, but detectable, Li and
Be.  The abundances of Li and Be are found to be correlated in such stars with
Li being more depleted than Be.  For stars in the temperature range of 5900 -
6650 K the relationship is:

A(Be) = 0.382 ($\pm$0.030) A(Li) + 0.105 ($\pm$0.078).

\noindent
When Li has decreased by a factor of 10, Be has decreased by only a factor of
2.4.  This relationship is very well matched by the predictions of models with
rotationally-induced mixing.

Through use of B abundances from HST data we have found that there are stars
with depleted, but detected, B.  And there is a correlation between the B and
Be abundances.  That relationship is:

A(B) = 0.175 ($\pm$0.058) A(Be) + 2.237 ($\pm$0.055).

\noindent
This slope is shallower than the Li-Be slope because the B preservation region
is larger and B atoms have to be mixed to deeper stellar layers to be
depleted.  When Be is down by a factor of 10, B is only reduced 1.5 times.

Li, Be, B all seem to increase at about the same rate with [Fe/H] in Galactic
disk stars.  The slope for A(B) with [Fe/H] is 0.40 and for A(Be) with [Fe/H]
is 0.38.  Large depletions have been found for all three elements in our
samples of F and G Population I stars.

\section{Carbon and Oxygen in Open Clusters}

After H and He, the most abundant elements are C, N, O, and Ne.  Determining
those abundances, however, is a difficult proposition.  This is a report on an
ongoing project to determine abundances in open clusters, and focuses on the
determination of Fe, C, and O abundances in three clusters: the Pleiades at an
age of $\sim$70 Myr, the Hyades at $\sim$700 Myr and M 67 at 5 Gyr.  The
spectra for all were obtained with Keck I + HIRES at high S/N and high
spectral resolution of $\sim$48,000.  The spectral range covered 5700 - 8120
\AA.  Abundances were determined from some 40 lines of Fe I, 6 of C I
and the 3 of the O I triplet.

\subsection{Oxygen Abundances}

Although abundances found from the O I triplet at 7771, 7773, and 7774 \AA\
are influenced by the effects of NLTE, the corrections to be applied are
complicated to determine and various researchers have found different results,
ranging from a few hundredths to a few tenths of a dex.  (In particular, there
is uncertainty in the size of the collision rates and cross sections for
collisions with neutral hydrogen, e.g.~Kiselman 2001.)  It is possible to take
an empirical approach on this issue.  First, we can determine O abundances in
a number of stars of different temperatures on the main sequence in the same
cluster.  All unevolved stars in a given open cluster can be expected to have
the same O abundance.  We have done this for 30 stars in the Hyades cluster in
a temperature range of 5700 - 7100 K; the spectra are from the Palomar 5-m
coud\'e and Keck + HIRES.  The O abundances (on the scale where log (H) =
12.00) from the O I triplet as a function of effective temperature are shown
in Figure 8 (left).  While the hotter stars show large O abundances, the
values found from Hyades stars cooler than 6200 K are consistent with each
other.  This suggests that the NLTE effects are small (at least consistent)
in the cool stars.

\begin{figure}[!ht]
\plottwo{ot2.ps}{ootttx.ps}
\caption{Left: Abundances of O from the O I triplet in Hyades main sequence
stars, showing the effect of stellar temperature.  All stars in the Hyades
should have the same O abundance, but the hotter stars give abundances that
are higher than the cooler stars, presumably due to effect of NLTE.  The
horizontal dotted line corresponds to a uniform value of log N(O)/N(H) + 12.00
= 9.10 for the 15 stars with $T_{\rm eff}$ $<$ 6200 K.  Right: Abundances of O
from observations of the O I triplet and the [O I] forbidden line in the same
stars, all having $T_{\rm eff}$ less than 6200 K.  The diagonal line shows the
equivalent abundance from the two techniques.  The stars are subdivided into
three temperature groups.  No differences are found in the three groups.  The
abundance errors are typically $\pm$0.10.}
\end{figure}

Another empirical approach is to examine O abundances found from the O I
triplet and the forbidden [O I] line at 6300 \AA\ when these features can be
measured in the same stars.  This can be done with the data set in King \&
Boesgaard (1995).  The result of this is shown in Figure 8 (right) for stars
cooler than 6200 K.  The diagonal line corresponds to the same abundance from
the two different features of O.  The two methods give the same result (within
the typical error of $\pm$0.10 dex) with no apparent difference in the three
temperature groupings shown in the figure.

As a result of these two empirical demonstrations, we have determined O
abundances from the O I triplet from observations of main sequence stars
cooler than 6200 K.  Note that Schuler et al.~(2004) find that O abundances
from the O I triplet begin to increase again for stellar temperatures below
5400 -- 5500 K in their study of O abundances in the Pleiades and M 34.  The
stars in our samples in the Pleiades and M 67 are all hotter than
5500 K.

\subsection{Hyades}

We have found abundances in some 18 Hyades late-F and early-G dwarfs from Keck
HIRES spectra with S/N from 610 to 730.  Figure 9 (left) shows the positions
of these stars in the Hyades HR diagram.  The abundances of Fe were

\begin{figure}[!ht]
\plottwo{hyhr.ps}{hyfet.ps}
\caption{Left: HR diagram for the Hyades from Hipparcos data.  The stars we
observed are shown as large open circles.  Right: Abundances of Fe in the
Hyades stars.  The horizontal dotted line shows the cluster mean [Fe/H] =
+0.18 $\pm$0.01.}
\end{figure}

\noindent
found from $\sim$40 Fe I lines for each star; those results are shown in the
right panel of Figure 9.  The mean cluster abundance is [Fe/H] = +0.18
$\pm$0.01, in good agreement with the recent value of +0.16 $\pm$0.02 (Yong et
al.~2004).

\begin{figure}[!ht]
\plottwo{hyspecci.ps}{hyspecoi.ps}
\caption{Examples of the spectra of the Hyades in the C I and the O I regions.
The top star is one of the hottest in our sample, the middle one is near the
solar temperature and the lower one is one of the coolest in the sample.}
\end{figure}

We have found O and C abundances from the high excitation lines of these
elements in the near IR spectrum.  The lines used are shown in each of three
Hyades stars in Figure 10.  The abundances are shown as a function of
temperature in Figure 11.  The stars studied are all cooler than 6200 K.
For the mean cluster [C/H] we find +0.16 $\pm$0.02 and a mean [C/Fe] =
$-$0.02.  For [O/H] we find the mean cluster abundance to be +0.17 $\pm$0.01
and a mean [O/Fe] = $-$0.01.

\begin{figure}[!ht]
\plottwo{hyct2.ps}{hykeckot1.ps}
\caption{Abundance results for the Hyades for C (left panel) and O (right
panel).  The horizontal dotted lines show the cluster means: [C/H] = +0.16
$\pm$0.02 and [O/H] = +0.17 $\pm$0.02.}
\end{figure}

\subsection{Pleiades}

We have obtained Keck/HIRES spectra of 20 late-F and early-G dwarfs with S/N
ratios of 95 -- 160.  The color-magnitude diagram for the Pleiades is shown in
the left panel of Figure 12.  The right panel of Figure 12 shows the results
for [Fe/H] in these Pleiades stars from $\sim$40 lines.

\begin{figure}[!ht]
\plottwo{plhr.ps}{plefet.ps}
\caption{Left: Color-magnitude diagram for the Pleiades with the large crosses
indicating the stars observed.  Right: Results for the Fe abundances in the
Pleiades stars.  The cluster mean [Fe/H] = +0.06 $\pm$0.02 (dotted line).}
\end{figure}

The mean value for the cluster is [Fe/H] = +0.06 $\pm$0.02, which is slightly
higher than previous values of +0.02 $\pm$0.06 (Boesgaard 1989), $-$0.03
$\pm$0.02 (Boesgaard \& Friel 1990), 0.00 $\pm$0.05 (Boesgaard, Budge \&
Ramsay 1988).  The abundance results for C and O are shown graphically in
Figure 13.  For [O/H] we find +0.11 $\pm$0.02 and thus [O/Fe] = +0.05.  Our
[O/H] is in good agreement with that from [O I] $\lambda$6300 of +0.14 from
Schulaer et al.~(2004).  Carbon is low in the Pleiades with [C/H] = $-$0.04
$\pm$0.02 and [C/Fe] = $-$0.10.

\begin{figure}[!ht]
\plottwo{plect.ps}{pleot93.ps}
\caption{Left: Carbon abundances in the Pleiades.  Right: Oxygen abundances in
the Pleiades.  The horizontal dotted lines show the cluster means: [C/H] =
$-$0.04 $\pm$0.02 and [O/H] = +0.11 $\pm$0.02.}
\end{figure}

\subsection{M 67}

The Keck/HIRES spectra of our 14 M 67 stars have S/N ratios ranging from 70 to
140.  The stars we selected were similar to the sun and have a range in
$T_{\rm eff}$ of 5600 - 6000 K.  Figure 14 (left) shows the color-magnitude
diagram for M 67 with our stars as open circles and the cluster represented by
a 5 Gyr isochrone from Vanden Berg (1985).  The [Fe/H] values for the M 67
stars are shown in Figure 14 (right) where the cluster mean is $-$0.05
$\pm$0.01.

\begin{figure}[!ht]
\plottwo{m67hr.ps}{m67fetc.ps}
\caption{Left: The color-magnitude diagram for M 67.  The line is the 5 Gyr
isochrone from Vanden Berg (1985) and the stars we observed are open circles.
Right: The [Fe/H] values for each star plotted against its temperature.  The
cluster mean [Fe/H] = $-$0.05 $\pm$0.01 (dotted line).}
\end{figure}

All of our M 67 stars are cooler than 6200 K (the hottest is 5974 K) and
hotter than 5500 K (the coolest is 5716 K).  The 14 stars are in good
agreement with each other in their values of [C/H] and [O/H].  Those results
are shown in Figure 15.  The cluster means are [C/H] = $-$0.02 $\pm$0.02 and
[O/H] = +0.01 $\pm$0.03.  The abundances of Fe, C, and O are quite close to
solar for the old open cluster, M 67.

\begin{figure}[!ht]
\plottwo{m67ct1c.ps}{m67ot1c.ps}
\caption{Left: Carbon abundances in the M 67.  Right: Oxygen abundances in the
M 67.  The horizontal dotted lines show the cluster means: [C/H] = $-$0.02
$\pm$0.02 and [O/H] = +0.01 $\pm$0.03.}
\end{figure}

\section{Carbon and Oxygen Summary}

The results for the three clusters are summarized in Table 1.  Although there
are only three clusters discussed here, it seems apparent that there is no
evidence of an age-metallicity effect in the disk clusters.  The differences
found in the composition of the clusters could result from the composition in
the local interstellar material from which they were formed, i.e. a ``place of
origin'' effect.

\begin{table}[!ht]
\caption{Open Cluster Abundances}
\smallskip
\begin{center}
{\footnotesize
\begin{tabular}{lrccccccccc}
\tableline
\noalign{\smallskip}

Cluster & Age & [Fe/H] & $\sigma$
& [C/H] & $\sigma$ & [O/H]
& $\sigma$ & [C/Fe] & [O/Fe] & [O/C] \\
\noalign{\smallskip}
\tableline
\noalign{\smallskip}
Pleiades & 70 Myr  & +0.06   & 0.02 & $-$0.04 & 0.02 & +0.11 & 0.02 & $-$0.10
& +0.05   & +0.15 \\
Hyades	 & 700 Myr & +0.18   & 0.01 & +0.16   & 0.02 & +0.17 & 0.02 & $-$0.02
& $-$0.01 & +0.01 \\
M 67	 & 5 Gyr   & $-$0.05 & 0.01 & $-$0.02 & 0.02 & +0.01 & 0.03 & +0.03
& +0.06   & +0.03 \\
\noalign{\smallskip}
\tableline
\end{tabular}
}
\end{center}
\end{table}

The Hyades is enhanced in Fe, C, and O relative to solar by
about +0.17 dex.  For M 67 the amount of the three elements is similar to that
in the Sun.  Although the Pleiades seems slightly enhanced in Fe and O by
about +0.05 dex compared to the Sun, it seems to be low in C with [C/H] =
$-$0.04 and [C/Fe] = $-$0.09.

\acknowledgements

I am grateful for the help of several graduate and undergraduate students on
aspects of the yet-unpublished part of this work: M 67 - Elizabeth Barrett and
John Lakatos; Hyades - Jennifer Beard and Edward Lever; Pleiades - Hai Fu.  I
am pleased to acknowledge all the clever help of my various co-authors in the
published papers, especially Jeremy R. King, Eric Armengaud, Constantine
Deliyannis, Alex Stephens, Elizabeth McGrath and David Lambert (to whom this
symposium is dedicated).  I am happy to thank Megan Novicki for important
contributions to the presentation.  Figures 1-6 are reproduced by permission
of the American Astronomical Society.  The work reported here has been
supported by N.S.F. grants AST 00-97945 and AST 00-97955 and by NASA/STScI
grants HST-GO-08770 and HST-GO-09048.

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