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President Bush Breaks Silence, Retains Class
Posted by Kathleen McCaffrey Tuesday, November 9, 2010 at 08:00am 17 Comments
Last night, President Bush started the tour for his new book Decision Points with a televised interview with Matt Lauer. Naturally he was interrogated about certain points of his time in office, particularly the war in Iraq. He professed his regret over reactions to incidences like Hurricane Katrina. But what I doubt will be touted in the media are his most endearing aspects:
"In March 2009, Bush said Obama "deserves my silence," and he plans to stick to that pledge. "Once you get back into the arena, and once you get back involved in politics," he says, "you will be a critic." He cares deeply about immigration, he says, but he doesn't expect to speak out about it. "That is the kind of issue that tends to suck one into the political environment," he says.
Obama often criticizes Bush, though he sometimes says "the previous administration" instead of using his predecessor's name. In an August speech, he said the recession was caused by Bush policies that "cut taxes for millionaires (and) cut working folks loose to fend for themselves."
Isn't Bush tempted to defend himself and his record? "No, because once you're in, you're in, and I don't want to be in. … Politics is a chapter in my life. It wasn't my whole life. If I feel uncomfortable doing something, I'm just not going to do it."
Did anyone else see the interview last night? What did you think?
Spartan | November 9, 2010 at 12:43 am
Dear Professor
I find President Bush an enigmatic figure. On the one hand there is much to admire in him, including the overcoming of an addiction. No one can doubt his patriotism. On the other hand his predelictions for big government provided the excuse this administration has used to expand the monster further. If he had not gone down that road would they have dared to go this far this fast?
ListKeeper | November 9, 2010 at 5:22 am
I find GWB enigmatic as well. I'm conflicted by letters of solicitation that come from his library foundation.
I'm tempted to give in admiration of the way he rallied the nation after 9/11 and his unvarnished love for those serving in the mililitary.
As of now, I've not donated because of the way he grew government and "abandonded the free market to save the free market."
kitty | November 9, 2010 at 6:48 am
Note: Rush will interview President George W. Bush Tuesday at 1:06 ET. It will be Bush's first national radio interview to promote his memoir, "Decision Points."
Independent Patriot | November 9, 2010 at 6:55 am
I saw parts of the interview last night. I thought the President was the same classy individual he always was. If we remember during his entire tenure in office no matter what anyone said about him, he did not respond but did his job. The fact that he could write this book and evaluate how he came to the important decisions in his administration and even accepting that there were mistakes shows that he is truly intelligent. In fact I would say far more intelligent than anyone in office today.I propose that his book is going to be invaluable to historians to come. For it details how and why decisions were made and it shows the reasoning required in the Oval office and of the most powerful individual on Earth. And unlike our current administration President Bush is able to Man-Up.
CHMusicus | November 9, 2010 at 7:28 am
I watched part of it. All those years of the media painting him as a buffoon, and I thought last night he spoke clearly and truthfully.
To someone that didn't invest effort into the political arena until only a few years ago (ignorance is bliss), some things he said were very interesting to me.
All that complaining about waterboarding, and it was used on 3 guys. Hmm..
But, like I said, he explained his decisions and encouraged people to come to their own conclusions, given his perspective. Well done.
Zachriel | November 9, 2010 at 8:56 am
CHMusicus: All that complaining about waterboarding, and it was used on 3 guys. Hmm..
Waterboarding is torture, and illegal under U.S. and international law; as is the use of stress positions, beatings, deprivation and rendition to countries known to abuse prisoners.
A.Worthing | November 9, 2010 at 9:15 am
I always said that there were two kinds of "class." The first is something you are allegedly born with (which I don't buy into). The second is something you give yourself.
Both Bush Sr. and Jr. allegedly have the first kind. But they definitely have the second kind in spades.
K | November 9, 2010 at 9:31 am
I'm with you Zachriel. However most popular objection to the torture under Bush seemed to be politically rather than morally motivated…as witnessed by the near evaporation of public outrage under the current president.
I'm sure some believe it stopped on 1/20/09…but I'm far too cynical to believe that.
CHMusicus | November 9, 2010 at 10:02 am
Zachriel, I didn't mean to downplay waterboarding at all. I personally was not aware it was used on so few prisoners.
I would agree with K in that the objection seems to have been politically motivated (W could do nothing right whilst in office, according to the media).
pasadenaphil | November 9, 2010 at 10:58 am
A good man with good intentions laying his share of pavement on the road to hell. How history remembers him depends on who ends up writing that history. Unfortunately, a favorable legacy for the Bushes will only be written if the one-world corporatist socialists win. We are on the other side. We want liberty.
Nathan | November 9, 2010 at 11:55 am
@pasadenaphil-would these be the same one-world corporatist socialists that spent 8 years waving around their BusHitler signs?
retire05 | November 9, 2010 at 12:01 pm
It takes a large, and honest, man to say "I made mistakes". That is not something we see with the current administration who has just been cut off at the knees.
And for those who consider the method we use to waterboard, I suggest you inform yourself to the method used by the North Vietnamese that made it illegal to do so. And are you now saying that all our SERE teams that have been waterboarded, as part of their training, are now "victims"? Please, let's have a little honesty here.
W is what is called a "compassionate" conservative. i.e., he is a left leaning conservsative. And I suggest that history will treat him with more kindness than most Americans did. Remember what Truman's ratings were when he left office, and now he is heralded as one of our best presidents.
Only time will tell if the liberation of Iraq will serve in the desire to create an ally in the Middle East and promote freedom in that region. But I can promise you, as Iraq prospers, and its people prosper under freedom, other nations are going to take a good hard look and understand that they too, can have the same freedom. Iran for one. We are already seeing signs that Iranians are bucking their oppressive government. Too bad the luguini-spined current POTUS did not support them in their endeavors for a free society. Instead, he went after tiny Hondouras, and lost.
Edward Cropper | November 9, 2010 at 1:02 pm
GW is basically a good decent man, but that in no way eradicates his big government escalation and the big problems he helped create.
vladdy1 | November 9, 2010 at 3:49 pm
I like GW as a person, especially his love of America.
But — even tho' he denies it — his approval of amnesty and most of all, his impressing upon the country that "Islam is a religion of peace" did more harm to America than…well, than anybody until Obama.
Listening to him talk brings back memories of the days when you could listen to a president talk like a human being, TO us, and not AT us in that smug, condescending manner.
Micha Elyi | November 9, 2010 at 6:30 pm
Zachriel: Waterboarding is torture…
Not everything unpleasant is "torture."
tuleesh | November 9, 2010 at 7:01 pm
Regarding President Bush's refusal to be goaded into dumping on the Secular Saviour:
It's simply Class vs. Crass. Obama's on the losing side on this one.
"Don't sell your soul for the sake of politics."
–G.W. Bush on the Oprah Winfrey Show
Zachriel | November 10, 2010 at 12:19 pm
Micha Elyi: Not everything unpleasant is "torture."
That's right, but waterboarding causes the type of severe pain and suffering associated with drowning.


text:
Un accelerador és o bé el primer tram d'un vehicle de llançament multitram o bé un coet amarrat que s'usa per augmentar la potència d'enlairament del vehicle i la seva capacitat de càrrega. Els acceleradors són generalment necessaris per llançar les naus espacials cap a l'òrbita terrestre o més enllà. En tots els casos l'accelerador es deixa caure a l'oceà quan el combustible s'esgota: aquest punt es coneix com a punt límit del motor accelerador (BECO, sigles en anglès de booster engine cut-off). La resta del vehicle de llançament continua el seu vol amb els seus trams restants. L'accelerador pot ser recuperat i reutilitzat, com és el cas del transbordador espacial.

Referències

Enllaços externs
 Solid rocket boosters  a nasa.gov
 Solid Rocket Booster Jettison a aerospaceweb.org

Motors de coet

redpajama_set_name: RedPajamaWikipedia


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She Quit Her Job, And Then Earned Over $10 Million From Her Trade and Travel Course on Teachable
by Charlene Rhinehart April 3, 2021 April 3, 2021 11724
(Image Credit: Instagram/TeriIjeoma)
Teri Ijeoma announced that she was the top course creator on the Teachable platform in 2020, earning over $10 million in revenue for her Trade and Travel course.
"You don't become one of the top-selling courses on Teachable by marketing. The course actually has to get people results. You guys have seen the testimonies of my students on my page. These are real people, having real results. That's what makes our course great."
She adds, "Now just imagine, making money from one of your businesses and then knowing how to trade to multiply the earnings! That's legacy building!"
From Assistant Principal to Trade and Travel Expert on Teachable
Before Ijeoma started her full-time trade and travel journey, she was working as an assistant principal at an elementary school. Although she was great at what she did, she knew the vision for her life went beyond the constraints of her job. Ijeoma started trading as a side hustle to earn extra income. When tensions became high at work and her friend passed away suddenly, trading gave her the courage to switch gears. She knew it was time to make the most of every minute she had.
In 2017, Ijeoma decided to quit her job, travel the world, and use her trading income to fund her lifestyle. A few months later, she found herself teaching others how to trade all over the world.
"I didn't seek to start a class," Ijeoma shared on the David Never Sleeps show. "I just wanted an exit strategy. While I was traveling, people started asking me to teach them how to trade. I did my first class in Thailand. The people loved it and asked me to do another one. I did my second class in Vietnam."
When she returned back home to the United States, she received more requests to teach others how to trade. She started off selling tickets for less than $100, attracting more people to her classes than she expected. When her training equaled her teacher salary, Ijeoma knew she wanted to continue teaching others how to trade stocks.
Instead of scheduling multiple trainings every day, Ijeoma developed a source of passive income using the Teachable platform.
Spreading the Power of Stocks on Teachable
Ijeoma's success within the last three years has been astounding. Her Trade and Travel courses have taken off and she's broken records on the Teachable platform.
"Only two-course creators made over $10,000,000 in 2020 and I am one of the two," Ijeoma told David Never Sleeps.
Her students have been able to earn $1,000 per day, retire their family members, and pay off debt. What drives Ijeoma to continue on her journey is to ensure more people have access to basic needs — even her family.
Ijeoma's success as a stock trader has helped her give her parents access to quality healthcare.
"I know money can't buy you happiness, but money can buy you dignity," Ijeoma's mother told her after an interaction during a doctor's visit. Her mother's ability to afford the services was questioned by the white staff. She was able to keep her head up knowing she had the money to pay for what she needed.
"That's my why," says Ijeoma. "I want to help people have dignity when they go into any situation – especially their healthcare."
Charlene Rhinehart
Charlene Rhinehart is the best selling author of "Dividends Are a Queen's Best Friend" available on Amazon. She makes investing in the stock market as simple as shopping at the mall! Charlene is on a mission to help more people build stock portfolios that are bigger than their shoe collection. Her work has helped many people leave the debt cycle and enter the dividend circle. Charlene is a Certified Public Accountant, Founder of Wealthy Women Daily, and Editor-in-Chief of The Dividend InvestHER. She is also the Managing Director of CEO Unlimited Communications Firm where she helps others break down complex information into digestible concepts that audiences love. She enjoys writing money, career, and travel articles for publications all over the web. Connect with Charlene on Instagram @charlenerhinehart or get access to weekly money insights, investing ideas, and travel tips by subscribing to Wealthy Women Daily Free Newsletter at www.wealthywomendaily.com.

redpajama_set_name: RedPajamaCommonCrawl


The Hole of Horcum is one of the most spectacular features in the North Yorkshire Moors National Park. It is a huge – a huge natural Devils Punchbowl feature, 400 feet deep and more than half a mile across. It was formed a long time ago when Wade the Giant scooped up a handful of earth to throw at his wife during one of their many arguments.
Actually, it was created by a process called spring-sapping, this is where water welling up from the hillside gradually undermines the slopes above. Over thousands of years, a once narrow valley has widened and deepened into an enormous punchbowl – and the process still continues today.
Unfortunately, we do not stay very long around the Punchbowl. Three of the walks get off the coach at the Hole of Horcum, the 10-mile route heads west on part of the Tabular Hills Walk and then goes south down past Levisham and then further west again through the woods at Heugh Howl before reaching Pickering. The 12.5-mile route heads along the Old Wifes Way and then south to reach the Bride Stones before continuing south into Stain Dale and Thorton Dale and then turning west along the valley passing Thorton-le-Dale to the north and coming into Pickering from the west.
The 11.5-mile route is also going along the Old Wifes Way and the Bride Stones but before then the route is going on a small diversion from the car park down into the Hole of Horcum. After the Bride Stones the route heads west across the valley towards Lockton then climbs towards Farwath crossing the North York Moors Railway line then heading south-west towards Pickering.
There are lots of Standing Stones in this area and most of them were often connected with fertility rites relating to successful crop harvests. The fertility rites were associated with an earth mother or goddess sometimes called the Old Wife and so we have the Old Wifes Way. The Bride Stones are odd shaped sandstone pinnacles, they are spread over 300 acres so the routes are just passing through between what is called the High Bride Stones and the Low Bride Stones. Why are they called the Bride Stones? Perhaps the Old Wifes fertility rites were a bit more successful than just a few crops and some marriages were called for.
The 7-mile route travels further down the A169 after the Hole of Horcum and gets off not far from Lockton which it passes to the north. It then swings south through Row Wood and picks up the same route as the 11.5-mile route at Farwath.
If you fancy a walk starting close to the Hole of Horcum with perhaps a wander along the Old Wifes Way or a visit to the Bride Stones or a loop along the Tabular Hills Walk you will find a variety of routes to choose from. You can get in touch with us from our Contact Page and you can find the walk descriptions here and the GPS routes here.


Family is one of the most important things in the world.
That's why, here at TYI, we've created a huge range of personal artwork which can be personalised with family names, dates and places to create individual pieces of wall art.
Available in a range of designs, you're sure to find artwork here that fits your family's image - plus you can personalise the artwork to help create a truly unique print.
These personalised artworks make amazing presents for any occasion.


Looking for something fun to do with the kiddos or an easy treat to bring to the Easter egg hunt this weekend? Try making these sweet and easy treats!
Fill a small bowl with sprinkles.
Melt a half cup of chocolate chips in a double boiler or in the microwave on low for two minutes, stopping to stir every 20 seconds.
Roll the edges of a Snapper in melted chocolate and then roll in the sprinkles, just enough to rim the edge of each piece.
Dip a small section of each jellybean in melted chocolate and gently push into center of the Snapper.
Let the finished nests set for ten minutes.


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Oneohtrix Point Never Thinks the Internet Sucks, But What Else is There to Be Addicted To?
By Nathan Taylor Pemberton
Photography Alexander J Rotondo
The noises you hear when listening to Daniel Lopatin's productions made as Oneohotrix Point Never are the swan song frequencies of a dying internet. And the scope of his project is growing. This summer, he staged a "quasi-libretto" called MYRIAD at the Park Avenue Armory, performing songs off his 2018 album, Age Of. This "concertscape," as an oversized playbill described it, included performances with cellist Kelsey Lu, noise musician Prurient, visuals by Nate Boyce, inflatable landscapes, and a band of dancers clad in cowboy contagion uniforms. It was a vision of something run amok—with Lopatin serving as a reserved master of ceremonies, controlling his set pieces from behind a midi keyboard. This spring, Lopatin plans to bring an expanded MYRIAD to London's iconic Round House.
Up close, Lopatin is less reserved about the scarred informational landscape we find ourselves in. The optimism found in the dark spaces of Web 1.0 rabbit holes and VHS fantasies is a key input that Oneohotrix Point Never has collected and redeployed. Whether through working for directors Sofia Coppola or the Safdie Brothers, or producing rejected demos for Usher, or through his latest release Love in the Time of Lexapro, out this month, Lopatin is filtering the grotesqueries of visual culture into something more tactile. He spoke with Interview about this very specific practice, the end of the internet as we knew it, his bastard genre-invention Vaporwave, and his tendencies to produce kitsch content. "You are what you eat," he said. "Kind of."
NATHAN TAYLOR PEMBERTON: You're really good at the internet.
DANIEL LOPATIN: My friends tell me I'm the best of the crew at the internet. I'm the internet boy.
PEMBERTON: The internet is boring now.
LOPATIN: Yeah, it sucks. It's become boring, to me. I think Web 2.0 was the beginning of the homogenization of the internet where everything had been templated. It's content management driven and just a giant pasteurization complex. Everything looks the same. All websites look the same. Blah, blah, blah.
PEMBERTON: How much are you on the internet every day when you're not producing?
LOPATIN: Really good question. I'm almost just a basic addict like everyone else. Instagram, Twitter. Refresh, refresh. All these things that were not a factor 5, 10 years ago. I don't really like it.
PEMBERTON: These are the new home pages now. I miss finding the deep—
LOPATIN: Raw emotion.
PEMBERTON: Yes, the weird blogs. Broken Angelfire sites. Shoddy HTML stuff.
LOPATIN: The blogs were great. The blogs I really miss. Just look at the history of the internet. It's oriented around hyperlinks, text. Even video games. The first adventure games basically dealt with poetry. As we moved away from that, towards the individual-oriented way of navigating the internet, we lost the ability to dream that way—in stories and ideas. The depth of language, I think, is missing. There is a connection between this and the idiocy that we're all feeling so constantly. It's sad to me that the main stage of history is a story of how we became this visually obsessed, extremely narcissistic, extremely concerned about image, culture. At least in the West.
PEMBERTON: You've done a very good job of articulating this cultural evolution (or regression) with OPN. Would you say that some portion of its success is because you've attached your music to such extreme visuals?
LOPATIN: We have this thing amongst the extended OPN family, that movement we're trying to orient ourselves around called "Compressionism" — basically a way of harnessing an overflow of images that are there to either titillate you or to make you feel bad about yourself, whatever they're there to do. It's a way to conquer all of these inputs. It's about organizing and sort of re-appropriating things that you don't want necessarily and seeing them in a way that is personal.
PEMBERTON: You're distorting things, everything, wherever you can.
LOPATIN: It's the Jewish mother in me. Trust me. That thing when you grow up in a family with a mother who is really trying to make sure everyone's not just fed but really well fed. Oh come on, do you want more? Let me give you some more. And then my hero, Stanley Kubrick, taught me that every frame you decide to share with people should be super specific and filled to the brim with choices. Specificity actually lends itself to being a Maximalist. I think of it as extremely helpful to just consider all the sub-dermal shit that doesn't usually surface. It may seem like a portentous amount of information, but actually what I am trying to do is just be generous.
"We lost the ability to dream that way—in stories and ideas. The depth of language [on the internet], I think, is missing. There is a connection between this and the idiocy that we're all feeling so constantly."
PEMBERTON: Do you have any complaints to lodge about the state of the conversation online?
LOPATIN: Vehement zealotry on both sides, like intense anti-intellectualism, bothers me a lot.
PEMBERTON: A major mood, for sure.
LOPATIN: Immediately, I feel alienated because I like words. I like explication of ideas, even if I'm wrong or even if it's a struggle or if it's a work in progress. Another thing I don't like: denial of works in progress because everything is being super assessed so quickly.
PEMBERTON: If I assessed your works as kitsch, how would you respond?
LOPATIN: Kitsch has been in my vernacular.
PEMBERTON: Super kitsch.
LOPATIN: It is super kitsch! I took a class when I was 19 or 20 years old at Hampshire College with an extremely talented and incredible thinker, philosopher, professor named Monique Roelofs. She taught a class on kitsch, and I made a piece of music for it. This is before 9/11. The first lyric of this song was: "The plane, the plane flew through my window." It detailed the moments before this plane comes through this apartment where this, like, archetypal rock star is writing a song with one knee up, smoking a cigarette. I just like cliches. I like tvtropes.com. It's pretty much my bible.
PEMBERTON: I've actually never seen.
LOPATIN: Check that out. It's one of the last great websites. If not a living testament to our culture. Kitsch is very important to me.
PEMBERTON: I found an old jewel case for the Chuck Person's Eccojams cassette in my apartment not long ago. It's a cult item now, I hear.
LOPATIN: The guy who pressed [Eccojams] has been amazing about not cheaply profiting off of it. We've never done a second run.
PEMBERTON: I look at the Discogs page now and then. One was recently listed for $2,000!
LOPATIN: There's like a really, really grotesque sub-market. That's what you get when you launch a genre [Vaporwave], I suppose.
PEMBERTON: People are selling cheap imitation bootlegs of it, it seems.
LOPATIN: That's so whack. That's fucked.
PEMBERTON: Are you going to re-issue it?
LOPATIN: I don't see the point. It's a mixtape, where we slowed down other people's music. So, making money off of that … I mean. It would be cool to do a re-release as some sort of charity scenario. Just do another 60 tapes, exactly like we did the first time, and try to raise money for Autism research. I think about that a lot, I think about the scenario where you're not able to connect to your environment on the level that others are.
PEMBERTON: Are you aware of how your work is perceived on the internet?
LOPATIN: From lurking on forums, I can ascertain certain tendencies.
PEMBERTON: Do you consider forums a kind of raw barometer of the cultural psyche?
LOPATIN: It's place of scatology and truth. You have to look in forums if you want to actually deal with reality a little bit. But at the same time, the difference between Rabelais' marketplace, for instance, and our internet forums is that you couldn't fucking hide behind an anonymous handle. You were responsible for your niche. You were responsible for your bag of bones.
Joey_Ramone-Legs_McNeil 1978
Punk May Be Dead, But Legs McNeil Sure Isn't
Wilsen is Listening to Hans Zimmer, "Monster Mash," and A Lot of Nick Drake


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A year passes after floods but relief work still lacks coordination
Doing away with parallel overlapping systems and establishment of fully functional, well-resourced and integrated disaster management system at the grass-root level could ensure a reduction in flood losses in future, experts told Pakistan Today.
Pakistan is a disaster prone country and its ill-preparedness to meet any natural calamity renders a large number of its people vulnerable putting their existence and resources at stake, the said. According to the National Disaster Management Authority (NDMA) and the UN Office for Coordination of Humanitarian Affairs (OCHA), around two to five million people were likely to be affected by the floods in the current monsoon season.
"There are around 20 organizations or departments in the country which are working in floods related fields and there is zero coordination among them. Pakistan is still far away from protecting its people from flood disaster," Arshad Abbasi, an expert in water and floods told Pakistan Today.
He also added that there was a lot of duplication in the works of the government departments which amounted to wastage of resources, adding that the government had failed to learn its lesson even after the last year's loss of $4 to 5 billion.
The Oxfam in its recent report had also stated that Pakistan was facing another monsoon season but was not prepared for any calamity.
Amir Zia, a researcher working on the state response to flood disaster of 2010, said that NDMA establishment under National Disaster Management Act 2010 by the government had stated that federal and provincial relief cells would be absorbed into the NDMA and the purpose of it was avoiding duplicity and improving the coordination among different departments, but still various government departments were working parallel to each other with overlapping mandates.
He also added that the Oxfam too had pointed out this issue in its report. The Oxfam had said that it was particularly important that certain departments were integrated into disaster management structure, including Pakistan Meteorological Department and clarity was needed regarding the role of Federal Flood Commission as its coordination with provincial irrigation departments was weak. Zia further suggested that absence of local government system in the floods of 2010 would have helped reduce losses "The local government system, or whatever the system of local bodies the provincial governments come up with in future, needs to be integrated with NDMA.
The local governments, which consist of representatives of the most immediate vulnerable communities, can help improve the performance of the District Disaster Management Authority and NDMA," Zia said. When NDMA spokesman Ahmed Kamal was contacted, he said that Pakistan was prepared. "I cannot say that Pakistan is completely prepared to face the disaster but it is certainly more prepared than last time," the NDMA spokesman said.
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Announcing the Division of Inclusive Excellence
Our Leadership»Announcing the Division of Inclusive Excellence
National First-Generation College Celebration
Remote Classes Nov. 22 and 23, Campus Discussions After Break
SU Campus Vaccinated Over 95%
Covid Fall Plan 2021 Update
Dear Students, Faculty and Staff,
I am writing to share an update on Susquehanna's inclusive excellence progress.
In 2020, University President, Jonathan Green called upon Susquehannans to support an actively anti-racist community. This included forming the CenSUs: Everyone Counts task force. One of the task force's recommendations to move the institution forward regarding diversity, equity, inclusion, and justice was to centralize that work into a cohesive unit.
This year, the Division of Inclusive Excellence was established. The Association of American Colleges and Universities defines "inclusive excellence" as focusing on student intellectual and social development, utilizing organizational resources to enhance student learning, and recognizing how the cultural differences of others enhance the student and organizational learning. It is from that premise that we look to create a synergy in which the whole is greater than the sum of its parts. Susquehanna has many strong initiatives and programs to educate our community, but there has been a lack of cohesion to focus the work. This change will address that fact.
The entities united within this newly created division are:
Center for Diversity and Inclusion
Office of the Chief Inclusion and Diversity Officer
Office of Jewish Life
Office of Religious and Spiritual Life
We have a number of things planned for this semester, including having a faculty member join the team (coordinator, faculty inclusion and diversity), unveiling a new faculty and staff DEI curriculum, and advancing the work of the Inclusion, Diversity, Equity in Action Council. (IDEA), which will build upon the foundation set by the task force.
We will provide regular updates to the community through our Inclusive Excellence website and other campus communications. Come visit our office on the main level in Degenstein Campus Center, next to the Hawk Hub, where you can find division staff strategizing and developing pedagogy to educate and teach about diversity, equity, inclusion, and justice.
As the new academic year gets underway, remember not to let a learning opportunity pass you by. When faced with a challenge, ask yourself, "What can I learn from this experience?"
Continuing to further the work,
Michael Dixon (he/him)
Chief Inclusion and Diversity Officer


Great opportunity for the adventure of a unique home - - situated in one of Lacona's original buildings. While this has functioned as a restaurant for the past 30+ years, over 4100 sq ft could be amazing living space with some alteration, which has been an option that has worked well in other nearby buildings in this community! Beautiful hardwood floors, original 1902 walk-in cooler, and a myriad of interesting spaces to make your own. Oversized detached garage, and absolutely amazing private deck/patio space. This is a project - but could have great reward! Let your creativity guide you to make it yours!


Could Sadie's life get any more cringey? Having a brother in a boy-band is bad enough. Living in a house with two warring grans and a flooded bedroom is worse. And with a new mate who's a stand-up comedian AND an undertaker, Sadie wonders if life will ever be, y'know … normal? The third starry-eyed story featuring sassy, down-to-earth Sadie!


An alternative to traditional fundraising events, the T.J. MARTELL FOUNDATION'S BOWLING BASH is a unique, new charitable event blending philanthropy, competition and most importantly to support the T.J. Martell Foundation's mission of funding leukemia, cancer and AIDS research.
Guests will be greeted with team shirts, two drink tickets, finger-foods and the upbeat sounds of Honorary Bowling Bash Chairman, DJ SEAN GLASS. Guests should be prepared for the ultimate charity competition and the chance to claim the 2014 T.J. MARTELL FOUNDATION'S BOWLING BASH trophy!
We are encouraging each team member to do their own fundraising for additional prizes including a top prize for our highest fundraising team. So gather your friends, family and co-workers and help support a great cause!
Click here to create your own individual or team fundraising page.
You can create a team with your friends by purchasing 6 tickets!


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Salt Space Hove is located at:
Salt Space Hove
372 – 374 Portland Road Brighton and Hove
BN3 5SD – East Sussex , United Kingdom
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New York's drinking water is some of the most delicious in the land, and it's filled with microscopic shrimp.
They're called copepods. This is one a guy took photos of under a microscope after H&E staining the sample. They're 1-2 mm long, transparent, have two sets of antenna, and feast on mosquito larvae. What are they doing in the water supply? Well, New York's water is of such high quality that it isn't required by the EPA to mechanically filter its H2O, which means you get to gulp down these cute little guys with every glassful. Bottoms up!


Tom Howie was interviewed on the one year anniversary of the tragic Amtrak/CSX accident in Cayce, SC that happened on February 4, 2018. Tom discusses what happened during the accident and how positive train control (PTC) works.
The video is below or you can read the article here.


You'll find yourself remarkably well-placed for the West End shops and theatres, the City and all major exhibition centres, sporting venues and tourist sights.
Hanwell and Ealing are served by the Piccadilly, Central and District Lines of the Underground for every part of London.
As well as non-stop rail services to London Paddington and many bus routes.By car, you're close to the A4/M4 and A40, the two main arteries to the West. Among the attractions within easy reach are Wembley stadium and arena, Twickenham Rugby, Richmond Deer Park, Kew Gardens, Wimbledon Tennis and Windsor Castle.
Hanwell is a peaceful and pleasant backwater, full of greenery and wildlife within easy walking distance.Your hotel is right beside Elthorne Park, with its canal-side paths.
A popular animal centre, and extensive water meadows that are home to many wetland bird species.
Contrast this with nearby Hanwell Community Centre, a historic building that was once a school attended by the young Charlie Chaplin and his brother.Only a little further is Osterley Park, a classical mansion in splendid grounds open to the public, not far from the magnificent Syon House, just the other side of Brentford Lock and Marina.
The amazing history of these is an equal attraction for those visiting Ealing.
Ealing has much to offer visitors, from its beautiful places.
There are much more facilities to visit nearby Towns, which is only 10min or 5 min drive from hotel.


Uma estrutura massiva, araneiforme, desceu sobre a atmosfera de Lisboa. Uma nave espacial, pensa-se, com um propósito científico: extrair uma substância essencial, um combustível, para que a nave alienígena possa descolar para outras paragens. E essa substância, que os invasores tanto precisam, e incessantemente sugam, e parece que nunca chega, tem o nome de... Anima lusa.
Thank you for downloading this free ebook. You are welcome to share it with your friends. This book may be reproduced, copied and distributed for non-commercial purposes, provided the book remains in its complete original form. If you enjoyed this ebook, please return to Smashwords.com to discover other works by this author. Thank you for your support.


text:
\section{Introduction}
Debris disks contain micrometer-sized dust grains, which can be observed in  scattered light in the optical to near-infrared wavelength range and by thermal emission at longer wavelengths. To interpret observations of debris disks these particles are often assumed to be compact, homogenous, and spherical (e.g \citealt{Roccatagliata2009}, \citealt{Ertel2011, Ertel2012b}). This is a convenient simplification, since it makes the Mie scattering formalism applicable (\citealt{Mie}, \citealt{WolfVoshchinnikov04}). However, there are various processes that would tend to create more complex, e.g. inhomogeneous or almost arbitrarily shaped, particles, instead. In cold clouds gas  molecules can  freeze out on the surface of dust grains, so that the particles  are composed of multilayer, inhomogeneous materials (\citealt{Kruegel}). In young, gas-rich circumstellar disks, collisions of particles occur in which the dust grains either agglomerate and  form larger particles  or  get shattered in fragments with complex shapes. In this context, porosity might support the grain growth process in the disk (\citealt{BlumWurm2008}).

Modeling recent observations of dust in various environments also motivates the concept of porous dust grains. For example, \cite{vanBreemen2011} used a distribution of hollow spheres to fit the $\unit[9.7]{\mu m}$ silicate absorption profile of the ISM based on the model of \cite{Min2005}. \cite{Demyk1999} applied some degree of porosity, which was necessary to reproduce silicate features in the spectrum of dust around the protostellar objects RAFGL7009S and IRAS 19110+1045. Scattered light images of the circumstellar disk surrounding the T Tauri star IM Lupi may indicate the presence of fluffy aggregates (\citealt{Pinte2008}). \cite{Birnstiel2010} and \cite{Ricci2010,Ricci2012} used porous spherical grains to specify the dust opacity in a sample of young protoplanetary disks. For a general study of the influence of porosity on the dust opacity in protoplanetary disks, see \cite{Semenov2003}.

Modeling debris disks is an important part of understanding the evolution and formation of stellar disks, hence the evolution of planetary systems. With that in mind, \cite{Augereau1999, Augereau2001}, \cite{Wyatt2002}, and \cite{Fitzgerald2007} used porous grains for disk modeling, resulting in suitable approaches to reproduce observational data of  HR$\,$4796$\,$A, $\beta\,$Pictoris, Fomalhaut, and AU Microscopii, respectively. \cite{Acke2012} found evidence of fluffy aggregates in the disk of Fomalhaut. These are required for the thermal emission characteristic of small grains and the scattering behavior of large particles. A dependence exists between grain porosity and dust temperature (\citealt{Greenberg1990}, \citealt{Vosh2}), causing a shift in the infrared emission to longer wavelengths.

Our study is motivated by the fact that debris disk modeling using compact grains often reveals
a significant discrepancy between  the minimum particle size and the calculated blowout size (e.g. \citealt{Roccatagliata2009}, \citealt{Ertel2011}). The influence of porosity on the radiation pressure has already been considered  in previous studies. \citet{Mukai92} and \citet{Kimura1997}  examined the $\beta$-ratio for fractal aggregates using effective medium theory, while \citet{Koehler2007} applied  discrete dipole approximation. We investigate porous particles and outline various aspects as the absorption efficiency factor, the blowout size, and dust temperatures. In  Sect.  \ref{losgehts} we provide an overview of the applied numerical tool for calculating the efficiency factors and describe our model of porous dust grains. The analysis of the absorption cross sections is presented in Sect. \ref{firstres}, and the blowout size as a function of selected parameters is discussed in Sect. \ref{Kapitel4}. Finally, we present the equilibrium temperature of porous dust particles in Sect. \ref{Staubtemp}.

\section{Calculation methods}
\label{losgehts}
\subsection{Porous grain model}
\label{AbschnittQuerschnitt}
Within the infinite variety of porous particles we consider those that are spherical and from which material is removed so that voids are formed. The advantage of this model is the small number of parameters describing each particle. A debris disk contains a vast number of grains of different shapes, sizes, and orientations. The appearance of the disk results from averaged optical properties. This motivates  for adopting a grain model that results from an ensemble of particles with similar geometric  properties. The spherical grain model with voids satisfies this task, if  the voids are distributed uniformly over the  volume and thus the grain orientation is negligible.

Porosity is the ratio of the vacuum volume to the total volume of the grain,
\begin{align}
 \mathcal{P}&=V_{\textup{vacuum}}/V_{\textup{total}}=1-V_{\textup{solid}}/V_{\textup{total}},\\
  \mathcal{P}&\in \left[0,1\right].\nonumber
\end{align}
For example, a compact sphere is given for $ \mathcal{P} = 0 $. The radius $ a $ is denoted as the minimum radius of a sphere that encases the grain.

Two grains with equal radius and porosity  can have fundamentally different hole sizes, considering the examples of a hollow sphere and a grain that contains many small holes. In principle,  holes of different sizes can be assumed  within a grain. \citet{Vosh1} adopted  a size distribution of the holes in their model, in which the  probability of the presence of a hole is assumed to be inversely proportional to its volume. The holes in our grain model are determined both by the number of dipoles and the process of the grain generation (Sect. \ref{genera}).

\subsection{DDSCAT}
\label{Vollkugeltests}
We used the program DDSCAT to calculate the scattering and absorption cross sections of  irregular particles (\citealt{Draine1994,Draine2010}). It is based  on the theory of discrete dipole approximation  (DDA), where a continuous particle is approximated by the corresponding spatial distribution of  $N$ discrete polarizable points on a cubic lattice. The great advantage of the DDA is the high flexibility of the particle structure, but the applicability is limited by the conditions that the lattice constant $d_{\textup{l}}$ must be small compared to the wavelength and to the scales of the internal grain structure. The first condition is roughly expressed by (\citealt{DraineGood}, \citealt{Draine1994} and \citealt{Draine2000})
\begin{align}
 |n|kd_{\textup{l}}<1,& \label{Kriterium}
\end{align}
where $n$ is the complex refractive index and $k=2\pi/ \lambda$ the circular wavenumber. This criterion is satisfied for  $|n-1|\lesssim3$ (\citealt{Draine2010}).  With the volume of the material in the particle, $V=N(d_{\textup{l}})^3=4/3\pi a^3(1-\mathcal{P})$, it follows $a=\left(\frac{3}{4\pi}\frac{N}{(1-\mathcal{P})}\right)^{1/3}d_{\textup{l}}=\left(\frac{3}{4\pi}\frac{N}{(1-\mathcal{P})}\right)^{1/3}  \frac{|n|kd_{\textup{l}}}{|n|} \frac{\lambda}{2\pi} $, and thus with condition \ref{Kriterium}
\begin{align}
a< 0.09873\frac{\lambda}{|n|}\left(\frac{N}{1-\mathcal{P}}\right)^{1/3}.\label{gultig}
\end{align}
For our studies we use astronomical silicate (\citealt{Draine2003a,Draine2003b}) with a bulk density of $\rho=\unit[3.5]{g\,cm^{-3}}$ (\citealt{Draine2003}).

Before applying the DDSCAT to investigate the behavior of porous grains, we verified the optimum parameter settings (number of dipoles used, etc.) in the case of compact spherical grains. Therefore, we calculate the absorption cross section with the DDSCAT and compare the results with absorption cross sections i) calculated  via Mie theory and ii) using the DDSCAT  with a number of dipoles decreased by a factor of 2. The results are summarized in Appendix \ref{review}.

In Fig. \ref{gultigBild} the applicability of the DDSCAT is illustrated for a compact spherical grain, represented by $\sim$500,000 dipoles. According to  condition \ref{gultig}, the DDSCAT delivers suitable results for the area  below the solid line. While for the solid line the refractive index of  the silicate is taken into account, the crosses are derived by the tests with the compact grains (Appendix \ref{review}). These crosses mark the used upper limit of applicability.
\begin{figure}[t!]
	\centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap2/WasKannEreng.pdf}
\caption{The limit of the applicability of the DDSCAT for a compact spherical grain of  astronomical silicate, represented by $\sim$500,000 dipoles.
According to condition \ref{gultig}, the DDSCAT delivers suitable results for particles with radius $a< 0.09873\frac{\lambda}{|n|}\left(\frac{N}{1-\mathcal{P}}\right)^{1/3}$ (solid line).
In Appendix \ref{review} tests with the DDSCAT are presented, and we define the crosses as the upper limit.}
\label{gultigBild}
\end{figure}
\subsection{Generating porous grains}
\label{genera}
We briefly describe the process of generating porous model grains: $N'=519,832$ dipoles are arranged on a cubic lattice, forming the shape of a compact sphere. A random number generator is used to remove single dipoles to create grains with a porosity $\mathcal{P}$. The remaining dipole arrangement contains $ N=(1-\mathcal{P})\cdot N'$ dipoles, forming a sphere with voids. Each dipole represents a cubic subvolume  $(d_{\textup{l}})^3$ of the  surrounding material, while a removed dipole represents a cubic void of the same size. The large number of dipoles and the application of the random generator ensure a statistical  distribution of the holes. Thus, no preferential direction exists and the optical properties  are roughly independent of the grain orientation. The number of dipoles for  the particles  used in this paper are listed in Table \ref{sovieleNs}. The particle cross sections are shown for different porosities in Fig. \ref{Teilchenquerschnitt}. Some dipoles seem to be  detached from the rest of the complex, but it should be considered that these dipoles may be connected to the particle in the direction perpendicular to the presented cross section. Nevertheless, the procedure of particle generation does not prevent the occurrence of single dipoles, which are isolated from the  rest of the configuration. For $\mathcal{P}=0.1$ the statistical number of  isolated dipoles is negligible  if compared to the number of dipoles of the entire grain, but this number rises sharply with porosity. Therefore, only particles with porosities up to $\mathcal{P}=0.6$  are considered in this paper.
\begin{figure}[t!]
	\centering
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,1.png}}
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,2.png}}
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,3.png}}
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,4.png}}
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,5.png}}
		\subfigure{\includegraphics[width=0.3\linewidth]{Bilder/Kap2/Teilchenquerschnitt/P=0,6.png}}
	\caption{Particle cross sections through the middle of the grain for porosities from $\mathcal{P}=0.1$ to $\mathcal{P}=0.6$.}
	\label{Teilchenquerschnitt}
\end{figure}
\begin{table}[t!]
 \centering\vspace{3mm}
\caption{Number $ N $ of dipoles for  particles with  porosity $\mathcal{P} $.}\vspace{-3mm}
\begin{tabular}{|c|ccccc|}\hline
 \large{$\mathcal{P}$}&$\mathbf{0.1}$&$\mathbf{0.2}$&$\mathbf{0.3}$&$\mathbf{0.4}$&$\mathbf{0.5}$\\\hline
$N$&467849&415866&363882&311899&259916\\\hline
\end{tabular}
  \label{sovieleNs}
\end{table}
\subsection{$\beta$-ratio and blowout size}
\label{Motivation1}
We imagine a spherical grain in the orbit of a central star that is attracted by stellar gravitation and repelled by the radiation force. With decreasing radius, the radiation  force becomes increasingly important. As a consequence, there is a minimum particle radius $a_{\mathrm{BO}}$, called blowout size, at which the particle is blown out of the system and which can be calculated as a function of the  grains' optical properties, the stellar luminosity $L_*$, and stellar mass $M_*$ (\citealt{BurnsLamy}, \citealt{Artymowicz}). By modeling the density and grain size distribution of debris disks, a minimum grain radius is derived, which is often significantly above (a factor of $\sim$2 up to one magnitude in some cases) the value calculated under the assumption of compact grains (e.g. HD 104860, HD 8907, HD 377, HD 107146, HD 61005, HD 191089; \citealt{Roccatagliata2009}, \citealt{Ertel2011}). Despite model degeneracies, particularly between minimum grain sizes and inner disk radii, there have been several attempts to explain this discrepancy. A more detailed grain size distribution, derived in collisional evolution studies of debris disks and resulting in an overdensity of small particles (\citealt{Thebault2003}, \citealt{Krivov2006, Krivov2008}), can explain a factor of two. Grain segregation (\citealt{Roccatagliata2009}) or the occurrence of ice (\citealt{Greenberg1990}) affect the value of the blowout size as well (\citealt{Augereau2001}). However, another possible explanation for this problem can be the nature of the porous particles, which requires more investigations, since porosity influences the scattering and absorption properties of the particles (\citealt{Voshchinnikov1999}, \citealt{Vosh1, Vosh2}).
\begin{table}[b!]
	\centering
\vspace{3mm}
\caption{The physical properties of  main sequence stars (\citealt{BinneyMerrifield}) and respective stellar constant $C_{*}$ (see text for details).}
\vspace{-3mm}
	\begin{tabular}{clllll}\hline\hline\vspace{-0.3cm}\\
\vspace{0.0cm}Spectral type&$\hspace{-0.15cm}\unit[T_{*}]{[K]}$&$\hspace{-0.3cm}M_{*}\hspace{0.05cm}[M_{\odot}]$&$\hspace{-0.3cm}R_{*}\hspace{0.05cm}[R_{\odot}]$	&$\hspace{-0.2cm}C_{*}\hspace{0.05cm}[C_{\odot}]$&$\hspace{-0.1cm}L_{*}\hspace{0.05cm}[L_{\odot}]$ \\\hline
A0	     &9520&$2.9$&$2.4$&$1.99$&$42.5$\\
A5	     &8200&$2.0$&$1.7$&$1.45$&$\enspace11.7$\\
F0	     &7200&$1.6$&$1.5$&$1.41$&$\enspace5.4$\\
F5	     &6440&$1.3$&$1.3$&$1.3$&$\enspace2.6$\\
G0	     &6030&$1.0$5&$1.1$&$1.15$&$\enspace1.4$\\
G5	     &5770&$0.9$2&$0.92$&$0.92$&$\enspace0.84$\\
K0	     &5250&$0.79$&$0.85$&$0.91$&$\enspace0.49$\\
K5	     &4350&$0.67$&$0.72$&$0.77$&$\enspace0.17$\\\hline
\end{tabular}
				 \label{CStern}
\end{table}
\subsubsection{Expression for the $\beta$-ratio}
We now derive an expression for the $\beta$-ratio, the ratio of radiation ($F_{\mathrm{rad}}$) to gravitational force ($F_{\mathrm{gra}}$),
\begin{align}
\beta:=\frac{F_{\mathrm{rad}}}{F_{\mathrm{gra}}}. \label{GlBetaallg}
\end{align}
Under the assumption of an optically thin disk, the resulting radiation force is given by
\begin{equation}
F_{\mathrm{rad}}=\frac{\pi^2 a^2}{c}\frac{R_{*}^2}{r^2}\int Q_{\mathrm{pr}}(\lambda)\,B_{\lambda}(T_*) \,\mathrm d\lambda,\label{GlFrad}
\end{equation}
(\citealt{Koehler02, Koehler04}) where  the star is considered as a black body with  effective temperature $T_*$,  radius $R_{*}$ and  mass $M_{*}$. The quantity $B_{\lambda}(T_*)$ is the Planck function, $c$ is the speed of light, and $Q_{\mathrm{pr}}(\lambda)$ is the wavelength-dependent efficiency factor of the radiation pressure,
\begin{equation}
Q_{\mathrm{pr}}=Q_{\mathrm{abs}}+Q_{\mathrm{sca}}(1-g),
\end{equation}
which is a function of the absorption ($Q_{\mathrm{abs}}=C_{\mathrm{abs}}/(\pi a^2)$) and scattering cross section ($Q_{\mathrm{sca}}=C_{\mathrm{sca}}/(\pi a^2)$), and the  asymmetry factor  $g$. For a given grain mass $m_{\mathrm{g}}= 4/3\pi a^3(1-\mathcal{P})\rho$ the gravitational force on the particle amounts to
\begin{equation}
F_{\mathrm{gra}}=\gamma\, \frac{M_{*}m_{\mathrm{g}}}{r^2}=\gamma\, \frac{4\,\pi\,M_{*}\, a^3\,\rho}{3\,r^2} (1-\mathcal{P}), \label{GlFgra}
\end{equation}
where $\gamma$ is the gravitational constant. Using the Eqs.  \ref{GlBetaallg}, \ref{GlFrad} and \ref{GlFgra} delivers
\begin{equation}
\beta=\,C_{*}  \frac{1}{a} \frac{1}{(1-\mathcal{P})} \frac{1}{\rho} \int Q_{\mathrm{pr}}(\lambda)\, B_{\lambda}(T_*) \,\mathrm d\lambda,
\label{betaGleichung}
\end{equation}
with
\begin{equation}
C_{*}:=\unit[117.76]{\frac{kg\,s^3}{m^4}}\,\frac{R_{*}^{2}}{M_{*}}.\label{Nikolaus}
\end{equation}
For the Sun one thus derives $C_{*}=C_{\odot}=2.865 \cdot \unit[10^{-11}]{s^{3}\,m^{-2}}$. The quantity $C_{*}$ is a function of stellar parameters alone, while the other factors in front of the integral in Eq. \ref{betaGleichung} represent the dust properties. The integral reflects the interaction between dust and star. In Table \ref{CStern}, the factor  $C_{*}$ is presented  for main sequence stars of spectral type A to K. The stellar parameters are taken from \citet{BinneyMerrifield}, as published in \citet{SchmidtKaler}.

The particle is ejected from the system, if $\beta (a)>1/2$. A particle that initially moves on a circular orbit is compelled  on an elliptic orbit for $\beta <0.5 $. The trajectory is parabolic (hyperbolic) for $ \beta = 0.5\hspace{0.2cm} (> 0.5 )$, and the particle leaves the system (\citealt{Krivov2006}).

We would like to remind the reader that in the literature (see \citealt{BurnsLamy}, \citealt{Artymowicz}, \citealt{Kruegel}, \citealt{Hahn}) an approximation equation is usually  given that neglects the wavelength dependence of $Q_{\mathrm{pr}}$. In the limit of the geometrical optics, $Q_{\mathrm{pr}}$ is equal to 1, resulting in
\begin{align}
\beta= 0.577\left(\frac{\rho}{\mathrm{g}\, \mathrm{cm}^{-3}}\right) ^{-1} \left(\frac{a}{\mu \mathrm{m}}\right)^{-1} \left(\frac{L_{*}}{L_{\odot}}\right) \left(\frac{M_{*}}{M_{\odot}}\right)^{-1}. \label{betakurzundeinfach}
\end{align}
Equation  \ref{betakurzundeinfach} is easy to handle and  therefore suitable for a  rough estimation of the blowout size. However, for more precise studies (as required in our investigations)  the wavelength dependence of $Q_{\mathrm{pr}}$ expressed in Eq. \ref{betaGleichung} must be considered.
\subsubsection{Previous studies}
The influence of porosity on the radiation pressure has already been considered  in previous studies.
\cite{Mukai92}, \cite{Kimura1997}, and \cite{Koehler2007} have examined porous aggregates with fractal structures, ballistic particle-cluster aggregates (BPCA), and ballistic cluster-cluster aggregates (BCCA), which are described in terms of the fractal dimension (e.g. \citealt{Witten1986}).
These aggregates are two extreme cases of relatively compact and highly porous aggregates, whereas we apply a grain model that allows us to increase the porosity step by step, permitting an analysis of the physical dust properties with changing porosity.
\cite{Mukai92} investigated the $\beta$-ratio based on Maxwell Garnett effective medium theory (\citealt{Garnett1904}), and \cite{Kimura1997} used the Bruggeman rule (\citealt{Bruggeman1935}). \cite{Hage1990} assessed the accuracy of $Q_{\mathrm{abs}}$ when determined with Maxwell Garnett, while \cite{Bazell1990} report a discrepancy at longer wavelengths. \cite{Voshchinnikov1999} found that effective medium theories are  considerably worse for calculating scattering cross sections and the asymmetry factor $g$ than for extinction cross sections.

In \cite{Koehler06,Koehler2007} the DDA is applied to simulate light scattering by irregular aggregates. They calculated the optical properties of larger grains only
 for one wavelength ($\lambda=\unit[0.6]{\mu m}$) and thus neglect the wavelength dependence of $Q_{\mathrm{pr}}$. In our study the number of dipoles is much larger, which allows us to calculate the optical properties for a wide wavelength range and for grains up to $a=\unit[4]{\mu m}$.  We then use the obtained data to investigate not only the $\beta$-ratio, but also the blowout size for various porosities, stellar temperatures, and number of dipoles, and simultaneously calculate the dust temperature of porous grains, especially the one of the blowout grains. This gives a comprehensive overview of porous grains in debris disks.

\section{Results for the efficiency factor of absorption}
\label{firstres}
The $\beta$-ratio of a dust grain is a function of the optical properties. The simulation software DDSCAT delivers the quantities $Q_{\mathrm{abs}}$, $Q_{\mathrm{sca}}$, and $g$ for each wavelength and radius, therefore we investigate the absorption cross sections  for porous  particles with radius  $a= \unit[1]{\mu m}$ (upper image of  Fig. \ref{qabsverpor}). The porosity varies in steps of $0.1$ from $\mathcal{P} = 0.0 $ to $0.6$. To emphasize the dependence on porosity, the curves are normalized to the values of compact spheres ($Q_{\textup{abs},0}$) in the bottom image of Fig. \ref{qabsverpor}.  The relative differences of $Q_{\textup{abs}}$ increase with porosity for all wavelengths lower than $\unit[25]{\mu m}$. $Q_{\textup{abs}}$ drops with increasing porosity for wavelengths from $0.2$ to $\unit[25]{\mu m}$ and increases for $\lambda<\unit[0.2]{\mu m}$. For $\lambda>\unit[50]{\mu m}$, $Q_{\textup{abs}}$ increases with porosity up to $\mathcal{P}=0.3$  and  then decreases again. The values for the porosity $\mathcal{P} = 0.6 $ are $ 0.21$ to $1.13$ times larger than the ones for compact spheres. Around $\lambda\sim\unit[1]{\mu m}$, the curves have a wavy pattern, which diminishes with increasing porosity.

Furthermore, we calculated the absorption cross sections of the same grain with an effective medium theory (Fig. \ref{qabsverporEMT}), using the Bruggeman rule (\citealt{Bruggeman1935}). Besides the main similarity of both figures, the main differences are found for $\lambda<\unit[0.2]{\mu m}$ and  $\lambda>\unit[20]{\mu m}$. The values for the porosity $\mathcal{P} = 0.6 $ are $0.25$ to $1.2$ times larger than the ones for compact spheres. In addition, the wavy pattern around $\lambda\sim\unit[1]{\mu m}$ is more pronounced and can be detected also for $\mathcal{P} = 0.6$.

\section{Blowout size for different parameter}
\label{Kapitel4}
We determine the blowout size as a function of the porosity and the stellar luminosity.

\subsection{Blowout size for porous particles in the solar system}
\label{Abschnitt36}
At first we investigate the impact of grain porosity on the  blowout size of the solar system. For this purpose, the $\beta$-distributions of compact spheres and porous particles are determined. The effective temperature of the Sun is $T_*=\unit[5777]{K}$, and the porosity  varies in steps of $0.1$ from $\mathcal{P} = 0.0 $ to $0.6$. The distributions are presented in Fig. \ref{BetaSonne}, and the corresponding blowout sizes are listed in Table \ref{BO0}.

\begin{figure}[t!]
	\centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap3/VerschiedenePorengDDA.pdf}
\includegraphics[width=1.0\linewidth]{Bilder/Kap3/VerschiedenePorengNormiertDDA.pdf}
	\caption{Wavelength-dependent absorption cross section $Q_{\textup{abs}}$ as a function of porosity $\mathcal{P}$. The particle radius is
$a=\unit[1.0]{\mu m}$.  Note the two characteristic silicate peaks  at $\lambda\sim\unit[10]{\mu m}$  and $\unit[18]{\mu m}$. In the bottom image the results are normalized to the values of compact spheres, $Q_{\textup{abs},0}$.}
	\label{qabsverpor}
\end{figure}
\begin{figure}[t!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap4/Betafaktor/BetaSonneeng.pdf}
\caption{The $\beta$-ratio as a function of the grain radius $a$ and porosity $\mathcal{P}$ for the solar system. The intersections of the different distributions  with the 0.5 limit mark  the blowout size $a_{\mathrm{BO}}$.}
\label{BetaSonne}
\end{figure}
\begin{table}[b!]
\renewcommand{\arraystretch}{1.15}
	\centering
\vspace{3mm}	\caption{Blowout size as a function of grain porosity $\mathcal{P}$ in the solar system.}\vspace{-3mm}
		\begin{tabular}{c|c|c|c|c|c|c}
$\mathcal{P}$              &$0.0$&$0.1$&$0.2$&$0.3$&$0.4$&$0.5$\\\hline
$a_{\mathrm{BO}}\,[\mu$m$]$&$0.455$&$0.500$&$0.549$&$0.603$&$0.678$&$0.744$
\end{tabular}
		 \label{BO0}
\end{table}
 \begin{figure}[t!]
	\centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap3/EMTBruggeman.pdf}
\includegraphics[width=1.0\linewidth]{Bilder/Kap3/EMTBruggemanNormiert.pdf}
	\caption{Same as Fig. \ref{qabsverpor}, but derived with effective medium theory (EMT, Bruggeman rule).\newline~\newline~\newline~}
	\label{qabsverporEMT}
\end{figure}
            \begin{figure}[h!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap4/Betafaktor/Beta_T_eng.pdf}
\caption{The $\beta$-ratio as a function of the grain radius $a$ for stars  of various spectral type (different stellar temperature). The particles are compact spheres.}
\label{BetaTemp}
\end{figure}

\begin{enumerate}
\item The $\beta$-value strongly increases with radius, reaching a maximum, and then starts falling off. With increasing porosity, the maximum of the $\beta$-distribution decreases and shifts towards larger radii. Thus, the maximum is the largest for compact spheres. Furthermore, the slope at the larger radii becomes flatter.
 \item The blowout size of compact spheres is $a_{\mathrm{BO}}=\unit[0.46]{\mu m}$. For comparison, the  value  $\unit[0.33]{\mu m}$ is obtained with the approximation Eq. \ref{betakurzundeinfach}. In \citet{Mukai92}  a blowout size between $\unit[0.3]{\mu m}$ and $\unit[0.35]{\mu m}$ can be estimated, and in \citet{Koehler02} between $\unit[0.45]{\mu m}$ and $\unit[0.5]{\mu m}$ (see paper, Figs. 4b and 1, resp.).
\item The higher the porosity, the larger the blowout size. For $ \mathcal{P} = 0.6 $ the blowout size is $ a_{\mathrm{BO}} = \unit[0.84]{\mu m}$, $1.8$ times larger than for $\mathcal{P} =0.0$. This factor is comparable to the factor between the minimum grain size obtained with disk modeling and the value calculated under the assumption of compact spheres.
\end{enumerate}

\subsection{Blowout size of stars of various spectral type}
\label{Abschnitt37}
The influence of different stellar luminosities on the blowout size is investigated. For this purpose, we consider compact spherical grains with  particle radii up to $\unit[4]{\mu m}$, since higher luminosities increase the radiation force and thus the blowout size. The values for $T_*$ and $C_{*}$ for the eight different spectral types from K0 to A5 are summarized in Table \ref{CStern}. The  resulting $\beta$-distributions are shown in Fig. \ref{BetaTemp}.
\begin{enumerate}
 \item The higher the luminosity, the higher the $\beta$-values, whereby the blowout size increases. In addition, the maximum of the\newpage~\newpage~\newpage $\beta$-distribution shifts to smaller particle radii for higher luminosities.
 \item For some luminosities one finds $ \beta <0.5 $ for all particle radii, so there no blowout size exists in these systems. In particular, only stars
with temperatures $T_*>\unit[5250]{K}$ have a blowout size. There is also no  blowout size at lower temperatures for porous grains, since the maximum  of the $\beta$-distribution is the greatest for compact spheres, and it decreases with increasing porosity (Sect. \ref{Abschnitt36}).
 \item The blowout size  at $T_*=\unit[9520]{K}$ is larger than $\unit[4]{\mu m}$, and even higher values are expected for porous  particles. Calculations of the optical properties of such large grains exceed our computational capabilities, therefore stars with $T_* \ge\unit[9520]{K}$ are not investigated further.
 \item Several temperature curves intersect the $0.5$ limit  in the examined particle radii interval even twice, whereby two values for the blowout size exist (e.g. the $T_*=\unit[5770]{K}$ curve). Further forces are acting on  very small particles, such as the Poynting-Robertson effect and the Lorentz force, which are negligible for larger grains, but have to be taken into account for the balance of forces on very small grains (\citealt{Grun2001}).
\end{enumerate}

\subsection{Parameter space}
\label{Abschnitt38}
As shown in the previous two sections, the blowout size depends on both the grain  porosity and the stellar temperature. We now determine the blowout size for each parameter configuration. The computational effort is large, especially  particles with radii $ a> \unit[2]{\mu m} $ increase the calculation time dramatically. We generate and evaluate the data for the following parameter space:
\begin{itemize}
 \item seven porosities: $\mathcal{P}=0.0$, $0.1$, $0.2$, $0.3$, $0.4$, $0.5$, and $0.6$,
 \item five stellar temperatures: $T_*=\unit[5770]{K}$, $\unit[6030]{K}$, $\unit[6440]{K}$, $\unit[7200]{K}$, and $\unit[8200]{K}$,
 \item six number of dipoles, from $54,432$ to $519,832$ dipoles.
\end{itemize}
We vary the total number of dipoles and thus the size of the inner voids to investigate the influence of different particle structures.
The calculated blowout sizes of the special particle presented in Sect. \ref{genera} are illustrated in Fig. \ref{sechsL} and listed in Table \ref{RESULT}. Missing table entries imply a blowout size larger than $\unit[4]{\mu m}$ and are thus not computable within the parameter settings.

Figure \ref{sechsL} again reveals the blowout size increasing  both with grain porosity and stellar temperature. For  $ T_* =\unit[5770]{K}$ the blowout size of porous grains ($\mathcal{P} = 0.5 $) is larger by a factor of $1.5$  if compared to compact spheres. The higher the temperature, the stronger the effect, so that  the factor amounts to $2.8$ for $T_* = \unit[7200]{K}$. These factors  are close to matching  the existing discrepancy mentioned in Sect. \ref{Motivation1}. The variation in the number of dipoles causes a dispersion of the blowout sizes. This dispersion increases also both with $\mathcal{P}$ and $T_*$. In most cases, $a_{\mathrm{BO}}$ rises with decreasing number of dipoles. However, there are exceptions. The largest deviations from the other calculated blowout sizes occur for the lowest number of dipoles, the coarsest particles, whose $a_{\mathrm{BO}}$ are significantly larger than those from the other ones (triple dotted lines).

Figure \ref{sechsL} can be used to estimate  the blowout size for a given grain porosity $ \mathcal{P}  $ and stellar temperature $T_*$. The different blowout sizes  at constant porosity and temperature, caused by the varying number of dipoles, set the range of applicability in which the blowout size  can be found.
\begin{figure}[t!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap4/Betafaktor/Blowout_P_eng.pdf}
\caption{Blowout size $a_{\textrm{BO}}$ as a function of porosity $\mathcal{P}$ and stellar temperature $T_*$ for various number of dipoles. Different  colors represent different  temperatures. The values for the special particle presented in Sect. \ref{genera} are illustrated as the solid line.}
\label{sechsL}
\end{figure}
\begin{table}[t!]
\centering
\vspace{3mm}\caption{Blowout size in $\mu$m as a function of grain porosity $\mathcal{P}$ and  stellar temperature $T_*$.}\vspace{-3mm}
\begin{tabular}{|c|ccccc|}\hline
&\multicolumn{5}{c|}{$\unit[T_*]{[K]}$}\\
$\mathcal{P}$&5770&6030&6440&7200&8200\\\hline
\vspace{-3mm}&&&&&\\
 $\mathbf{0.0}$&$0.42$&$0.60$&$0.83$&$1.29$&$2.15$\\
$\mathbf{0.1}$&$0.45$&$0.67$&$0.94$&$1.50$&$2.45$\\
$\mathbf{0.2}$&$0.50$&$0.75$&$1.07$&$1.75$&$2.94$\\
$\mathbf{0.3}$&$0.54$&$0.86$&$1.25$&$2.12$&$3.67$\\
$\mathbf{0.4}$&$0.60$&$0.99$&$1.52$&$2.69$&\\
$\mathbf{0.5}$&$0.64$&$1.18$&$1.93$&$3.64$&\\
$\mathbf{0.6}$&$0.70$&$1.51$&$2.75$&&\\\hline
\end{tabular}
			 \label{RESULT}
\end{table}
\subsection{Fitting model}
\label{Abschnittfit}
In this section  an approximation function  $ f \, (\mathcal{P}, T_* $) for the  blowout size is  derived. We find that the results of the special particle presented in Sect. \ref{genera} can be analytically approximated very well using the following equation:
\begin{align}
a_{\mathrm{BO}}\left(\mathcal{P},\,T_*\right)=(k_1 T_*+&k_2) \cdot \mathcal{P}^{\alpha}\,+\,\left(k_3 T_*+k_4\right), \label{GlFit}\\[0.3cm]
k_1=\unit[5.07\cdot 10^{-3}]{\frac{\mu m}{K}},&\quad k_2=\unit[-28.85]{\mu m},\nonumber\\[2mm]
k_3=\unit[7.01\cdot 10^{-4}]{\frac{\mu m}{K}},&\quad k_4=\enspace\unit[-3.65]{\mu m},\nonumber\\[2mm]
\alpha=1.781-&\frac{61.72\,\mathrm{K}}{T_*\,-\,5670\, \mathrm{K}}.\nonumber
\end{align}
It contains seven coefficients (three for $\alpha$, and the $k_i$,  $i \in \mathbb{N}_{\le 4}$).

The fit is  presented in Fig. \ref{Fitmodell}. The relative deviation  between fit and measured values is for the highest temperature lower than $8\,\%$, so Eq. \ref{GlFit} is a good way to estimate the size of the blowout. An online tool for calculating the blowout size based on this approximation function is available at
\\ \textit{http://www1.astrophysik.uni-kiel.de/blowout/}.
\begin{figure}[t!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap4/Fitbilder/Blowout1LochMitFit.pdf}
\caption{Calculated blowout sizes (solid line) and derived approximation function (dotted lines). Using the equation, it is possible to estimate $a_{\mathrm{BO}} $ as a function of grain porosity and stellar temperature.
}
\label{Fitmodell}
\end{figure}

\subsection{$\beta$ influenced by other effects}
\label{Abschnitt39}
We discuss other possible effects which might influence the $\beta$-ratio.

\subsubsection{Particle modeling}
The particles  used in this paper have a spherical shape, into which holes are formed. Besides prolate and oblate shapes, real particles can have a much more complex non symmetric structure. However, the vast variety of particle shapes cannot be examined. The spherical shape with inclusions was chosen  as representative of all porous and arbitrary shaped particles.

It should be noted that large particles are generally more porous than smaller ones, because they can be seen as agglomerates of smaller subunits.
\citet{LamyGrun} modeled  the density of small grains by $\rho=2.2-1.4\,(a^2+a)$, where $a$ is in $\mu$m and $\rho$ in $\textup{g}\, \textup{cm}^{-3}$. With increasing particle radius this  density law leads to higher $ \beta $-values.

There is no unique definition of the optical properties and bulk densities of what is considered as an ``astronomical silicate``. As the $\beta $-ratio is inverse to the density, the choice of $\rho$ has a strong impact on the blowout size. It is  also conceivable that individual particles consist of several materials.

The mentioned  points   do not lead to errors in the calculations. Instead, they show the possible complexity  and variety of  particles in the disk, hence the difficulty in specifying the blowout size of a  stellar system, since a separate  $\beta $-value can be allocated to each particle and  even to each particle orientation.

\subsubsection{Central star}
The stellar component is considered as a black body with the effective temperature $T_*$. In contrast to this, \citet{Lamy74b} and  \citet{Artymowicz} motivated to use an observed  or a modeled photospheric spectrum (e.g. Kurucz model). We did not consider this in our parameter space study because fundamentals are first investigated. In the treatment of a real object, the shape of the spectrum should be used. Furthermore, $C_{*}$ is calculated for parameters of a main-sequence star model. Real stars can deviate from these values, so real values should be used for stellar mass and radius if available.
\subsubsection{Ejection limit}
The ejection limit $\beta_{\mathrm{ejection}}=0.5$ only applies to particles  that have been produced by planetesimals that move in circular orbits, i.e. for which the orbit eccentricity is $e  = 0.0$. The general $\beta$ threshold depends on the position $\Phi$ of the elliptical orbit, where the particle is set free, and is  $  \beta_{\Phi,\mathrm{ejection}}=\frac{1}{2}\left(\frac{1\,-\,e^2}{1\,+\,e\,\cos{(\Phi})}\right)$. Even  eccentricities as low as $ e = 0.1 $ can cause $ \beta$-values from $ 0.45 $ to $0.55 $. Owing to the different  ejection conditions for each particle, the blowout size depends on the eccentricity. This influence  is  quite strong compared to the other effects discussed above.
\subsubsection{Further  forces acting on dust grains in debris disks}
The derivation of Eq. \ref{betaGleichung} for  $\beta$ only considers gravitational and radiation forces. In addition, the Poynting-Robertson effect and stellar wind drags are acting  on the particles, and  in the case of charged particles also the Lorentz force. The magnitude of these forces depends strongly on the particle size. The gravitational force dominates for particles with radii $a>\unit[1]{\mu m}$. For particles with radii $\unit[0.05]{\mu m}$ or lower, the Lorentz force prevails. For intermediate particle radii, the radiation force is important   beside gravitation and Lorentz force. In \citet{Grun99}, the various forces  are listed and compared for different particle radii.

\section{Dust temperature of fluffy grains}
\label{Staubtemp}
Finally, the influence of porosity on the dust equilibrium temperature is investigated. For this purpose the dust temperature $T_{\mathrm{g}}$ is determined if the grains are only heated by direct stellar radiation. When taking the energy conservation into account, the distance $r$ of the particle from the star is
\begin{equation}
r=\frac{R_*}{2}\sqrt{\frac{\int_0^\infty B_{\lambda} \left(T_*\right) Q_{\mathrm{abs}}\left(a,\lambda\right)  \,\mathrm d\lambda }{\int_0^\infty B_{\lambda}\left(T_{\mathrm{g}}\right) Q_{\mathrm{abs}}\left(a,\lambda\right)  \,\mathrm d\lambda }}\, ,\label{AbstanddT}
\end{equation}
(\citealt{WolfHillenbrand2003}). We calculated the dust temperature at a distance of $r=\unit[50]{AU}$ for stellar temperatures $T_*=\unit[5770]{K}$ and $T_*=\unit[7200]{K}$ and illustrate them in Figs. \ref{TempT=5770K} and \ref{TempT=7200K}, respectively.

\begin{figure}[h!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap5/Tdust5770K50AU.pdf}
\caption{Dust temperature $T_{\mathrm{g}}$ at the distance of $\unit[50]{AU}$ from a star with the effective temperature $T_*=\unit[5770]{K}$, depending on the grain radius $a$ and porosity $\mathcal{P}$. The blowout sizes are marked as crosses.}
\label{TempT=5770K}
\includegraphics[width=1.0\linewidth]{Bilder/Kap5/Tdust7200K50AU.pdf}
\caption{Same as Fig . \ref{TempT=5770K}, only for the stellar temperature $T_{*}=\unit[7200]{K}$.}
\label{TempT=7200K}
\end{figure}
\begin{figure}[h!]
 \centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap5/TaBO.pdf}
\caption{Dust temperature of the blowout size grains $T_{\mathrm{BO}}$ as a function of porosity $\mathcal{P}$ and the distance $r$ from the central star. The stellar temperature is $T_*=\unit[5770]{K}$.}
\label{TaBO}
\end{figure}
\begin{figure}[h!]
\includegraphics[width=1.0\linewidth]{Bilder/Kap5/TdustSiliAC1.pdf}
\caption{Dust temperature $T_\textup{g}$ at the distance of $10^4$ stellar radii from a star with effective temperature $T_*=\unit[2500]{K}$, depending on the porosity and the effective radius  $a_{\mathrm{eff}}=(1-\mathcal{P})^{\nicefrac{1}{3}}\, a$. The dust material is a 1:1 mixture of astronomical silicate and amorphous carbon.}
\label{TempAC1}
\end{figure}
\begin{enumerate}
\item The temperature of the smallest particles  increases with the grain radius up to a maximum before it falls off steeply for larger radii. In addition, the maximum shifts with increasing porosity from $\unit[0.28]{\mu m}$ for $\mathcal{P}=0.0$ to $\unit[0.5]{\mu m}$ for $\mathcal{P}=0.6$ in the case of $T_*=\unit[5770]{K}$, and from $\unit[0.24]{\mu m}$ for $\mathcal{P}=0.0$ to $\unit[0.43]{\mu m}$ for $\mathcal{P}=0.6$ in the case of $T_*=\unit[7200]{K}$.
\item For particles with radii $\unit[0.03]{\mu m}<a< \unit[1.2]{\mu m}$ the following is valid. The higher the porosity, the colder is the particle. For a fixed radius, the drop in temperature decreases with increasing porosity. For $\mathcal{P} = 0.6$  and radii $a<\unit[0.03]{\mu m}$, the temperature is  even higher than for corresponding radii at $\mathcal{P}=0.5$.
\item The blowout sizes as calculated in Sect. \ref{Abschnitt38} are marked in the figures and reveal that most of the presented dust particles will be blown out of the system.
\end{enumerate}

The temperature of the blowout grains is an important parameter, because this is the quantity that is derived from observations. We calculated the dust temperature of the blowout grains $T_{\mathrm{BO}}$ at different distances from the star, since it might depend on the cooling efficiency, and hence on the stellar distance (Fig. \ref{TaBO}). The temperature of the blowout grains is at all distances for porous grains slightly lower than for compact spheres. For example, at $r=\unit[5]{AU}$ and for $\mathcal{P}=0.6$, the dust temperature is $\unit[22]{K}$ below the one for $\mathcal{P}=0.0$. At $\unit[100]{AU}$ this difference is $\unit[9.2]{K}$.

\cite{Vosh2} determined the dust temperature for porous particles  using the effective medium theory once and the method of layered spheres once. The material  was a mixture of  astronomical  silicate  (\citealt{DraineLaor1993}) and amorphous carbon (\citealt{Rouleau1991}) with a weighting of 1:1. Comparing our grain model  with  the studies from \cite{Vosh2}, we furthermore calculated  the dust temperature for a mixture of astronomical silicate and amorphous carbon, which is presented in Fig. \ref{TempAC1} as a function of the effective radius,  $a_{\mathrm{eff}}=(1-\mathcal{P})^{\nicefrac{1}{3}}\, a$. The central star has an effective temperature of $T_*=\unit[2500]{K}$, and the assumed grain distance is  $r = 10^4\,R_{*}$.

The results of \cite{Vosh2} are comparable to the ones calculated with the DDA. For the layered spheres the temperature decreases  with increasing porosity. This statement applies to the EMT only up to a porosity of $\mathcal{P} = 0.7 $, when the temperature increases again. The decrease in temperature for lower porosities can also be observed in our approach. \citet{Greenberg1990} ascertained in their studies the increasing of temperature at very high porosities, where the temperature approaches the value of subunits of the porous particle. Certainly the behavior differs for the lower porosities, since the temperature remains constant or increases slightly. \citet{Vosh2} have also performed investigations  for different stellar temperatures and distances  and found the same behavior. For high porosities, the differences between the method of layered spheres and the EMT could reach $\sim 15\, \%$, and  for compact grains they were less than $1 \,\%$.

In conclusion,  porous  particles with radii up to $\unit[1.3]{\mu m}$  are generally colder than compact spheres, and the maximum of the infrared emission is thus shifted to longer wavelengths. Our results agree very well with those of \citet{Vosh2}.

\section{Conclusions}
When modeling the density and grain size distribution in debris disks, the minimum particle size is often significantly larger than the corresponding blowout size.
We investigated porous dust grains, which provide a possible explanation. Since the introduced $\beta$-ratio depends on the optical properties of the grain, we determined the absorption cross sections of porous particles as a function of the porosity.  The blowout sizes  of six different sample stars and seven porosities (including compact spheres)  were calculated. We found that the blowout size increases with grain porosity and stellar temperature. It should be noted that both the choice of the bulk density, as well as the particle ejection limit, has a strong influence on the obtained results. An approximation equation was derived from the numerically calculated values with which the blowout size can be estimated. Finally, the dependence of the dust temperature on  particle radius and porosity was investigated. It was found that porous particles  are colder than compact spheres, and the temperature of blowout grains in particular decreases for porous particles.

The optical properties of porous particles were determined with the DDSCAT for an extended range of wavelengths and particle radii. These efficiency factors of absorption, scattering, and radiation pressure are summarized in several tables and are available for further applications. An online tool for calculating the blowout size based on the derived approximation function is available at  \textit{http://www1.astrophysik.uni-kiel.de/blowout/}.
\begin{figure}[b!]
	\centering
\includegraphics[width=1.0\linewidth]{Bilder/Kap2/ersteTestsKapPoros/MieDDAklein.pdf}
\includegraphics[width=1.0\linewidth]{Bilder/Kap2/ersteTestsKapPoros/MieDDAgross.pdf}
	\caption{Absorption cross section  $Q_{\textup{abs}}$ derived with DDA (crosses) and Mie (solid lines) as a function of the wavelength. The particles are compact spheres  with radii $a$ from $0.5$ to $ \unit[5.0]{\mu  m}$ (above) and  $ 10.0 $ to $ \unit[100.0]{\mu m}$ (bottom).}
	\label{Vollkugeln}
\end{figure}
\begin{acknowledgements}
We would  like to  thank Steve Ertel for a helpful discussion. F.K. thanks the DFG for financial support under contract WO 857/7-1.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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This achievement is achieved when you fail the same mission three times in a row.
On a mission where you only have a construction yard just sell it repeatedly or if you have a few troops have them killed.
Did this one today on The Pentagon (2nd level GDI).
At the start of the level you have to restore power to some buildings to get the Pentagon back online. The buildings are under attack.
There are currently no gaming sessions for the Simon Says you LOSE achievements that you can join - why not register and make a new session?


There is a lot of money to be made from CPA Marketing, but there is also a dark side that many people do not know about or maybe refuse to believe. The problem with the CPA industry is that it can be very unethical. There is no formal governing organization to regulate the industry.
As you may learn, cash making fortunes continue to become larger on the internet. One year its one thing, while the next year its completely different. As you learn your Internet Marketing course, you want to stay grounded and focused.


text:
FECA, DEA and OIG
Who is an employee entitled to workers' compensation benefits anyhow?
If it's the Federal Government, employees include informants and whistleblowers who remain anonymous due to their intentionally secret lifestyle as a consequence of their spy status.
Something doesn't smell right...
And because they're so secret, the government doesn't even know how much, or for how long, some of these informants receive compensation under the Federal Employees Compensation Act because no one keeps any records - these people are, after all, confidential sources.
An audit report released yesterday by the Office of the Inspector General, the investigative arm of the U.S. Department of Justice says informants working with the Drug Enforcement Agency also get federal employee workers' compensation and death benefits without any oversight or review, according to a story published this in this morning's issue of WorkCompCentral News.
The OIG report says the DEA has been using FECA to pay informants for more than 30 years, but the cost is unknown because there are only a handful of records for any of the claims.
The report references a DEA manual that states FECA pays benefits when a confidential source is injured or killed as a result of cooperating with the agency. The manual references another DEA document that says non-federal law enforcement officers injured or killed while apprehending someone who committed a federal crime are covered by FECA and suggests this also applies to informants.
The DEA cites United States Code Title 21, Section 886 as the basis for allowing informants to collect comp benefits. But that section simply authorizes the attorney general to pay confidential sources out of DEA funds. It has no relationship to FECA, according to the OIG.
"In our view, 21 U.S.C. 886 does not provide a legal basis for the DEA's position that its confidential sources were appropriately categorized as non-federal law enforcement officers eligible for FECA benefits," the audit says.
After reviewing a draft of the audit report, the DEA said U.S. Code Chapter 5, Section 8101(1)(B) extends FECA benefits to any person working with the federal government and performing jobs similar to what another federal worker might do.
Regardless of whether this section does, in fact, allow the DEA to qualify informants for federal workers' compensation benefits, the OIG said, it is not the legal basis the agency cites in its own policy documents. The agency needs to consult with the Department of Justice "to come to a conclusion about whether there is a legal basis and, if so, whether it is appropriate to extend eligibility for FECA benefits to confidential sources," the audit says.
The extent of confidentiality of this program is highlighted by sources cited in the report who said they don't keep any files on these cases. They rely on the Department of Labor to manage and administer the claims. But the DoL likewise handles confidential cases differently, and likewise keeps nearly zero records on them, so there is no audit trail, no accounting for the cost, no accountability, period.
What OIG has uncovered is alarming. The report cites investigative cases uncovering millions of dollars paid by the DEA to informants for things like housing, while the informant also collects monthly FECA payments.
The DEA in response to a 2005 audit said confidential sources are not "choir boys" and the DEA sometimes has to rely on information from people whose credibility is questionable.
"Therefore, when the DEA submits an application for a confidential source to receive FECA benefits, we believe that the DEA should employ appropriate oversight and evaluate these cases thoroughly," OIG said. "Although the identity of the claimants may be sensitive, this does not alleviate the DEA's responsibility to be judicious stewards of taxpayer dollars and ensure that payments are warranted."
As you might expect on something as embarrassing and culpable as this is, WorkCompCentral's calls to the DEA's Office of Congressional and Public Affairs were not returned Tuesday.
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Can I Lose My Job After Complaining About Sexual Harassment?
Title VII of the Civil Rights Act of 1964 states that employers are prohibited from retaliating against their employees. When an employer fires, demotes or refuses to hire a person as a result of that employees complaints, the employer can be held accountable for violating Title VII.
The purpose of this blog is to make you familiar with retaliation law in the United States and what steps you can take to rectify it.
Retaliation occurs when an employer or supervisor takes adverse action against an employee for voicing a complaint or participating in an investigation.
It is strictly illegal for an employer to retaliate against any of their employees or applicants for employment because of their complaints to the employers illegal conduct or because they cooperate in an investigation against the employer.
It is not uncommon for cases of harassment to give rise to retaliation cases. Often times employers against whom a claim of discrimination or harassment have been filed take adverse action against any individuals who opposed the unlawful acts or assisted in an investigation of those unlawful acts.
As such, if an employee is being sexually harassed in the workplace and they complain about it, their employer cannot take adverse employment actions against them because of their complaints.
To establish a claim of retaliation an employee must meet three elements. 1) The employee engages in a protected activity; 2) Adverse action is taken against the employee; 3) a causal link between the protected activity and the adverse action.
This list is not exhaustive but provides some examples of what constitutes engaging in protected activity.
The employee must also be able to show that they suffered some sort of adverse action due to their complaints. Typically, adverse action could include termination, demotion or even a pay cut.
Lastly, the employee would need to show that the adverse action was taken a result of the employee engaging in a protected activity. This is generally most difficult thing to prove in a retaliation claim.
If an employee feels as though they are being retaliated again in the work place then they should seek to file a claim with the EEOC. The EEEOC will conduct an independent investigation into the employees claim and determine whether or not they can be substantiated. The EEOC may contact supervisors and co-workers due interview them regarding the employees complaints. The EEOC will then provide the employee with a Right to Sue Notice, which allows the employee to pursue a lawsuit against the employer in court..
If you feel as though you're a victim of retaliation you should consider finding an attorney who is experienced in labor law. If you feel as though you are being retaliated against by your employer, you should contact an attorney who has experience in labor and employment law. The laws governing retaliation are complex. There are strict regulations governing the process for filing a lawsuit. Furthermore, there are strict time restrictions, known as statute of limitations, as to when a lawsuit can be filed. The experienced attorneys at Shegerian Conniff are ready to hold your employer accountable, fight for your legal rights, and seek justice. Click here to contact us today or call us at 310-322-7500 for a free consultation.
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Calgary/Edmonton, AB - Joni Mitchell was presented with the Alberta Ballet Founder's Award, honouring her commitment to Alberta Ballet, at Tuesday night's Raising the Barre gala fundraiser held at the Jubilee Auditorium.
"Joni has been an inspiration to us all," said Artistic Director Jean Grand-Maître, "We can all learn something from her passion for the world we live in. I am honoured that I was able to collaborate with her, and Alberta Ballet will be forever changed by her influence."
The evening featured the world premiere of a very early Joni Mitchell recording, The Way It Is, which had never appeared on any of Mitchell's albums. Alberta Ballet company artists also danced excerpts from Joni Mitchell's The Fiddle and The Drum, the groundbreaking collaboration between Mitchell and Grand-Maître. The Honourable Lindsay Blackett, Alberta's Minister of Culture and Community Spirit, was in attendance along with some of the province's top arts supporters.
Thanks to a special print donated by Ms. Mitchell, the inaugural Raising the Barre evening brought in over $100,000. The funds will go towards furthering Alberta Ballet's artistic development, programming and operations.
"It was vital, at an economic time like this, for us to celebrate the successes of not only our art, but our community," said Executive Director Darryl Lindenbach, "the world is so focused on the negative that we often forget the truly great things we have. On Tuesday night Ms. Mitchell reminded us why supporting the arts is so important and just what is possible if you do."
Alberta Ballet sincerely thanks all those who supported the event and helping to ensure the Company continues to play a vital role in arts development in this province, across the country and around the world.
This article has been viewed 1,733 times since being added on November 13, 2009.