Duratuff Select's new generation of vinyl cladding weatherboards offers rich, vibrant colours with authentic wood grain textures for a more beautiful home. Cladding, put simply is the process of covering and protecting the outside of your home for a more aesthetically pleasing appearance.
It's that time of year again. Winter is upon us already! , increasing the need to warm your home. So why not add style and elegance with a fireplace made from the eye-catching CraftStone. Exclusively available through Austech in a range of colours and textures, CraftStone allows you to build your dream fireplace including all the benefits of natural stone, without the hefty price tag.
Many home owners have previously selected CraftStone as their favoured product when developing a fireplace. The stone product has a wide range of other applications in new constructions and renovations. As well as fireplace's, it is perfect for stone walls, as a architectural element, an alternative for external feature walls, and also interior feature walls and entries. "We offer many textures and colours and meet over a dozen of the strictest code requirements, which give users a vast array of design options," said Dean Smith, Marketing Coordinator of Austech External Building Products. "When you combine such quality and choice, you're going to have a winning product."
Austech Building Products have a display at their head office in Blacktown, showcasing CraftStone. The external display can be viewed every day, with an internal display also available during office hours. For further information on CraftStone and the wide range of products available please visit Austech, or contact the team on (02) 9831 1623.
Firstly there is the manufacturing procedure involved in creating the product. Expanded Polystyrene(EPS) is made using small expandable beads that inflate with heat, and then are placed into a mould, where they expand to fit the shape. The expanded beads trap air, which gives expanded polystyrene its insulation properties, but also leaves it venerable to water absorption, reducing the insulations effectiveness over time.
Vinyl Cladding has a number of functions to perform when it comes to your home. Of course there is the aesthetic value of whatever material you decide will best suit the house you live in and look at every day; a finish which is pleasing to the eye and enhances the look of your home, as well as improving your property (and its value). This is not the least of the considerations you have to take account of when choosing the best cladding for the purpose as its durability and performance is equally important.
Vinyl cladding, also called vinyl siding, refers to plastic exterior cladding for homes and commercial buildings. The siding is used as an alternative to traditional wood, fiber cement, and aluminum cladding. The cladding is made up of about 80% polyvinyl chloride (PVC) resin and the remaining 20%, ingredients to give the material its color, gloss, opacity, flexibility, durability, and impact resistance. Vinyl siding has been in the market since the late 50s and it is today one of the most popular exterior building products in the U.S. and Canada. There are several reasons why you should consider installing vinyl cladding.
This is one of the most affordable sidings in the market. You will spend between 25% and 50% less than what you would have spent on aluminum and wood siding. Most vinyl cladding manufacturers offer competitive warranties.
Many people neglect their homes' exteriors, but waterproofing the exterior is important because it improves the longevity of your walls and it saves you money on repairs. A strong wall is also important for your security.
With the evolution of technology comes the introduction of new and innovate programs, in the building industry the ability to visualise the outcome of your project is a sought after skill. Austech has combined with Royal Building Products and produced a Virtual Re-Modeler. The Virtual Re-Modeler gives the customers the ability to select their own colours and design a house with their choice of cladding.
The Program offers 9 different houses in which to renovate with our Duratuff Select Vinyl Cladding. For a more personal experience, the option to upload a photo of your own home is the perfect solution for those fussy home owners.
Austech has worked closely and proudly with Danrae Water Proofing on Australia's First Living Building Project. The University of Wollongong's Sustainable Building Research Centre is currently under construction, and is due to being completed by mid-2013. The Living Building Challenge comprises seven performance areas; water, energy, health, materials, equity and beauty. Austech provided more than 500sqm2 of Polyboard Enviro 300, in both the 50mm and 75mm thickness, for rooftop and plaza deck insulation.
The 2,600 sqm2 building is set to produce more energy per year than it consumes, via a rooftop photovoltaic (solar) panels along with a wind turbine. Austech's Polyboard Enviro 300 is a zero Ozone Depletion Potential, (meaning it releases no chemicals when manufactured) Green Star compliant extruded Polystyrene making it the perfect match for the Living Building Project.
Foamular Extruded Polystyrene was used for a roof membrane system and under the Main Plaza. 4500 meters square of Foamular was used throughout the project. 60 mm Foamular was chosen which gives an R-value of two.
The building uses chilled beams throughout to cool the building as an alternative to air-conditioning. This is an Australian first and is expected to reduce overall electrical consumption by 30 %.
Austech Western Australia will be setting up displays next week on Tuesday the 26th and Wednesday the 27th of March at Hannan's Boulevard. There will be several products on display and staff to assist with any queries you may have. There will be plenty of samples and even the chance to take down details to arrange an appointment for an obligation free quote. The Display was last set up at Wagin, Woollorama and was a great success.
Duratuff Select Vinyl House cladding was selected to be installed as a maintenance free exterior to an extra 58 cabins at the Barney Beach Caravan Park in Gladstone to relieve pressure on the districts' accommodation shortage.
Barney Beach Caravan Park is a waterfront property situated at Gladstone's historic Barney Point Beach. The park was Gladstone's first, and is today one of Queensland's oldest parks still owned and operated by the original owners, the Corones Family.
The "boutique-style" park is steeped in charm and history offering guests superior service and immaculate facilities in a parkland setting. Located 80 metres from a swimming and fishing beach and five minutes to the city centre, Barney Beach Caravan Park offers caravan and camping sites and has the largest range of award winning value accommodation in the Gladstone Region.
Custom Cubbies are a family owned and run Australian business that specializes in not only children's cubbies, but also in sheds, cabins and any other outdoor building you could need. Custom Cubbies now offer Duratuff Select Vinyl Cladding on all their products, helping owners benefit from maintenance free cubbies that last longer and look better.
The key concern in designing cubbies for children is safety and durability. Vinyl cladding will not rot, split or peel so there is no danger of splinters. On top of this it needs to last, cladding is designed to be impact resistant, colour fast and easy to clean.
One huge issue for Custom Cubbies was transportation. The Cubbies are pre-fabricated in their factory and shipped all over Australia. The shipping process often lead to damage to the exterior cladding, but with Vinyl this is rarely a problem since it doesn't scratch, dent or crack.
Austech recognizes the need for environmentally friendly products as Australia moves towards a green future. With the recognition of this movement comes as a solution in the form of Duratuff Select Vinyl Cladding.
Vinyl was first created in the 1920's and quickly became a key component in many products, including wall cladding. Vinyl is now the world's second most used plastic, but unlike its counterparts, Vinyl has many environmentally friendly features.
The main building block for vinyl is Chlorine, made from common salt. This makes up just under 60% of vinyl's chemical structure. Meaning it is a sustainable and cost effective product.
Austech along with Craftstone provide the perfect solution for your entertainment area problems. Our Craftstone can create a wall feature that is a stunning departure from the traditional entertainment centres.
Perhaps one of the most cherished rooms in the house, the lounge room. Traditionally the family TV is either wall mounted onto a bracket or sits upon a Cabinet or table. Flat Screen TV's, surround sound speakers and Blue ray players are all making up the modern media experience in homes all around Australia. With these entertainment devices comes an unwanted compromise of the room's aesthetics and style. You can hide all those untidy cords by simply transforming your wall with Austech wide range of Crafstone Products.
The look of a picturesque stone feature wall adds class and life to a once dull area of the house. Brighten and add warmth to your living room today.
Austech External Building Products have now added a new line of products to their existing range. Now certified distributors of BGC Fibre Cement Cladding & Stonesheet, Austech can supply and deliver material at wholesale prices. As specialists in external lightweight claddings and facades, Austech are now able to offer more choice and an even wider range to suit your home or project. BGC products are made and manufactured in Australia.


Could Morgan (Lennie James) be on the run again or does he have a plan to help his friends?
Fear the Walking Dead Season 4 Episode 16: "...I Lose Myself"
case, but I think it applies to this woman too.
Morgan: I still gotta try though.
John: I know you do.
Permalink: I know you do.
Morgan: She's stuck. Whatever happened to her, she thinks killing is the only way.
John: How you gonna convince her otherwise?
Morgan: Because I understand her... I used to be her.
Permalink: Because I understand her... I used to be her.


Looking For General Practice Attorneys?
Our Lawyers are committedto providing excellence in representation with cost-effective approach. As the largest group of family lawyers in British Columbia we offer lawyers with various levels of experience and expertise. We provide a range of services including Court proceedings, collaborative law and mediation.


This exhilarating introductory level cycling tour along the Kathmandu Valley Rim at an altitude above 1,350 metres is an experience like no other. From the ridge-top trails that encircle the Kathmandu Valley, amazing vistas can be observed as one cycles against a spectacular alpine backdrop of Himalayan mountain peaks.
We leave Kathmandu after breakfast through the bustling back streets of Thamel and on to good wide undulating jeep tracks into jungle. Our efforts are rewarded by spectacular mountain views. We travel downhill and then on upwards for the seriously fit ride (22km) up to Kakani. We camp in a reserve at 2,000m to enjoy the stunning views of mount Ganesh and Langtang, and the valley of Likhu Khola (river) 1,000m below.
exposure to rarely frequented pockets of Nepalese culture and the unforgettable warmth of local villagers.
This activity is recommended for people who love bike riding and who are looking for new, 'out of the way' places to visit. This mountain bike ride is a wonderful way to explore the natural beauty of the valley and its surrounds, and offers a unique opportunity to come into contact with aspects of Nepalese culture not often seen by travellers.
Fitness Level Required: A good level of fitness is required as the trail at times throws up some challenging climbs. This is an off-road ride which avoids vehicle access roads.
Skill Level Required: Moderate. Some sections along the route are a bit technical.
This is an ad-on tour. Your tour starts from Kathmandu. Ride from Kathmandu to Kakani. Overnight in guest house.
Ride from Kakani to Budhanilkantha. Overnight in resort. 53 km.
Ride from Budhanilkantha to Nagarkot. Overnight in hotel.
Ride from Nagarkot to Dhulikhel via Nala. Overnight in hotel.
Ride from Dhulikhel to Sisneri via Panauti & Drive to Kathmandu.
Comfortable hotels in Kathmandu and local lodges during cycling tour.
Kathmandu hotel will include breakfast. Three meals a day will be provided during cycling tour.
Bike not provided but it can be hired if you are not bringing your own. Guide will have First Aid Kit and Mechanical Backup. 50% of this trip is vehicle supported.
Once every Week throughout the year.
AU$1150 per person on twin share basis.


text:
When will the COVID-19 vaccines get full FDA approval?
The short answer — at least for one vaccine — is sometime between now and January 2022.
Vials of the Moderna COVID-19 vaccine that are being administered for local residents at a vaccination center at the building part of the Tokyo Skytree, the tallest structure in Japan, Wednesday, June 30, 2021, in Sumida ward of Tokyo. (AP Photo/Eugene Hoshiko)
By: Mvalverde
When will the COVID-19 vaccines get full Food and Drug Administration approval?
That's a question on a lot of minds as the daily number of COVID-19 cases rise across the U.S., driven by a more contagious mutation of the coronavirus. More public and private institutions are considering or imposing vaccine mandates on their employees. And some, including the Department of Defense, say they will consider requiring employees be vaccinated once the Food and Drug Administration gives the vaccines final approval.
When will that happen? The short answer — at least for one vaccine — is sometime between now and January 2022.
Pfizer and BioNTech, which developed one of the three COVID-19 vaccines available in the U.S., in May completed their application for full FDA approval for use in people ages 16 and older. They are the only companies to have completed an approval application so far. The FDA is giving the application priority review, which expedites the process by a few months, with a decision deadline of January 2022. But the agency says it expects to have a decision before January.
Moderna said in June that it had begun submitting parts of its application. Johnson & Johnson has not yet submitted an application, but plans to this year.
In the meantime, the three vaccines are all under what is known as emergency use authorization. Two of the vaccines, Pfizer/BioNTech's and Moderna's, got that designation as far back as December 2020. Johnson & Johnson's vaccine received the authorization in February 2021.
The FDA requires even more information from the manufacturers before it grants full approval.
Some experts believe that once the vaccines get full licensure, confidence about their safety and effectiveness will grow among the sizable portion of the population who have not been vaccinated.
What's the holdup?
Here's what we know about where the process stands.
What's an emergency use authorization?
During public health emergencies, like the coronavirus pandemic, the FDA has the legal power to grant emergency use authorization to certain products if they meet specific criteria and when there's no adequate, approved and available alternative to treat the malady. A goal of this authority is to make products available quickly, when people urgently need them. Scientists and physicians at the FDA decide whether to grant such authorization.
When COVID-19 was declared a pandemic in early 2020, there weren't any approved vaccines for it. As manufacturers developed therapeutics for COVID-19 — such as testing kits, blood purification devices and vaccines — they sought emergency use authorizations from the FDA. The agency has published information about these products throughout the COVID-19 pandemic.
Under an emergency use authorization, products become available based on the best available evidence at the time and if the benefits outweigh any known or potential risks. An FDA approval depends on more substantial evidence that the product is effective and that its benefits outweigh its risks.
"An emergency use authorization has a slightly lower bar to cross than full approval, but has come about after a comprehensive review of the data," Seema Shah, a Northwestern University professor of medical ethics previously told PolitiFact.
The FDA has granted emergency use authorizations for diagnostic tests and treatments during other public health emergencies, including the H1N1 pandemic that started in 2009.
What does the FDA consider when approving a vaccine?
It's up to companies to submit applications that would move their products from emergency use authorization to full approval.
Companies seeking FDA approval must submit to the agency a Biologics License Application, which includes technical information, at least six months of clinical data, non-clinical data on the development of the vaccine in the lab, detailed manufacturing information, and data on the safety of the vaccine.
Before granting approval for a vaccine, the FDA must determine whether clinical data and other information show that it is safe and effective and whether it can be manufactured according to federal quality and control standards.
The FDA reviews and verifies data in detail, and full approval hinges on the information in a complete application, said Peter Marks, FDA's Center for Biologics Evaluation and Research, in a letter to the editor published by the New York Times on July 9.
"This approach helps to ensure that the FDA has all the available data from clinical studies and provides the public with trust and confidence in the quality, safety and effectiveness of any vaccine that the agency approves," Marks said. Any approval without a high-quality review "would undermine the FDA's statutory responsibilities, affect public trust in the agency and do little to help combat vaccine hesitancy," he said.
What is the status of approval applications to the FDA?
The FDA on July 16 formally accepted Pfizer and BioNTech's application for approval of the vaccine for people age 16 and older. The companies said they plan to request approval for people ages 12 to 15 once they have additional required data. They got an emergency use authorization for this age group in May.
Moderna said in June that it had started a "rolling" submission process with the FDA for approval of its vaccine on people ages 18 and up. Under a rolling review, a manufacturer can submit sections of the application for review as they are completed, rather than waiting to submit them all at once. Moderna also plans to request priority review. Under priority review, an FDA decision on approval is expected within six months of receiving a completed application, compared with 10 months for a standard review.
Johnson & Johnson has not submitted an application for approval. A spokesperson said Johnson & Johnson is continuing to gather data and plans to file a licensing application with the FDA "later in 2021."
This article was originally published by PolitiFact, which is part of the Poynter Institute. It is republished here with permission. See the sources here and more of PolitiFact's reporting and fact checks here.
Tags: Coronavirus, PolitiFact
mvalverde

redpajama_set_name: RedPajamaCommonCrawl


Artistically decorated pianos have popped up at various locations in the CBD as part of the Play Me, I'm Yours street piano project.
Running from January 19 to February 4, the interactive installation features pianos donated and decorated by community artists and groups at locations such as Flinders Street Station, the County Court, Chinatown and Queen Victoria Market.
The initiative encourages people to pull up a stool and play the pianos to activate the urban space.
Indian architecture student Zari Subhlok and Chinese artist Xiaolan Li painted the street piano in front of the County Court on William St with a few other international students.
This piano features a combination of Asian and Australian art patterns and words from international students about their "Melbourne experience".
The two artists, both new to Melbourne, reflect their own cultural heritage through the artwork.
"Our piano represents international students who are also part of Melbourne's community," Ms Li said.
Ms Subhlok said she was excited to see passer-bys play the piano and hear music waft through the CBD's law precinct.
"County Court is such a serious place and it's great to hear some music that can help relieve people's stress," she said.
Play Me, I'm Yours has been touring around the world since 2008, with more than 1850 pianos installed across 55 cities.
The project is the brainchild of British artist Luke Jerram whose original idea was to facilitate more conversation and music in the community.
"Melbourne is such a creative and dynamic city and people can use the piano to express themselves. Some people go on 'piano trials' to play all the pianos they can!" Mr Jerram said.
The project first came to Melbourne in 2014 and this year has more diverse locations across the CBD, Arts Precinct, and suburbs such as Cranbourne and Williamstown.


text:
Q: Creating a list of plots using a for loop I'm having trouble with creating a list of plots using for loops, and I don't know why.
Here's the code that doesn't work (i.e. returns aplotfinal as an empty list)

aplotfinal <- list()
for(i in 1:length(Rlist)){
  a <- Rlist[[i]] %>%
    select(Frame_times, average)
  del <- 0.016667
  x.spec <- spectrum(a$average, log = "no", plot = FALSE)
  spx <- x.spec$freq/del
  spy <- 2*x.spec$spec
  aplotfinal[[i]] <- plot(spy~spx, main = names(Rlist)[i], xlab = "frequency", ylab = "spectral density", type = "l")
}

The plot function works, I just want to apply it for a list of dataframes that I have (i.e. Rlist). Thank you!

A: the base R plot() does not return an object, it just draws on the device. So you have to do a multiplot or save onto a pdf to have a record of the plots.
To store it in a list, I guess you need something like ggplot, for example:
library(ggplot2)
library(gridExtra)

Rlist = lapply(1:5,function(i){
data.frame(Frame_times = seq(0,1,length.out=100),average=runif(100))
})
names(Rlist) = letters[1:5]

aplotfinal <- lapply(1:length(Rlist),function(i){
  a <- Rlist[[i]] %>% select(Frame_times, average)
  del <- 0.016667
  x.spec <- spectrum(a$average, log = "no", plot = FALSE)
  spx <- x.spec$freq/del
  spy <- 2*x.spec$spec
  aplotfinal[[i]] <- qplot(y = spy,x=spx,geom="line") +
  ggtitle(names(Rlist)[i]) +
   xlab("frequency")+ylab("spectral density")
})

grid.arrange(grobs=aplotfinal,ncol=5)

A: Here is an example you can use to tweak your code. Plots get saved to the plot_list variable and then to pdf residing at path/to/pdf. Note that you have to initiate a device first (in my case, pdf).
library(ggplot2)
library(dplyr)

df <- data.frame(country = c(rep('USA',20), rep('Canada',20), rep('Mexico',20)),
                 wave = c(1:20, 1:20, 1:20),
                 par = c(1:20 + 5*runif(20), 21:40 + 10*runif(20), 1:20 + 15*runif(20)))

countries <- unique(df$country)

plot_list <- list()
i <- 1

for (c in countries){
  pl <- ggplot(data = df %>% filter(country == c)) +
    geom_point(aes(wave, par), size = 3, color = 'red') +
    labs(title = as.character(c), x = 'wave', y = 'value') +
    theme_bw(base_size = 16)

  plot_list[[i]] <- pl
  i <- i + 1
}

pdf('path/to/pdf')
pdf.options(width = 9, height = 7)
for (i in 1:length(plot_list)){
  print(plot_list[[i]])
}
dev.off()

redpajama_set_name: RedPajamaStackExchange


From here, click the "Change Header" button and upload an appropriate image from your computer. This is not the background image for your Twitter profile, this is an image to go behind your Header area. If you have not uploaded an image, you will not have a header area. The area only shows up once you have uploaded an image. Be creative with this area. This is the first thing someone will see if they go directly to your Twitter page.


Thanks to its attractively simple shaker lines Petworth comes alive either with the natural warmth and beauty of a Natural Oak finish or when splashed in any one of our painted colours.
A door style for lovers of the natural beauty of timber.
Iconic shaker styling for a timeless look.
Click here to find a display of Petworth near you.


Port State Control inspections has revealed many deficiencies in relation to MARPOL Annex VI, Prevention of Air Pollution from Ships. In response to this we have developed a new on-board training concept to prepare for Port State Control inspections, by raising awareness of the most common defects found on inspections and giving advice on how to avoid them.
Paris MOU deficiencies (https://www.parismou.org/inspection-search/inspection-results-deficiencies) and announcement that Paris MOU will have a concentrated inspection campaign on MARPOL Annex VI in 2018.
This Pocket Guide will be a good guide and tool ensuring your ship complies with MARPOL Annex VI. The module will explain the topic in a simple way with strong focus on what is important related to a port state control. At the end of the module the crew can print out a checklist that will assist them to check compliance with MARPOL Annex VI.
Have a raised awareness of items which are leading to deficiencies being raised on current PSC inspections.


Rug cleaning is best left to professional rug cleaners like RugPro Oriental Rug Cleaning, and, likewise, carpet cleaning is best left to carpet cleaners like First Coast Home Pros. Their technicians are IICRC certified in the most effective carpet cleaning techniques in the industry and their carpet cleaning service is unparalleled in its approach and quality of service.
Because residential carpets are typically made of synthetic fibers, carpet cleaners are able to use far more aggressive cleaning techniques than the techniques that are available to rug cleaners. It is important to know the difference between an effective carpet cleaning process and an effective rug cleaning process. For the very best in professional carpet cleaning services in Jacksonville, FL, we recommend you call First Coast Home Pros.
What Is The Difference Between Carpet Cleaning and Rug Cleaning?
Carpet cleaning and oriental rug cleaning are completely different services. Wall to wall carpeting is best cleaned using the hot water extraction method according to the IICRC. Not so with oriental rugs. This method of cleaning wall to wall carpets, also called steam cleaning, is often advertised by carpet cleaners as their "rug cleaning service." However, this process is nothing more than our maintenance rug cleaning package , which cleans the face yarns only.
This is nothing like our deep rug cleaning or restorative rug cleaning packages . These cleaning process are specifically designed to clean the entire rug front to back, mimicking the flow of a river to do so. This process has been in use for thousands of years, and a carpet cleaning wand could never replicate its deep cleaning results.
Nevertheless, many customers are tempted to just go ahead and have their carpet cleaners clean the rugs while they are there. Unless your rugs need just a maintenance cleaning (which is typically only if you've had your rugs cleaned already within the last 6-12 months), please don't do this! Let rug cleaners clean your rugs, and let carpet cleaners clean your carpets. For the latter, we hope you'll consider First Coast Home Pros' carpet cleaning services.


The Amazing Spiderman sequel. Guardians of the Galaxy. Captain America, Winter Soldier. This summer will be replete with superhero movies on the big screen. Sales of books, cartoons and videos, action figures and other toys, continues apace.
What is it about the superhero that enthralls us?
In some ways, superheroes keep pace with the times. Superman started as fairly modest. He grew up on a planet with high gravity, and therefore was very strong on Earth. He could jump high, fight, flip over cars. As the world became more and more globalized, his enemies grew in stature. In the beginning, he brought cats down from trees and beat up robbers. Later, he thrashed mob bosses and union busters. While he took no part in World War II, he did learn to fly, gained heat-ray vision and eventually became strong enough to lift continents.
In the Brandon Routh iteration, he floated above the Earth listening to millions of human voices crying out for some resolution to their troubles, effectively godlike.
The thing is, we need a Superman right now. Our problems are outstripping not only our ability to fix them but also our ability to know them. Climate change is happening now. The natives of Kiribati are out looking for a new home as their low-lying Pacific islands are sinking under the rising seas. Venice is under several inches of water now each summer for some 100 days. Worse, these changes are escalating, with the most pessimistic views of the data proven right every year. Now we know the Antarctic ice shelf is melting and breaking apart, as is Greenland—potentially surpassing the most pessimistic estimates of ocean raise by a large margin.
Worst still, human activity is responsible for more than climate change. Perhaps the most depressing fact ever reported: saltwater fish are expected to be extinct by 2048. http://www.cbsnews.com/news/salt-water-fish-extinction-seen-by-2048/ Not unless we change our ways, but in most likely any event. Too many tipping points are past at this time.
Where is Superman now? What is it about us that we can turn away from these big issues and wait for some great hero to fix them? This summer, millions of people will go to the theaters to watch imaginary folks solve imaginary problems. If Godzilla is not an allegory for climate change and pollution, I don't know what is. And essentially nobody will take any action.
There isn't a Superman. There is only us. What can we do?
But there is a Lex Luther. Several of them, in fact. Oil companies lobby not just the government but also the citizens to vote their way, and the Koch Brothers could not do more to escalate climate change and pollution if they were actually scheming to destroy the Earth.
Unfortunately, as Jung might have observed, the superhero narrative is archetypal. And Yalom wrote pages and pages about the need for us to join with some admired other, give up our power to them so we can avoid the uncomfortable feeling of responsibility, even if it means ditching freedom. We are also stuck with an inability to digest data because of an evolutionary bias towards experiential and anecdotal evidence. The stories the Kochs tell us in their political advertising resonate much more strongly than the data in the journals.
So we rest in the theater and eat popcorn, watching crises resolved by a few great men.


text:
Investigators: some teens in crash were riding in the trunk
Jun 14, 2018, 7:50 AM | Updated: 11:49 am
BY LINDSAY AERTS
(UPDATED: 11:40 a.m.)
WEBER COUNTY — Investigators say two of the seven teens who were in a car that careened off a steep slope overnight were riding in the trunk of the vehicle.
According to Weber County Sheriff's Lieutenant Matt Jensen, one of those teenagers is now in critical condition. He says the driver of the Honda Accord was a 16-year-old male.
Jensen says investigators believe the driver failed to navigate a right turn on Highway 39, south of the Monte Cristo Campground, launching off the road and landing 180 feet down a ravine, coming to rest upside-down in a tree. Crews had to use a pulley system to get it out.
Sheriff's Sergeant Mark Horton told KSL speed was likely a factor on the winding mountain road, where the limit is 40 miles per hour.
"We're putting the car at 70 plus," Horton says. "One of the occupants was able to crawl up to the roadway to get cell phone service."
Four medical helicopters took four of the teens to local hospitals. The other 3 were taken by ambulance with less serious injuries.
All the teens are from the Ogden area.
Follow @lindsayonair
Simone Seikaly
Taylorsville police have identified 21-year-old Eduardo Moreno Lujan as one of the victims of a shooting in Taylorsville on Monday night.
The Utah Department of Transportation reports that a herd of around 40 elk is stranded on the east bench.
According to Sgt. Cameron Roden with the Utah Highway Patrol, a vehicle entered the interstate going southbound in northbound lanes when it hit another car.


Coffee Table ~ 0515606 Pe639939 S3 Jpg Ikea Coffee Table Tables Console Hemnes Hack Round Black Brown Lack Turned 95 Amazing Ikea Coffee Table. Ikea Lack Coffee Table Parts. Ikea Coffee Table Hemnes. Ikea White Square Coffee Table.


text:
\section{Introduction}
\label{s-intro}

Some of the  most interesting objects in our  Galaxy are close compact
binary  stars, such  as cataclysmic  variables (CVs),  low  mass X-ray
binaries, or  double degenerate white  dwarf (WD) binaries.   The vast
majority of  close compact binaries form through  common envelope (CE)
evolution occurring  when the  more massive star  of the  initial main
sequence binary fills  its Roche-lobe on the first  giant branch (FGB)
or on the asymptotic giant  branch (AGB). This may trigger dynamically
unstable mass transfer causing the giant's envelope to engulf its core
(the  future compact  object) and  the main-sequence  companion.  Drag
forces transfer  orbital energy and  angular momentum from  the binary
orbit  to   the  envelope,  reducing  the   binary  separation,  until
eventually  the  envelope  is  expelled  and a  short  orbital  period
post-common envelope binary (PCEB)  consisting of a compact object and
a main-sequence companion is exposed.

A commonly used method to predict the outcome of binary star evolution
and to theoretically investigate close compact binary star populations
are  Binary  Population  Synthesis   (BPS)  studies  which  have  been
performed     e.g.     for     Supernova    Type     Ia    progenitors
\citep{han+podsiadlowski04-1},     short      gamma     ray     bursts
\citep{belczynskietal06-1}, or  Galactic WD plus  main sequence (WDMS)
binaries \citep{willems+kolb04-1,davisetal10-1}.   However, in current
BPS  models CE evolution  is commonly  approximated by  a parametrized
energy  equation, i.e.  a  fraction of  the available  orbital energy,
known as  the CE efficiency ($\alpha_\mathrm{CE}$), is  equated to the
binding  energy  of  the envelope  \citep{paczynski76-1,  webbink84-1,
  iben+tutukov86-1,  iben+livio93-1}.  While  recent  observational as
well as theoretical results indicate rather small efficiencies for the
use    of   orbital    energy,    i.e.    $\alpha_\mathrm{CE}\sim0.25$
\citep{zorotovicetal10-1, ricker+taam12-1}, it remains unclear if, and
to what  extent, additional energy  sources play an important  role in
unbinding the envelope.

On   the   one   hand,   the   long  orbital   period   PCEB   IK\,Peg
\citep{landsmanetal93-1,  vennesetal98-1}  and  perhaps also  the  two
symbiotic    systems    T\,CrB    \citep{webbink76-1}   and    RS\,Oph
\citep{livioetal86-1} have been claimed to provide direct evidence for
additional       energy       contributions      \citep{davisetal10-1,
  zorotovicetal10-1} and  atomic recombination is  often considered to
be the  most promising candidate  \citep[e.g.][]{webbink07-1}.  On the
other hand,  \citet{soker+harpaz03-1} argue that  recombination energy
cannot significantly contribute to  the ejection process as, according
to  them, the  opacity in  the envelope  is too  small and  the energy
provided  by  recombination  should   be  radiated  away  rather  than
accelerating the gas.

During  the last  few years  we have  successfully identified  a large
number of  PCEBs among WDMS  binaries discovered by the  Sloan Digital
Sky          Survey          \citep[SDSS,][]{adelman-mccarthyetal08-1,
  abazajianetal09-1}, and  measured the orbital periods  of 58 systems
\citep{schreiberetal10-1,                    rebassa-mansergasetal11-1,
  nebotetal11-1}. So far  we have found not a  single system providing
additional direct  evidence for recombination energy  to be important.
As a continuation of this large scale project, we here present orbital
period  measurements   of  the  PCEBs   SDSSJ\,121130.94-024954.4  and
SDSSJ\,222108.45+002927.7      (hereafter     SDSSJ\,1211-0249     and
SDSSJ\,2221+0029, see their  SDSS spectra in Figure\,\ref{f-spec}) and
find these two  systems to be the longest orbital  period PCEBs in our
sample, and  currently the second  and third longest WDMS  PCEBs known
after  IK\,Peg.  We  discuss the  implications of  these  findings for
theories  of CE  evolution with  particular emphasis  on  the possible
contributions  of recombination  energy  to the  energy  budget of  CE
evolution.

\begin{figure}
\includegraphics[angle=-90,width=\columnwidth]{spectrum.ps}
\caption{\label{f-spec} SDSS spectra of SDSSJ\,1211-0249 and
  SDSSJ\,2221+0029.}
\end{figure}

\section{Observations}
\label{s-obs}

We start with a brief summary of the performed spectroscopic follow-up
observations     of     SDSSJ\,1211-0249     and     SDSSJ\,2221+0029.
Instrumentation,  data   reduction  and  calibration   procedures  are
identical to  those described in \citet{nebotetal11-1}.  A  log of the
observations is provided in Table\,\ref{t-log}.

\subsection{SDSSJ\,1211-0249}

\begin{table}
\setlength{\tabcolsep}{2ex}
\caption{\label{t-log}  Log  of  the  observations. Provided  are  the
  telescopes and instruments used,  and the observing dates (observing
  periods  are   provided  for  the   GS  and  VLT   telescopes).  The
  corresponding NTT ESO program ID is 082.D-507(B).}
\begin{center}
\begin{small}
\begin{tabular}{cccc}\hline\hline
Object & Telescope & Instr.  & Date or \\
SDSSJ  &           &         & Obs. Period  \\
\hline
       1211-0249   & GS      & GMOS  & 2008\,A and \,B \\
                   & NTT     & EFOSC & Mar. 17-25 2009\\
                   & M.Baade & IMACS & May 14-16 2009\\
                   & M.Baade & IMACS & Dec. 26-29 2009\\
                   & VLT     & FORS2 & 085.D-0974(A) (2010) \\
                   & VLT     & FORS2 & 087.D-0721(A) (2011) \\
\hline
       2221+0029   & VLT     & FORS2 & 080.D-0407(A) (2007)\\
                   & WHT     & ISIS  & 5-10 Jul. 2008 \\
                   & CA3.5   & TWIN  & 25-28 Jul. 2008 \\
                   & CA3.5   & TWIN  & 24-25 Sep. 2009 \\
                   & VLT     & FORS2 & 085.D-0974(A) (2010) \\
                   & VLT     & FORS2 & 087.D-0721(A) (2011) \\
\hline
\end{tabular}
\end{small}
\end{center}
\end{table}

SDSSJ\,1211-0249  was identified  as a  PCEB  by \citet{nebotetal11-1}
based  on   three  \Lines{Na}{I}{8183.27,8194.81}  absorption  doublet
radial velocities measurements from GMOS spectra taken at Gemini South
(GS)  during  the  semesters  2008\,A  and\,B.   Additional  follow-up
spectroscopy   aiming    to   determine   the    orbital   period   of
SDSSJ\,1211-0249 was  performed at the New  Technology Telescope (NTT)
equipped with EFOSC  during eight consecutive nights. We  took a total
of  18   spectra  providing   radial  velocities  with   rather  large
uncertainties  ($\sim20-30\,  \mbox{$\mathrm{km\,s^{-1}}$}$) due  to  relatively poor  weather
conditions.  This first  data-set revealed  long-term  radial velocity
variations for SDSSJ\,1211-0249. Additional follow-up spectroscopy was
performed at Magellan/Baade armed with  IMACS during two runs of three
and  four nights  respectively,  resulting in  five additional  radial
velocities  revealing a  promising  orbital period  estimate of  about
seven days.  However several aliases resulting  from integer multiples
of  a  day did  not  allow a  definite  determination  of the  orbital
period. Finally, service mode observations at the Very Large Telescope
(VLT)  UT\,1 equipped  with FORS2  in periods  85 and  87  provided 14
additional radial velocities spanning the entire semesters which broke
the  alias degeneracy and  allowed to  accurately measure  the orbital
period.

\subsection{SDSSJ\,2221+0029}

Based  on two  spectra obtained  with  VLT/FORS2 during  period 80  we
discovered    the   close    binary    nature   of    SDSSJ\,2221+0029
\citep{nebotetal11-1}. A  first attempt to measure  the orbital period
was  performed with  ISIS mounted  at the  William  Herschel Telescope
(WHT),  where we  obtained  six  spectra. Given  the  long term  trend
revealed by the  radial velocities derived from these  WHT spectra, we
obtained  seven additional spectra  during two  observing runs  at the
3.5\,m telescope at Calar  Alto (CA\,3.5) equipped with TWIN. However,
as in the case of SDSSJ\,1211-0249, the short time span of our visitor
mode observations provided multiple  choices for the orbital period of
SDSSJ\,2221+0029.   We hence  obtained service  mode  observations (20
spectra)  at the  VLT/FORS2  during  periods 85  and  87 that  finally
allowed   to   unambiguously   determine   the   orbital   period   of
SDSSJ\,2221+0029.

\section{Orbital Periods}
\label{s-porb}

The  data described  in  Section\,\ref{s-obs} allow  us to  accurately
determine    the    orbital    periods   of    SDSSJ\,1211-0249    and
SDSSJ\,2221+0029. Radial  velocities were  measured in all  cases from
the  \Lines{Na}{I}{8183.27,8194.81} absorption  doublet,  in the  same
fashion  as  described  in  \citet[][]{rebassa-mansergasetal08-1}  and
\citet{schreiberetal08-1}. The measured radial velocities are given in
Table\,\ref{t-rvs}.

\begin{figure}
\includegraphics[angle=-90,width=\columnwidth]{curve_1211.ps}
\caption{\label{f-curve1211}  Top panel:  \textsf{ORT/TSA} periodogram
  obtained  from  the  radial  velocity data  of  SDSSJ\,1211-0249  in
  Table\,\ref{t-rvs}.   A   clear  peak  at   0.128\,d$^{-1}$  can  be
  seen. Bottom panel: the radial velocity curve folded over the period
  provided by the periodogram in the top panel.}
\end{figure}

A   \citet{scargle82-1}  periodogram   calculated   from  the   radial
velocities of  SDSSJ\,1211-0249 to investigate the  periodic nature of
the  velocity variations  contained a  number  of aliases  due to  the
sampling  pattern  of  the   visitor  mode  observations.   Using  the
\textsf{ORT/TSA} command in \textsf{MIDAS}, which folds and phase-bins
the data  using a grid of trial  periods and fits a  series of Fourier
terms      to      the      folded     radial      velocity      curve
\citep{schwarzenberg-czerny96-1}, we produced the periodogram shown in
the top panel of  Figure\,\ref{f-curve1211} which reveals a clear peak
at 0.128\,d$^{-1}$.  The same  method applied to the radial velocities
of  SDSSJ\,2221+0029  yields  a  periodogram  with  a  clear  peak  at
0.104\,d$^{-1}$ (top panel of Figure\,\ref{f-curve2221}).

To obtain a definite value  for the orbital periods we finally carried
out sine-fits of the form
\begin{equation}
\label{e-fit}
V_\mathrm{r} =
K_\mathrm{sec}\,\sin\left[\frac{2\pi(t-T_0)}{P_\mathrm{orb}}\right]
+\gamma
\end{equation}
to  the radial  velocity data  sets,  where $\gamma$  is the  systemic
velocity,  $K_\mathrm{sec}$ is the  radial velocity  semi-amplitude of
the companion star,  $T_0$ is the time of  inferior conjunction of the
secondary star, and $P_\mathrm{orb}$ is the orbital period. We adopted
the frequency corresponding to the strongest peaks in the periodograms
as  the initial orbital  period. The  parameters resulting  from these
fits are reported in Table\,~\ref{t-param} with the orbital periods of
SDSSJ\,1211-0249   and  SDSSJ\,2221+0029  being   7.818$\pm$0.002  and
9.588$\pm$0.002  days  respectively.  These  are  the longest  orbital
periods measured so far in our survey.

\begin{table*}
\setlength{\tabcolsep}{0.6ex}
\caption{\label{t-rvs}  \Ion{Na}{I} radial  velocities (RV)  and their
  errors  (RVe) measured  for  SDSSJ\,1211-0249 and  SDSSJ\,2221+0029.
  Heliocentric  Julian  dates  (HJD)  are also  provided.  The  radial
  velocities are given in $\mbox{$\mathrm{km\,s^{-1}}$}$.}
\begin{center}
\begin{small}
\begin{tabular}{ccccccccccccccc}\hline\hline
HJD & RV & RVe & HJD & RV & RVe & HJD & RV & RVe & HJD & RV & RVe & HJD & RV & RVe \\
\hline
SDSSJ1211-0229 & &  & & & & & & & & & & & & \\
 2454510.792206 &   72.5 &   5.6 & 2454642.555408 &   33.0 &   5.7 & 2454644.539962 &   81.7 &   6.6 & 2454911.808350 &   45.1 &  14.1 & 2454915.737374 &   28.6 &  14.9 \\
 2454966.586407 &   27.5 &   8.9 & 2454967.523802 &   29.7 &   7.7 & 2454967.671370 &  -11.7 &   8.6 & 2455192.758500 &   39.9 &  11.4 & 2455195.755007 &    9.2 &  11.9 \\
 2455287.587077 &   17.2 &   4.8 & 2455289.592162 &  -16.9 &   5.0 & 2455291.642618 &   38.1 &   4.6 & 2455293.515465 &   75.1 &   7.5 & 2455295.568011 &   12.8 &   5.2 \\
 2455297.512659 &   -6.2 &   6.1 & 2455299.628209 &   47.6 &   5.1 & 2455306.504832 &   19.4 &   5.9 & 2455660.552464 &   89.4 &  11.5 & 2455665.519683 &   -3.7 &   6.8 \\
 2455671.572157 &   -5.5 &   5.9 & 2455674.596450 &   49.1 &   5.1 & 2455677.712572 &   57.5 &   5.2 & 2455704.665357 &    3.7 &  12.6 &                &        &       \\
\hline
SDSSJ2221+0029 & &  & & & & & & & & & & & & \\
 2454386.661042 &   27.8 &   4.5 & 2454387.598545 &    2.2 &   5.3 & 2454653.712600 &    8.7 &   7.2 & 2454654.647388 &    0.5 &   8.7 & 2454654.719920 &    0.1 &   7.1 \\
 2454655.676768 &    0.5 &   6.6 & 2454656.622337 &   -7.2 &   7.6 & 2454658.677219 &   -3.7 &   5.9 & 2455329.885273 &   -0.1 &   8.3 & 2455334.874227 &    3.2 &   6.0 \\
 2455344.812435 &    6.9 &   7.6 & 2455346.823441 &    2.9 &  13.2 & 2455346.834686 &   -1.7 &  10.0 & 2455346.851469 &    0.7 &  11.3 & 2455346.862695 &   -6.1 &  11.3 \\
 2455354.846936 &    8.0 &   5.3 & 2455357.851973 &   -9.5 &   5.0 & 2455359.794378 &   -4.3 &   5.5 & 2455360.805659 &   -9.0 &   7.6 & 2455382.720068 &    6.1 &   6.4 \\
 2455385.783274 &   -6.3 &   5.0 & 2455399.671028 &   -2.9 &   8.5 & 2455699.895126 &    0.4 &   6.1 & 2455711.878306 &   -5.4 &   9.2 & 2455720.842993 &   -5.4 &   9.0 \\
 2455724.834694 &   -8.9 &   5.8 & 2455736.779456 &    4.4 &   6.5 & 2455741.903011 &   -7.9 &   5.9 & 2454672.643400 &    0.8 &  13.7 & 2454673.556708 &    1.2 &  10.4 \\
 2454674.577014 &    7.5 &  10.7 & 2454675.442195 &   -4.3 &  17.5 & 2454675.641213 &   -7.4 &   6.3 & 2455099.432743 &   -2.0 &   7.1 & 2455100.353820 &   -9.5 &   8.8 \\
\hline
\end{tabular}
\end{small}
\end{center}
\end{table*}
\begin{figure}
\includegraphics[angle=-90,width=\columnwidth]{curve_2221.ps}
\caption{\label{f-curve2221}  Top panel:  \textsf{ORT/TSA} periodogram
  obtained  from  the  radial  velocity data  of  SDSSJ\,2221+0029  in
  Table\,\ref{t-rvs}.   A   clear  peak  at   0.104\,d$^{-1}$  can  be
  seen. Bottom panel: the radial velocity curve folded over the period
  provided by the periodogram in the top panel.}
\end{figure}

\section{Binary parameters}
\label{s-param}

We provide in this Section the binary (orbital and stellar) parameters
of the two PCEBs studied  in this work.  The WD effective temperatures
($\mbox{$T_{\mathrm{eff}}$}_\mathrm{(WD)}$),  surface  gravities ($\log  g_\mathrm{(WD)}$)
and masses  ($M_\mathrm{wd}$), as well as the  secondary star spectral
types   (Sp$_\mathrm{sec}$),   masses   and  radii   ($M_\mathrm{sec},
R_\mathrm{sec}$)  are  obtained  following  the  decomposition/fitting
technique  described in  \citet{rebassa-mansergasetal07-1}.   In brief
this routine  follows a two-step procedure.  First,  the SDSS spectrum
is fitted  with a  two-component model, and  the spectral type  of the
secondary  star is  determined (Figure\,\ref{f-rdfits}).   Second, the
best-fit M-dwarf is subtracted and  the residual WD spectrum is fitted
with a  model grid of DA  WDs \citep{koester10-1} to  determine the WD
effective  temperature and  surface  gravity (Figure\,\ref{f-wdfits}).
From  an  empirical spectral  type-radius-mass  relation for  M-dwarfs
\citep{rebassa-mansergasetal07-1} and  a mass-radius relation  for WDs
\citep{bergeronetal95-2,fontaineetal01-1}  we then calculate  the mass
and radius of the secondary star and the WD respectively.

For the majority of SDSS PCEBs the spectroscopic decomposition results
in an  uncertainty of the  spectral type of $\pm0.5$  spectral classes
\citep{rebassa-mansergasetal10-1, rebassa-mansergasetal12-1}, and this
applies as  well to SDSS\,J2221+0029.   However, the SDSS  spectrum of
SDSS\,J1211-0249  suffers  from   low-frequency  structure  (there  is
substantial  structure left  in  the residual  WD  spectrum after  the
decomposition) that  results in  a substantially larger  uncertainty in
the  determination  of  the   spectral  type  of  the  companion,  and
correspondingly  larger uncertainties  in the  white  dwarf parameters
(see      left      panels      of     Figure\,\ref{f-wdfits}      and
Table\,\ref{t-param}).    For    SDSS\,J2221+0029,    $M_\mathrm{wd}$,
$\mbox{$T_{\mathrm{eff}}$}_\mathrm{(WD)}$,  $\log  g_\mathrm{(WD)}$, $M_\mathrm{sec}$  and
Sp$_\mathrm{sec}$  are obtained by  averaging the  fit results  of two
independent SDSS spectra, and  the uncertainties are the corresponding
standard deviations.  For  SDSS\,J1211-0249, we average the parameters
over  two  possible solutions  for  the  spectral decomposition  using
either an  M2 or  M3 template, and  determine the  uncertainties again
from the corresponding standard deviations.

\begin{figure*}
\includegraphics[angle=-90,width=\columnwidth]{SDSSJ121130.94-024954.4_fit.ps}
\includegraphics[angle=-90,width=\columnwidth]{SDSSJ222108.45+002927.7_fit.ps}
\caption{Two-component fit  to the spectra  of SDSSJ\,1211+0249 (left)
  and SDSSJ\,2221+0029 (right). The top panels show the spectra of the
  objects as  a solid black lines  and the two  templates, white dwarf
  and M-dwarf, as  dotted lines. The bottom panel  shows the residuals
  from  the  fit.  SDSS  MJD,   PLT  and  FIB  identifiers  are  also
  indicated.}
  \label{f-rdfits}
\end{figure*}

\begin{figure*}
\includegraphics[width=84mm]{SDSSJ121130.94-024954.4_wdfit.ps}
\includegraphics[width=84mm]{SDSSJ222108.45+002927.7_wdfit.ps}
\caption{Spectral model fit to the white dwarf in SDSSJ\,1211+0249 and
  SDSSJ\,2221+0029,  obtained after  subtracting the  best-fit M-dwarf
  templates  (see Figure\,\ref{f-rdfits}).  Top left  panels: best-fit
  (black    lines)    to    the    observed    $\mathrm{H}\beta$    to
  $\mathrm{H}\epsilon$ (gray lines, top  to bottom) line profiles. The
  model  spectra and  observations have  been normalised  in  the same
  way. Top  right panels:  1, 2 and  3\,$\sigma$ contour plots  in the
  \mbox{$T_{\mathrm{eff}}$}-$\log  g$ plane.  The black  contours refer  to the  best line
  profile fit, the red ones (which collapse into a dot on the scale of
  the  plot) to  the fit  of the  spectral range  3850--7150\,\AA. The
  dashed  line indicates the  occurrence of  maximum $\mathrm{H}\beta$
  equivalent  width.  The  best  ``hot''  and  ``cold''  line  profile
  solutions are  indicated by  black dots, while  the best fit  to the
  whole spectrum by a red one. Bottom panels: the residual white dwarf
  spectra  resulting from  the spectral  decomposition and  their flux
  errors (gray lines) along with the best-fit white dwarf model (black
  lines)  in  the  3850--7150\,\AA\  wavelength range  (top)  and  the
  residuals of the fit (gray line, bottom).}
  \label{f-wdfits}
\end{figure*}

To calculate the binary inclinations we use Kepler's third law,
\begin{equation}
\frac{(M_\mathrm{wd}\sin i)^3}{(M_\mathrm{wd}+M_\mathrm{sec})^2}
=\frac{\mbox{$P_{\mathrm{orb}}$} K_\mathrm{sec}^3}{2\pi G}
\end{equation}
\noindent rewritten as
\begin{equation}
\sin i = \frac{K_\mathrm{sec}}{M_\mathrm{wd}} \left(\frac{\mbox{$P_{\mathrm{orb}}$}}
{2\pi G}\right)^{1/3}(M_\mathrm{wd}+M_\mathrm{sec})^{2/3},
\label{e-incl}
\end{equation}
\noindent
with  the  orbital  periods   and  semi-amplitude  velocities  of  the
companions  $K_\mathrm{sec}$ as  determined  in Section\,\ref{s-porb},
and  the stellar  masses as  obtained from  the analysis  of  the SDSS
spectra     outlined    above.      The     well    known     relation
$M_\mathrm{sec}/M_\mathrm{wd}     =    K_\mathrm{wd}/K_\mathrm{sec}=q$
provides an estimate of the expected semi-amplitude velocity of the WD
$K_\mathrm{wd}$.   Finally, estimates of  the orbital  separations and
Roche lobe radii of the secondary stars $R_\mathrm{L\mathrm{sec}}$ are
obtained     from     Kepler's     third    law     and     Eggleton's
(\citeyear{eggleton83-1}) expression
\begin{equation}
R_\mathrm{L\mathrm{sec}} = \frac{a\,0.49\,q^{2/3}}
{0.6\,q^{2/3} + \ln(1+q^{1/3})}
\label{e-rl}
\end{equation}
respectively.    The   complete   sets   of  binary   parameters   for
SDSSJ\,1211-0249     and     SDSSJ\,2221+0029     are     given     in
Table\,\ref{t-param}.

\begin{table}
\caption{\label{t-param}     Binary     parameters    obtained     for
  SDSSJ\,1211-0249     and     SDSSJ\,2221+0029.      $M_\mathrm{wd}$,
  $M_\mathrm{sec}$, $R_\mathrm{sec}$,  spectral type of  the companion
  Sp$_\mathrm{sec}$, $\mbox{$T_{\mathrm{eff}}$}_\mathrm{(WD)}$\, and $\log g$ are obtained
  following    the   decomposition/fitting   routine    described   in
  \citet{rebassa-mansergasetal07-1}.   The orbital  period  \mbox{$P_{\mathrm{orb}}$}, the
  secondary  star semi-amplitude  $K_\mathrm{sec}$,  and the  systemic
  velocity       $\gamma_\mathrm{sec}$      are       measured      in
  Section\,\ref{s-porb}.   Estimates of  the  orbital separation  $a$,
  mass ratio $q$, white dwarf semi-amplitude velocity $K_\mathrm{wd}$,
  secondary   Roche  lobe   radius   R$_\mathrm{L_\mathrm{sec}}$,  and
  inclination   are    obtained   from   the    equations   given   in
  Section\,\ref{s-param}.}
\begin{flushleft}
\begin{center}
\setlength{\tabcolsep}{0.9ex}
\begin{tabular}{llcccccc}
\hline\hline
\noalign{\smallskip}
 & &\multicolumn{3}{c}{SDSS\,J1211--0229}  & \multicolumn{3}{c}{SDSS\,J2221+0029}\\
\hline
$M_\mathrm{wd} [M_\odot]$                  &&    0.52&$\pm$&0.07    &   0.54&$\pm$&0.03\\
$M_\mathrm{sec} [M_\odot]$                 & &   0.41&$\pm$&0.05  &   0.38&$\pm$&0.07\\
$q$                                      &&    0.79&$\pm$&0.15    &   0.70&$\pm$&0.15 \\
$a [R_\odot]$                             &&    16.2&$\pm$&0.5    &   18.5&$\pm$&0.5 \\
\mbox{$P_{\mathrm{orb}}$}\ [d]                               &&  7.818&$\pm$&0.002  & 9.588&$\pm$&0.002\\
$\gamma_\mathrm{sec} [\mbox{$\mathrm{km\,s^{-1}}$}]$              &&     30&$\pm$&2       &  -29&$\pm$&2    \\
$K_\mathrm{sec} [\mbox{$\mathrm{km\,s^{-1}}$}]$                   &&     44&$\pm$& 3     &   49&$\pm$& 2  \\
$K_\mathrm{wd} [\mbox{$\mathrm{km\,s^{-1}}$}]$                    &&     35&$\pm$& 7     &    34&$\pm$& 7 \\
Sp$_\mathrm{sec}$                          &&     M2.5&$\pm$& 1   &   M3&$\pm$& 0.5\\
$R_\mathrm{sec} [R_\odot]$                 &&   0.42&$\pm$&0.05   &  0.39&$\pm$&0.08\\
$R_\mathrm{sec}/R_\mathrm{L\mathrm{sec}}$  & &   0.07&$\pm$&0.01    &   0.06&$\pm$&0.01    \\
$i [^\circ]$                               &&     49&$\pm$& 7     &    58&$\pm$& 7    \\
$\mbox{$T_{\mathrm{eff}}$}_\mathrm{(WD)}$ [K]                   &&  13130&$\pm$&860   & 18440&$\pm$&150 \\
$\log g_\mathrm{(WD)}$                      &&    7.84&$\pm$&0.13    &   7.85&$\pm$&0.06  \\
\hline
\noalign{\smallskip}
\end{tabular}
\end{center}
\end{flushleft}
\end{table}

\section{Discussion}
\label{s-disc}

We have presented in the previous Sections the discovery of the second
and  third longest  orbital period  (detached) PCEBs  containing  a WD
primary. In  what follows we  reconstruct the evolutionary  history of
both  systems and  discuss implications  for our  understanding  of CE
evolution.

\subsection{The evolution of SDSSJ\,1211-0249 and SDSSJ\,2221+0029}
\label{s-evol}

Having at hand the orbital periods, the stellar mass estimates of both
components and the WD  effective temperatures allows us to reconstruct
the evolutionary history  of SDSSJ\,1211-0249 and SDSSJ\,2221+0029 and
predict   their   future   following   \citet{zorotovicetal11-1}   and
\citet{schreiber+gaensicke03-1}  respectively.  First,  we interpolate
the       cooling      tracks       of       \citet{wood95-1}      and
\citet{althaus+benvenuto97-1}  to determine  the cooling  age  of both
systems. Second,  we derive the  orbital period at  the end of  the CE
phase  using the  the most  up-to-date version  of  disrupted magnetic
braking    \citep[][including    the    normalization   provided    by
  \citealt{davisetal08-1}]{hurleyetal02-1}.    Third,   we   use   the
single-star   evolution  (SSE)   code  of   \citet{hurleyetal00-1}  to
reconstruct the  CE phase for a  given value of the  CE efficiency and
obtain the orbital and stellar parameters prior to CE evolution.

We  here  follow   \citet{zorotovicetal10-1}  and  \emph{assume}  that
recombination energy  contributes to  expelling the envelope  with the
same    efficiency     as    the    orbital     energy    (given    by
$\alpha_{\mathrm{CE}}$) and take into account the uncertainties in the
stellar  component masses  and WD  effective temperatures.   We obtain
solutions  for rather  large  ranges  of the  CE  efficiency for  both
systems that are  given together with the resulting  range of possible
parameters and  evolutionary time scales  of the progenitor  system in
Table\,\ref{tab:reco}.  As  outlined in the  introduction, there seems
to  be some  evidence  for a  relatively  small CE  efficiency and  we
therefore  additionally  provide  the progenitor  parameters  assuming
$\alpha_{\mathrm{CE}}=0.25$      in     Table\,\ref{tab:reco}     (the
uncertainties of  the stellar masses and WD  effective temperature are
not  considered  here).  This  complements  the  results presented  in
\citealt{zorotovicetal11-1}  (their  Table\,3).  Given  that  magnetic
braking is not  efficient in long orbital period  systems, the current
orbital periods  (Table\,\ref{t-param}) are nearly  identical to those
at  the  end  of  the  CE  phase.  The  masses  of  the  reconstructed
progenitors  for both  objects are  similar, which  is  not surprising
since the available estimates of  the stellar masses are quite similar
too.

Since   the   current   orbital   periods  of   SDSSJ\,1211-0249   and
SDSSJ\,2221+0029 are very long  for PCEBs, the stellar components will
not  be close  enough to  trigger the  second phase  of  mass transfer
before  the secondaries  in both  systems  evolve away  from the  main
sequence.   Both secondaries  will  therefore fill  their Roche  lobes
during the FGB transforming SDSSJ\,1211-0249 and SDSSJ\,2221+0029 into
symbiotic  systems with stable  mass transfer  from a  red giant  to a
white dwarf. This is supposed to  happen in many Hubble times when the
orbital periods have shrunk to $\sim1-1.5$\,days.

\begin{table}
\caption{\label{tab:reco}   Applying   the  reconstruction   algorithm
  described  in  \citet{zorotovicetal11-1}  we determine  the  orbital
  periods at  the end of  CE evolution $P_{\mathrm{CE}}$,  the initial
  mass of the  primary $M_{\mathrm{1,o}}$, the mass of  the primary at
  the  onset of  CE evolution  $M_{\mathrm{1,CE}}$,  the corresponding
  orbital separation  $a_{\mathrm{i}}$, the main  sequence lifetime of
  the  primary  $t_{\mathrm{evolv}}$,  the   cooling  age  of  the  WD
  $t_{\mathrm{cool}}$,  and the time  until the  second phase  of mass
  transfer  will occur  from now  on $t_{\mathrm{sd}}$  and  since the
  progenitor  main  sequence  binary  has  formed  $t_{\mathrm{tot}}$.
  Columns   two   and   four   correspond   to  a   fixed   value   of
  $\alpha_{\mathrm{CE}}=0.25$.  Columns three and five give the entire
  range  of possible  solutions.  Note  that since  disrupted magnetic
  braking  is  very  inefficient  for  long  orbital  period  systems,
  $P_{\mathrm{CE}}$    is    nearly    identical   to    \mbox{$P_{\mathrm{orb}}$}\,    in
  Table\,\ref{t-param}. }
\begin{flushleft}
\begin{center}
\setlength{\tabcolsep}{1.6ex}
\begin{tabular}{llcccccccc}
\hline\hline
\noalign{\smallskip}
                    & \multicolumn{4}{c}{SDSS\,J1211--0229} &\multicolumn{4}{c}{SDSS\,J2221+0029}\\
\hline
$\alpha_{\mathrm{CE}}$ & \multicolumn{3}{c}{0.25} & 0.03-1 & \multicolumn{3}{c}{0.25} & 0.06-1\\
\hline
$P_{\mathrm{CE}}$ [d]        & \multicolumn{3}{c}{7.820} & 7.819-7.822 & \multicolumn{3}{c}{9.589} & 9.588-9.589\\
$M_{\mathrm{1,o}} [M_\odot]$  & \multicolumn{3}{c}{1.31} & 0.98-2.35    & \multicolumn{3}{c}{1.44} & 1.31-2.35\\
$M_{\mathrm{1,CE}} [M_\odot]$ & \multicolumn{3}{c}{1.1} & 0.8-2.3     & \multicolumn{3}{c}{1.2} & 1.0-2.3\\
$a_{\mathrm{i}} [R_\odot]$    & \multicolumn{3}{c}{480.8} & 246.2-613.9 & \multicolumn{3}{c}{512.2} & 295.5-611.3 \\
$P_{\mathrm{sd}}$ [h]       & \multicolumn{3}{c}{26.0} & 24.0-28.2    & \multicolumn{3}{c}{32.0} & 28.9-36.0 \\
$t_{\mathrm{evolv}}$ [Gyr]    & \multicolumn{3}{c}{4.82} & 0.95-13.29   & \multicolumn{3}{c}{3.53} & 0.95-4.82  \\
$t_{\mathrm{cool}}$ [Gyr]    & \multicolumn{3}{c}{0.24} & 0.24-0.43    & \multicolumn{3}{c}{0.08} & 0.07-0.09 \\
$t_{\mathrm{sd}}$ [Gyr]      & \multicolumn{3}{c}{225.3} & 140.1-339.7 & \multicolumn{3}{c}{268.5} & 150.13-454.36 \\
$t_{\mathrm{tot}}$ [Gyr]     & \multicolumn{3}{c}{230.4} & 141.3-353.4 &\multicolumn{3}{c}{272.1} & 151.15-459.27\\
\hline
\noalign{\smallskip}
\end{tabular}
\end{center}
\end{flushleft}
\end{table}

\subsection{The energy budget of CE evolution}
\label{s-budget}

In  their  review,   \citet{iben+livio93-1}  describe  several  energy
sources apart  from orbital energy that might  contribute to expelling
the  envelope,  ranging  from  recombination  energy  to  dust  driven
winds. Since  the writing  of this review,  the energy equation  of CE
evolution  in  general, and  especially  the  potential importance  of
recombination    energy,    has    been    a    matter    of    debate
\citep[e.g.][]{dewi+tauris00-1,         webbink07-1,        xu+li10-1,
  loveridgeetal11-1, soker+harpaz03-1, zorotovicetal10-1}.

In the  previous Section  we reconstructed the  evolution of  the long
orbital    period   PCEBs   SDSSJ\,1211-0249    and   SDSSJ\,2221+0029
{\em{assuming}} that recombination energy contributes to expelling the
envelope  with the  same efficiency  as the  orbital energy  and found
large ranges of possible  solutions.  Here we investigate whether this
assumed additional energy is  a necessary ingredient to understand the
evolutionary  history of  SDSSJ\,1211-0249  and SDSSJ\,2221+0029.   To
that  end we  now reconstruct  the CE  phase of  both  systems without
considering recombination energy.  Taking into account the uncertainty
of the  measured stellar parameters, we find  possible progenitors for
both   systems    without   violating   energy    conservation,   i.e.
$\alpha_{\mathrm{CE}}=0.21-1$       for      SDSSJ\,1211-0249      and
$\alpha_{\mathrm{CE}}=0.42-1$  for   SDSSJ\,2221+0029.   We  therefore
conclude that  the existence  of the two  systems does not  confirm or
disprove whether recombination (or  any other additional) energy plays
an  important  role  during   the  CE  phase.   However,  the  current
configuration  of   SDSSJ\,2221+0029  can  only  be   explained  if  a
relatively large  fraction of the released  orbital energy contributes
to  envelope ejection,  i.e.   $\alpha_\mathrm{CE}>0.42$.  This  value
exceeds the  estimates given  in recent studies  of CE  evolution that
seem     to     converge     towards     a    CE     efficiency     of
$\alpha_{\mathrm{CE}}\sim0.25$                \citep{zorotovicetal10-1,
  ricker+taam12-1,  passyetal12-1}.   If this  is  generally true,  at
least a small  fraction of recombination energy (or  any other form of
additional energy) seems to  have contributed to the envelope ejection
in SDSSJ\,2221+0029.   Although this interpretation  appears tempting,
the fact  remains that not a  single PCEB within  the homogeneous SDSS
sample  \citep{nebotetal11-1}   provides  {\em{direct}}  evidence  for
additional sources of energy playing a role during CE evolution.

\subsection{Future perspectives}
\label{s-future}

IK\,Peg has  been highlighted  as a  key object as  it is  the longest
orbital  period system and  contains the  most massive  secondary star
among  the known  PCEBs  containing  a white  dwarf  primary.  IK  Peg
requires  extra energy  that helps  to  expel the  envelope during  CE
evolution  \citep[e.g.][]{davisetal10-1}.  Indeed,  IK\,Peg  cannot be
reconstructed unless at least a small fraction of recombination energy
is  taken  into  account  \citep{zorotovicetal10-1}.  In  contrast  to
IK\,Peg   the   two  PCEBs   discussed   here,  SDSSJ\,1211-0249   and
SDSSJ\,2221+0029,    contain   relatively   low-mass    C/O-core   WDs
(Table\,\ref{t-param}), therefore their progenitors filled their Roche
lobes early on the AGB, i.e.  when the envelope was not very extended.
Recombination energy,  however, is expected to be  most important when
the WD  progenitor radius is large  and the envelope  is loosely bound
\citep{webbink07-1}. The peculiarity of  IK\,Peg is therefore not only
its  long orbital  period but  also  the high  mass of  its WD,  which
implies that  the system entered the  CE phase when the  radius of the
primary was very large on the  AGB, a peculiarity our two PCEBs do not
share.

\begin{figure}
\includegraphics[angle=-90,width=\columnwidth]{M1P.ps} \caption{\label{fig:M1P}
  Maximum orbital period versus WD mass assuming a secondary star mass
  of $\mbox{$M_\mathrm{sec}$}=0.4$ (black lines) $\pm0.1\mbox{$\mathrm{M}_{\odot}$}$ (gray lines).  The dashed
  lines correspond to the  maximum orbital period if all recombination
  energy goes  into CE  ejection, while the  solid lines  provides the
  same limit  but without  taking into account  possible contributions
  from recombination.  Any system  located between the two lines would
  provide  direct  evidence  for  the contributions  of  recombination
  energy.  The difference between both  lines is largest for high mass
  WDs as the relative  importance of recombination energy increases on
  the AGB.  So  far all PCEBs in the homogeneous  SDSS sample lie well
  below  the solid lines.   Note that  the exact  location of  the two
  lines depends  on the secondary  star mass. PCEBs with  more massive
  secondaries have  more orbital energy  available and the  limits are
  hence slightly shifted towards longer orbital periods. }
\end{figure}

To  predict which  kind  of  PCEBs would  provide  the desired  direct
evidence for  contributions of recombination  energy we once  more use
the  reconstruction algorithm described  in \citet{zorotovicetal11-1}.
As usual we assume  that the WD mass is equal to  the core mass of the
giant progenitor at the onset  of mass transfer and that the secondary
star mass remains constant during CE evolution.  For a given core mass
we  use the  SSE  code from  \citet{hurleyetal00-1}  to calculate  all
possible  progenitor masses  and their  radii.  As  the radius  of the
progenitor must have been equal to the Roche radius at the onset of CE
evolution we obtain  the initial separation for given  white dwarf and
main sequence  companion masses, leaving the final  orbital period and
the CE efficiency  as the remaining free parameters  connected via the
energy  equation.    For  each  progenitor  mass   the  solution  with
$\alpha_\mathrm{CE}  \simeq 1.0$ corresponds  to the  longest possible
final orbital  period not violating energy  conservation.  Among these
possible solutions  we finally can  select the maximum  orbital period
for a given combination of white dwarf and secondary star masses.

In Figure\,\ref{fig:M1P}  we show  the resulting PCEB  maximum orbital
period as a  function of WD mass assuming a  fixed secondary star mass
of  $\mbox{$M_\mathrm{sec}$}=0.4\pm0.1\mbox{$\mathrm{M}_{\odot}$}$.   The  positions of  SDSSJ\,1211-0249  and
SDSSJ\,2221+0029 are indicated by  black solid dots.  The dashed lines
have been  obtained by assuming  that all the  available recombination
energy goes into envelope ejection while the solid lines represent the
maximum  orbital period  if the  envelope is  expelled by  the  use of
orbital  energy only.   The upper  and lower  (solid and  dashed) gray
lines    correspond   to    $\mbox{$M_\mathrm{sec}$}=0.5\mbox{$\mathrm{M}_{\odot}$}$    and   $\mbox{$M_\mathrm{sec}$}=0.3\mbox{$\mathrm{M}_{\odot}$}$
respectively.  The  orbital period limits increase  with the secondary
star  mass  because PCEBs  with  more  massive  secondaries have  more
orbital energy available.

Any PCEB located above the  solid line in Figure\,\ref{fig:M1P} (for a
given  secondary   star  mass)  would  provide   direct  evidence  for
contributions of additional energy sources.  Apparently, recombination
energy as  the most likely extra-energy  can only be  important on the
tip   of   the   FGB  and   on   the   AGB   (see  dashed   lines   in
Figure\,\ref{fig:M1P}).  For high  mass WDs ($\mbox{$M_\mathrm{wd}$}\gappr0.8\mbox{$\mathrm{M}_{\odot}$}$) the
range of orbital periods that would provide evidence for recombination
energy  is significantly shifted  towards shorter  (easily measurable)
orbital periods  of a few  days.  However, so  far not a  single known
PCEB  apart  from  IK\,Peg   has  a  relatively  long  orbital  period
\emph{and}  contains  a  high-mass  WD.   The seven  SDSS  PCEBs  with
accurately   determined  orbital   periods   and  stellar   parameters
containing massive  WDs ($\geq0.8\mbox{$\mathrm{M}_{\odot}$}$) have  orbital periods shorter
than  one  day (see  Table\,3  in \citealt{zorotovicetal11-1}).   This
might further indicate that the fraction of recombination energy going
into  envelope  ejection  is  small.  However,  further  observational
constraints  are  required  to  confirm  this  supposition.   We  have
therefore  just  started  an  observing campaign  to  measure  orbital
periods  of  additional SDSS  PCEBs  with  $\mbox{$M_\mathrm{wd}$}  \raisebox{-0.4ex}{$\gppr$} 0.8\mbox{$\mathrm{M}_{\odot}$}$  to
further  constrain the  importance of  recombination energy  during CE
evolution.   The  secondary star  masses  of  the  PCEBs in  our  SDSS
follow-up project  are mostly in the  range of $\mbox{$M_\mathrm{sec}$}\sim0.2-0.4\mbox{$\mathrm{M}_{\odot}$}$
which corresponds  to orbital period limits  given by the  full use of
orbital  energy  of   $\sim\,1-3$  days  (see  Figure\,\ref{fig:M1P}).
Direct evidence for additional energy, most likely from recombination,
would  be provided if  at least  one system  will be  found to  have a
period exceeding  this limit.  If in  contrast no such  system will be
detected, the contribution of recombination energy during CE evolution
is likely of minor importance.

\section{Conclusion}
\label{s-concl}

We  have   measured  the  orbital  periods   of  SDSSJ\,1211-0249  and
SDSSJ\,2221+0029  to  be   7.818$\pm$0.002  and  9.588$\pm$0.002  days
respectively.   This  makes  them  the longest  orbital  period  PCEBs
containing a  WD primary  and main sequence  companion after  the well
known record holder IK\,Peg. We reconstructed the CE evolution of both
systems  taking  into  account  and  ignoring  additional  sources  of
energy. Although no direct evidence for contributions of recombination
energy during CE  evolution is provided, it appears  plausible that at
least a small  fraction of this energy helped  expelling the envelope.
Measuring  the  orbital periods  of  more  PCEBs containing  high-mass
($\mbox{$M_\mathrm{wd}$} \raisebox{-0.4ex}{$\gppr$}  0.8\mbox{$\mathrm{M}_{\odot}$}$) WDs will provide further  constraints on the
importance of recombination energy during CE evolution.

\section*{Acknowledgments}

ARM acknowledges financial support from  Fondecyt in the form of grant
number  3110049.  MZ acknowledges  support from  Gemini/Conicyt, grant
number  32100026.   MRS  acknowledges  support from  Milenium  Science
Initiative,  Chilean  Ministry  of  Economy,  Nucleus  P10-022-F,  and
Fondecyt (1061199).  ANGM acknowledges  support by the Centre National
d'Etudes Spatial  (CNES, ref.  60015).  This project  was supported in
part  by the  DFHG under  contract  Schw536/33-1.  We  also thank  the
anonymous referee  for his/her  suggestions that helped  improving the
quality of the paper.

The presented research is based on observations collected at the
following telescopes: the European Organisation for Astronomical
Research in the Southern Hemisphere, Chile (080.D-0407(A),
082.D-0507(B)) 085.D-0974(A), 087.D-0721(A));
the  Gemini Observatory, which is operated  by the Association of
Universities for
Research in  Astronomy, Inc., under  a cooperative agreement  with the
NSF  on  behalf  of  the  Gemini  partnership:  the  National  Science
Foundation  (United  States), the  Science  and Technology  Facilities
Council  (United  Kingdom), the  National  Research Council  (Canada),
CONICYT   (Chile),  the   Australian  Research   Council  (Australia),
Minist\'erio  da Ci\'encia  e  Tecnologia (Brazil)  and Ministerio  de
Ciencia,   Tecnolog\'ia    e   Innovaci\'on   Productiva   (Argentina)
(GS-2008A-Q-31, GS-2008B-Q-40);
the Magellan Baade  Telescope located
at Las  Campanas Observatory,  Chile;
the William  Herschel Telescope,
operated on  the island of La Palma  by the Isaac Newton  Group in the
Spanish Observatorio  del Roque de  los Muchachos of the  Instituto de
Astrof\'isica  de Canarias;
and at  the Centro  Astron\'omico Hispano
Alem\'an  (CAHA) at  Calar Alto,  operated jointly  by  the Max-Planck
Institut  f\"ur  Astronomie  and  the Instituto  de  Astrof\'isica  de
Andaluc\'ia.

redpajama_set_name: RedPajamaArXiv


Long Bets is a web site where you can bet money on your own or others predictions. All winnings are donated to a charity of the winner's choice. This page describes how to make a bet.
Here are some of the predictions on Long Bets.
By 2007, the U.S. Government will intervene to prevent at least one of the Incumbent Local Exchange Carriers (ILECs)/Regional Bell Operating Companines (RBOCs) (e.g. Verizon, SBC, Bell South, and EXCEPTING Qwest) from filing for Chapter 11 bankruptcy protection.
By 2100 a world government will be in place and in control of: business law, environmental law, and weapons of mass destruction.
By the year 2020 solar electricity will be as cheap or cheaper than that produced by fossil fuels.


Your child's friends are coming for a sleepover, and you want to keep them occupied and away from your flat screen TV. What do you do? One way to keep them distracted is to make a delicious snack, so that they know which friend's parent makes the best snacks. Here are an assortment of sleepover ideas and recipes you can serve to the army of children that have invaded your home.
Would you like to make a quick and cool sleepover snack, while also subtly poking fun at your child's friends? Make them some toasted malt nuts! Crazy kids deserve a crazy snack, and this quick recipe can be served up in just ten minutes. All you need to do is add some of CTL Foods's Soda Fountain Malted Milk Powder to some nuts, put them in the oven, and if you like, you can even add some candy to the mix afterwards. Just make sure you save yourself some.
While protecting your valuables, you may find yourself becoming nostalgic for the days when you were a child and had friends over. The best sleepovers were always the ones where your family went out of the way to make sure these were special occasions, so why not do the same for your child? Malty chocolate chip cookies are a classic with a twist, as the Soda Fountain Malted Milk Powder really shakes things up. The children infesting your home are sure to be astounded by the richness of these tasty treasures. Again, make sure they don't eat them all.
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So it's the next day, everyone is getting ready to go home, and you want to remind everyone who is the cool parent to rule all cool parents. One goodie to end the sleepover with is this scrumptious DIY sleepover malt pancake recipe. All you have to do is make your usual pancakes, and just add some of CTL Foods's Soda Fountain Malted Milk Powder. Yeah, it's that easy. Now that that ordeal is over, allow yourself to relax, and make sure your kid actually cleans up whatever mess is left. Also, eat some pancakes, because you remembered to save yourself some, right?


text:
package com.haulmont.cuba.gui.sys;

import com.haulmont.cuba.gui.Dialogs;
import com.haulmont.cuba.gui.Fragments;
import com.haulmont.cuba.gui.Notifications;
import com.haulmont.cuba.gui.Screens;
import com.haulmont.cuba.gui.config.WindowInfo;
import com.haulmont.cuba.gui.screen.ScreenContext;
import com.haulmont.cuba.gui.screen.ScreenOptions;

public class ScreenContextImpl implements ScreenContext {

    protected final ScreenOptions options;
    protected final WindowInfo windowInfo;

    protected final Screens screens;
    protected final Dialogs dialogs;
    protected final Notifications notifications;
    protected final Fragments fragments;

    public ScreenContextImpl(WindowInfo windowInfo, ScreenOptions options,
                             Screens screens, Dialogs dialogs, Notifications notifications, Fragments fragments) {
        this.windowInfo = windowInfo;
        this.options = options;

        this.screens = screens;
        this.dialogs = dialogs;
        this.notifications = notifications;
        this.fragments = fragments;
    }

    @Override
    public ScreenOptions getScreenOptions() {
        return options;
    }

    @Override
    public WindowInfo getWindowInfo() {
        return windowInfo;
    }

    @Override
    public Screens getScreens() {
        return screens;
    }

    @Override
    public Dialogs getDialogs() {
        return dialogs;
    }

    @Override
    public Notifications getNotifications() {
        return notifications;
    }

    @Override
    public Fragments getFragments() {
        return fragments;
    }
}

redpajama_set_name: RedPajamaGithub


Thank you to Sandy Gerencer and her very cute Palomino mare for letting me capture the special bond between the two of you. You were both full of energy and excitement, it was great seeing the both of you having such a great time in each other's company.
Because of some limitations in the setting, I felt it was a great opportunity to work on a lot of close up work, as I truly believe that it is essential in every Equestrian Photographer's portfolio.


text:
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Chapman expects to be ready by March 20
Third baseman to be limited in Spring Training after shoulder surgery
By Jane Lee
MESA, Ariz. -- A's star third baseman Matt Chapman will be slowed by ongoing rehab this spring, but don't count him out from the club's March 20 regular-season opener against the Mariners in Tokyo."I know I'll be ready by the season," Chapman said Sunday.:: Spring Training coverage presented by Camping
MESA, Ariz. -- A's star third baseman Matt Chapman will be slowed by ongoing rehab this spring, but don't count him out from the club's March 20 regular-season opener against the Mariners in Tokyo.
"I know I'll be ready by the season," Chapman said Sunday.
The Platinum Glove Award-winning infielder succumbed to two minor operations this winter; he had surgery on his right thumb in October, then underwent a procedure to alleviate issues with the AC joint in his left shoulder in December.
Chapman is still recovering from the latter and, like last spring, when he was bothered by his thumb, won't appear in preseason games right away. His thumb has since been fixed by the surgery, but his shoulder is still limiting his activity. Chapman is already taking grounders and throwing, but he remains on a swinging progression and hopes to start hitting overhand tosses next week.
• Prospect Kaprielian experiences lat discomfort
"It's hard to say when everything is going to be full-go," he said, "but working every day to get better. All depends on how everything from here on out goes, but the way it's looking I'll be not too far behind everyone else.
"I'm kinda putting myself back together this offseason. Not exactly how you'd draw it up."
Chapman, 25, said his shoulder periodically bothered him last season, but he assumed it was an ailment that could be alleviated simply by rest, which is why he waited until the end of the year to have it checked out.
• A's sluggers look to pick up where '18 left off
"In a perfect world, I would have said something right off the bat," he said. "I just figured it was from the long season and it would get better. I knew I was having thumb surgery, so I figured once I had that and rested and started working out, everything would be good again.
"Obviously it's not ideal to get two surgeries or start Spring Training a little late, games-wise, but luckily I can use this time to get strong and get myself prepared and be able to get the at-bats I need and be ready for the year."
Chapman's thumb issue cost him a couple of weeks in 2018, yet he still managed to play in 145 games and collect 24 home runs. He finished seventh in the American League Most Valuable Player vote, hitting .278 with an .864 OPS and a Major League-leading 29 defensive runs saved for this 97-win team.
"We're definitely excited to pick up where we left off and keep getting better, because we've got a really good core group of guys and we keep bringing in good players, and I think we're all on the same page," Chapman said. "Now people know we can play, and we need to keep doing what we've been doing."
Chapman was sporting a pencil-thin mustache upon reporting for his physical Sunday, similar to the barely there hair seen on his face at times last year.
"This is the first time I've really been able to grow some facial hair, so I'm wearing it proud," he said. I'm gonna rock what I've got."
Jane Lee has covered the A's for MLB.com since 2010.


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The 18 Best Coffee Table Books Every Fashion Lover Owns
Sacha Strebe
Graphic by Cristina Cianci
If there's one area of your living room that should never be overlooked, it's the all-important coffee table. What it doesn't have in size it makes up for in stature. This humble piece of décor is key to setting the tone of your living room's entire design; in fact, for most, it is the focal point the interior is built around.
Since it's the center of attention, it deserves a stylish surface. Enter: the fashionable coffee table book. These trendy tomes are as chic as they are clever; their beautiful covers are filled with creativity and industry insight for the fashion-obsessed. And they also make for great conversation starters.
And if your love for fashion is verging on the obsessive territory, consider other places to style these outside of the traditional coffee tabletop. For my living room makeover, I chose to display our best fashion books on exposed metal bookshelves where the books double as artwork. Scroll down to find out which stylish spines we think every fashion lover should have on her coffee table.
Here are our picks for the best coffee table books to add to your collection.
Images of Women II by Peter Lindbergh
Peter Lindbergh Images of Women II: 2005-2014 $99
If you're looking for the ultimate reference in fashion photography, don't pass up Peter Lindbergh's Images of Women II. The internationally acclaimed photographer is renowned for his iconic portraits of '80s supermodels: Who could forget his famous British Vogue cover with Cindy, Naomi, Christy, and Linda? Just like his seminal book Images of Women, this sequel truly celebrates female power, sans the glitz and glamour. Flip through for some of Lindbergh's greatest photos from 2005 to 2014, including portraits of actresses and models like Milla Jovovich, Isabella Rossellini, Monica Bellucci, Tilda Swinton, Kate Moss, and Jessica Chastain. This book is so powerful it even inspired one female leader to start her own business.
Harper's Bazaar Models by Derek Blasberg
Derek Blasburg Harper's Bazaar Models $65 $24
Have a slight model obsession? Don't worry, you're clearly not alone. In fact, Harper's Bazaar dedicated an entire book to them in a bid to satisfy our voyeuristic fascination. Penned by fashion darling (and every supermodel's bestie) Derek Blasberg, this chic hardcover is brimming with juicy anecdotes and exclusive access. Consider this your backstage pass to the rich and diverse lives of 28 of the most famous supermodels from past and present, including Iman, Cindy Crawford, Lara Stone, Lily Donaldson, and Hilary Rhoda.
Alexander McQueen: Savage Beauty by Andrew Bolton
Andrew Bolton Alexander McQueen: Savage Beauty $50 $36
Alexander McQueen was one of the most influential, imaginative, and provocative designers of his generation. His whimsical, otherworldly, and radical designs are highly revered by the fashion community for his combination of haute couture and technological innovation. You'll be intrigued by this designer's stunning anthology of work that's both provocative and captivating.
Chanel by Francois Baudot
Francois Baudot Chanel $75 $60
If there's one female leader in history who truly forged a new path for women, it's Coco Chanel. The bold fashion designer revolutionized style all while building her own global empire that's now considered one of the world's most luxurious houses. Her modern aesthetic and bold attitude liberated women from their traditional garb and showed them the power of a chic pantsuit. She inadvertently changed the entire fashion landscape with her revolutionary style.
Becoming by Cindy Crawford
Cindy Crawford Becoming by Cindy Crawford $50 $39
With her signature smile, svelte figure, and trademark mole, Cindy Crawford is one of America's most iconic models. Her success as a model in the '90s made her an international celebrity, walking countless runways, starring on numerous covers, and appearing in George Michael's music video for the hit single "Freedom '90" along with fellow supers Linda Evangelista, Tatjana Patitz, and Christy Turlington. Her latest book, Becoming, chronicles her incredible life and career.
Advanced Style: Older & Wiser by Ari Seth Cohen
Ari Seth Cohen Advanced Style: Older & Wiser $35 $25
In an industry obsessed with youth, it's refreshing to see a book that celebrates the over-60 set. Inspired by his own grandmother's style, Ari Seth Cohen launched his blog, Advanced Style, to document women like her in the world's most stylish suburbs. After the overwhelming success of his self-titled book, Cohen recently released the sequel, Advanced Style: Older and Wiser, with even more senior street style from around the world, including some well-dressed gentlemen.
Grace: 30 Years of Fashion at Vogue by Grace Coddington
Grace Coddington Grace $175 $155
At the tender age of 74, fashion stylist, author, and creative director Grace Coddington told The Business of Fashion she was stepping down from Vogue to take on external projects. Never one to slow down, the flame-haired creative has become an inspiring female leader for young women across generations. Her 408-page book, Grace: Thirty Years of Fashion at Vogue, celebrates her legendary work alongside the industry greats, including Helmut Newton, Peter Lindbergh, Steven Klein, Annie Leibovitz, and Herb Ritts.
Louis Vuitton Windows by Francesco Bonami
Francesco Bonami Louis Vuitton Windows $895
Before we purchase something, we shop it first with our eyes, which is why storefront window displays are so crucial. Perhaps the most exciting of them all are the windows to the world's most luxurious fashion houses. Louis Vuitton is renowned for its window displays, which is why the company compiled the wonderful spectacle into a collectible book. New York Times fashion director and critic Vanessa Friedman wrote the introduction to the hand-bound work of art that truly captures the spirit and inside world of Louis Vuitton.
Impact: 50 Years of the CFDA by Patricia Mears
Patricia Mears Impact $65 $30
While we adore and revere the iconic fashion houses, it's the next generation of designers who will carry the torch forward. This is why the Council of Fashion Designers of America is so lauded. The council's specialized team of experts, editors, and industry heads have discovered and nurtured some of today's biggest talents. Impact celebrates 50 years of the CFDA with an essay on its history and 300 personal statements from influential designers, including Marc Jacobs, Proenza Schouler, and Alexander Wang. The bright pink cover is sure to be a hit on any coffee table.
Influence by Ashley and Mary-Kate Olsen
Mary Kate Olsen Influence $12
With their inimitable style and creative careers, it was only a matter of time before Ashley and Mary-Kate Olsen put it all into a book. But this one is different. Influence takes on an Interview approach whereby the twins document their conversations with the people they admire, including Karl Lagerfeld, Diane von Furstenberg, John Galliano, Lauren Hutton, and Christian Louboutin.
Tom Ford by Tom Ford
Tom Ford Tom Ford $140 $82
Is there anyone more iconic in fashion than Tom Ford? His risk-taking attitude transformed Gucci into one of the sexiest fashion brands in the world (and certainly one of the most popular). This bold book catalogs Tom's reign and vision at Gucci and Yves Saint Laurent from 1994 to 2004, including fashion, architecture, store design, and advertising. Flip through more than 200 pages of his work, including memorable images from Richard Avedon, Steven Meisel, Helmut Newton, Herb Ritts, and Craig McDean. Ford's insatiable style and sensual approach to fashion will keep you coming back to this book time and time again.
Valentino: Themes and Variations by Pamela Golbin
Pamela Golbin Valentino $80 $40
Just the cover alone could compel anyone to purchase this beautiful book. Valentino is notorious for creating visually arresting modern fashion without compromising its history. The brand's clothing is steeped in history, with a foot firmly in the contemporary space. It's why Valentino's exquisite designs are beloved by hot young Hollywood stars as well as society's elite. This book chronicles the dresses, the culture, and the art behind the brand.
The Little Dictionary of Fashion by Christian Dior
Christian Dior The Little Dictionary of Fashion $20 $15
If we ever had to recommend one authority to consult on fashion, Christian Dior would be it. The legendary couturier created venerable masterpieces that transcend time and trends; in fact, women still clamor to don his designs. Thankfully the modern fashion lover has access to his impeccable style secrets courtesy of his charming handbook, The Little Dictionary of Fashion. Discover the right way to tie a scarf, what to wear to a wedding, and how to walk with grace. You might want to leave a page open on the coffee table so your guests can take a leaf out of Dior's book.
Love Style Life by Garance Dore
Garance Dore Love Style Life $30 $13
Garance Doré has charmed us with her effortless French-girl style, impeccable wit, and fresh approach to fashion on her self-titled site. If like us, you're one of the millions of fans who've bookmarked her blog, you'll adore this beautiful behind-the-scenes compilation of her life, travels, and candid tales. Consider this your backstage pass to the world of Garance.
Frida Kahlo: Fashion as the Art of Being by Susana Martinez Vidal
Susana Martinez Vidal Frida Kahlo $252
Her extraordinary artwork aside, Frida Kahlo's story is fascinating. The iconic artist was renowned for her daring style and razor-sharp wit, all of which made her an early feminist icon for women around the world. Her take on fashion and beauty continues to influence creatives today. This book is a stunning showcase of Frida's work, style, beauty, and art. A coffee table must-have.
D.V. by Diana Vreeland
Diana Vreeland D.V. $17 $7
Who wouldn't want to live like Diana Vreeland? The dynamic style icon and editor in chief of Vogue led a fascinating life mingling with all the big names from Coco Chanel to Andy Warhol. Well, why not? Or as Vreeland famously said, "There's only one very good life, and that's the life you know you want and you make it yourself." And boy, did she live. This extraordinary autobiography takes you along for the whirlwind ride, into the glamorous parties and onset of the most famous photoshoots. It's pure magic.
Martin Margiela: The Women's Collections 1989-2009 by Alexandre Samson
Alexandre Samson Martin Margiela $55 $37
Martin Margiela is one of the most important designers of our generation, yet few know who he is or what he looks like. Unlike the self-promotional world we live in today, Margiela never showed his face in a bid to have the work stand on its own, and it did. This book is a must for Margiela fans who crave a beautiful compilation of the designer's fashion shows, spaces, music inspiration, and iconic pieces from the past 20 years.
Andy Warhol Portraits: 1958-1987 by Richard B. Woodward
Richard B. Woodward Andy Warhol Polaroids 1958-1987 $145
While we're more than familiar with Andy Warhol's photography and screen prints, it's his polaroids that really set his work apart. He was rarely seen without the iconic camera, which he used at every party and event to document the personalities of his day, many of whom were celebrities. The cover of this book alone is enough to make anyone buy it, but the imagery in between doesn't disappoint.
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What users want to know is: "Will it make my applications run faster?" The short answer is yes. But there's more to the story.
Different applications (such as office productivity tools, email clients, VoIP, etc.) use different protocols to communicate over the Internet. In fact, many protocols were developed to handle specific applications. So, at first blush you would think that if we optimize the underlying protocol, we're done. Well, optimizing the communications protocols is an important first step to improving applications performance. But in many cases significant additional improvements can be realized by developing special modules to proxy common programs.
Proxy modules improve responsiveness by reducing unnecessary roundtrips that application natively generated. Reducing superfluous chatter boosts performance on any link – even connections where TCP has already been optimized. Otherwise, inefficiencies in the application-level protocols can overwhelm improvements made at the transport layer. In some instances, streamlining application communications can eliminate up to 98% of the network chatter from a specific application. Thus, application optimization can deliver significant improvement in data throughput and program responsiveness.