text:
Import prices in April 2008
May 14, 2008
The U.S. Import Price Index increased 1.8 percent in April. The 1.8-percent rise followed increases of 2.9 percent, 0.2 percent, and 1.5 percent in March, February, and January, respectively.
Petroleum prices advanced 4.4 percent in April after a 9.2-percent rise in March. Prices for petroleum rose 57.2 percent for the year ended in April following a 1.1-percent drop over the previous 12-month period.
Nonpetroleum prices increased 1.1 percent for the second consecutive month, matching the largest one-month increase for the index since nonpetroleum prices were first published on a monthly basis in December 1988.
The price indexes for overall imports and nonpetroleum imports advanced 15.4 percent and 6.2 percent, respectively, during the past year.
These data are from the BLS International Price program. Import price data are subject to revision. Learn more in "U.S. Import and Export Price Indexes -- April 2008" (PDF) (HTML), news release USDL 08-0663.
Bureau of Labor Statistics, U.S. Department of Labor, The Economics Daily, Import prices in April 2008 on the Internet at http://www.bls.gov/opub/ted/2008/may/wk2/art03.htm (visited September 30, 2016).
Recent editions of Spotlight on Statistics
A look at healthcare spending, employment, pay, benefits, and prices
As one of the largest U.S. industries, healthcare is steadily growing to meet the needs of an increasing population with an increasing life expectancy. This Spotlight looks at how much people spend on healthcare, current and projected employment in the industry, employer-provided healthcare benefits, healthcare prices, and pay for workers in healthcare occupations.
Employment and Wages in Healthcare Occupations
Healthcare occupations are a significant percentage of U.S. employment. Some of the largest and highest paying occupations are in healthcare. This Spotlight examines employment and wages for healthcare occupations.
Fifty years of looking at changes in peoples lives
Longitudinal surveys help us understand long-term changes, such as how events that happened when a person was in high school affect labor market success as an adult.


text:
2009-05-14 / Obituaries
Belton Eugene "Nully or Geno" Nall
March28,1941- May7,2009
Belton Eugene "Nully or Geno" Nall, 68, passed away Thursday morning, May 7, 2009, at his home in Lexington. Funeral services were held Monday, May 11, 2009 at Eagles Wing Christian Center in Lexington, with Pastor Dave Harkreader officiating. Burial followed in the Lexington Cemetery.
Subscription Required!
Subscription Required!
If you are already an online subscriber, please sign in below.

subset: commoncrawl


text:
There might be a pipe with the wrong density for a particular coupling or elbow you have, or you might have to get more piping. Keep the following recommendations in mind the next time you develop a relationship with a plumbing supply company.
There are 2 sorts of perks you can expect to get from a plumbing supply store. The very first set is the official choices they provide dealerships. Often by paying a little members charge, or just registering your business as a wholesale buyer (assuming either you or your company has a wholesale license) is going to save you massively right away. But, aside from this obvious detail, there are typically other perks to working with a company regularly.
The 2nd sort of perk you need to be looking for is client dedication. Does the company attempt their hardest to satisfy customer demands and goals? Here's a good screening approach: Go into the plumbing supply store on a hectic midmorning, when there is a line up to the purchasing counter. Experience how the clerks and staff interact with the plumbing technicians they aid. Are they friendlier? Are they on a first-name basis? This real connection is a good indication that you will be making a clever decision by constructing a relationship with that company in time. To get more information about plumming click on boilerdoctor247.com .
When it concerns company, there has to be more than simply exceptional client service. What type of shipping offers do they organize for last-minute and emergency situations? If your client needed their shower taken care of prior to a huge household gathering, and you required a part ASAP, would they have the ability to ensure that it was overnighted, and guarantee an arrival time?
Likewise inspect to see when their restocking schedule revolves. Simply put, what day of the week do most of their deliveries can be found in? Do they put shipments as quickly as an item gets short on stock, or do they wait to place huge orders at the end of the week? These type of accessibility choices can considerably influence the efficiency and turnaround times you can provide to customers, which will certainly in turn, affect your success.
You might have a better time collaborating with either a sales or operations manager to ensure that your requirements can be met. Get a sincere viewpoint from them when detailing your client volume. With the variety of plumbing technicians they already have being available in, can they handle another?
Has your moms and dad company worked with this supplier before? Speak to your very own manager to get a more comprehensive image of exactly what is readily available. If you're independent, talk to some regional companies, and try to get a concept which plumbing supply business they prefer to work with.


text:
WOW Yuzuru! How does he manage all that in his busy schedule...
Did he take the university entrance exam between NHK and GPF?
WOW Yuzuru! How does he manage all that in his busy schedule...
Did he take the university entrance exam between NHK and GPF?
Congrats to Yuzuru! Though I'll always root for Daisuke, I feel lucky to be a fan while Yuzuru is skating, and it's exciting to realize that he's just starting his climb to excellence.
"I still can't believe that I won, somehow I could manage to hold on because of the score of SP."
"Takahashi-senshu was very strong, he narrowed the gap of the score after FS. If I were him, I could not have done that. I should practice more and more and want to skate better in FP."
This article says that Yuzuru passed an essay examination, and after that, he had an oral examination using Skype on Dec.9 in Sochi. No wonder he got sick from a lot of mental pressure.
I'm verry looking forward to seeing EX!!
Last edited by yude; 12-23-2012 at 11:33 PM.
Last edited by dorispulaski; 12-26-2012 at 08:05 AM. Reason: make link clickable
Awwww, I love this Yuzuru's number, whish he'd skated it all year. Plus R&J, ehat can be better? He's soooo beautiful when he's 100% into music
Last of Samurai perhaps? Or something by a Japanese composer?
This uploader translated the song lyrics and subtitled his NHK version: http://www.youtube.com/watch?v=X1PNaAM37LA I'm glad he performed it again!
As for future programs... I'd actually love for him to skate to something by Joe Hisaishi (not Nausicaa though since Taka already skated to that).


text:
SET 1: Wilson > NICU, Wolfman's Brother, Ocelot, Torn and Frayed, Strange Design, Ginseng Sullivan, Albuquerque, Split Open and Melt, Dirt, Limb By Limb, Run Like an Antelope
SET 2: Rock and Roll > Ghost > If I Could, Backwards Down the Number Line > Prince Caspian, Suzy Greenberg > Also Sprach Zarathustra > The Squirming Coil
ENCORE: Sleeping Monkey, Axilla
Add a Review
Mike Gordon: September 23, 2016
5 days ago
Catskill Chill at New Minglewood
Set 1: Say Something, Jumping, Waking Up Dead[1], Andelmans' Yard, Horizon Line, How Do I Know > Looking for Clues, Don't Chin The Dog, Let's Go[1], Tiny Little World
Encore: Yarmouth Road
[1] Mike Gordon debut.
Phish.net is a non-commercial project run by Phish fans and for Phish fans under the auspices of the all-volunteer, non-profit Mockingbird Foundation.
This project serves to compile, preserve, and protect encyclopedic information about Phish and their music.
Credits | Terms Of Use | Legal
The Mockingbird Foundation is a non-profit organization founded by Phish fans in 1996 to generate charitable proceeds from the Phish community.
And since we're entirely volunteer – with no office, salaries, or paid staff – administrative costs are less than 2% of revenues! So far, we've distributed over $750,000 to support music education for children – 210 grants in 43 states, with more on the way.


text:
Great White Way suffers post-holiday slump
The post-holiday slide snowballed into an avalanche last week, with total Broadway grosses dropping around $2.5 million to $14.8 million.
Except for the strong-selling "Coast of Utopia" ($299,449 for four perfs) and Manhattan Theater Club's previewing "Translations" ($182,632), every single on of the 27 offerings on the boards saw a dip in sales. And some of those dips were worryingly large.
"The Color Purple," for instance, plummeted nearly $250,000 to $481,854, drawing just 51% of capacity. Two other tuners from last season, "The Drowsy Chaperone" ($669,889) and "Tarzan" ($472,524), also saw sizable drops in receipts.
Long-runners felt the chill, too, as they usually do when tourists trickle away from the city. "The Lion King" ($864,047), "Beauty and the Beast" ($468,724), "Hairspray" ($425,894) and "Rent" ($297,156) were among the perennials to fall off at the box office.
Meanwhile, "Mary Poppins" ($1,043,950) is maintaining its holiday momentum, hanging on to the third-place slot behind "Wicked" ($1,365,614) and "Jersey Boys" ($1,172,292).
Also staying strong is "Spring Awakening" ($469,786), which saw only a slight dip of about $10,000. Fellow arthouse tuner "Grey Gardens" ($427,032) fell by around $40,000.
Among the plays, things looked good for "Utopia," but "The Vertical Hour" ($382,042) played to 64% capacity and "The Little Dog Laughed" ($193,849), which shutters next month, was down to 47%.
Overall, though, Broadway came out a little ahead of the same frame last year, when sales dipped to approximately $14.2 million.


text:
on November 6, 2013 - 7:12 PM
Karen Jean (Klein) Bacziewicz, 51, died Nov. 3.
Alfred P. Barletta, 85, formerly of Springville, died Nov. 3.
Elizabeth "Betty" (Matyas) Brennan, retired school bus driver, died Oct. 31.
Joseph E. Connor, died Oct. 31.
Thomas Felger, died Nov. 4.
Melrose I. (Myers) Fishman, died Nov. 2.
Scott Edward Gribben, died Nov. 4.
Elder Water Gayles Sr., pastor of Pentecostal Church of God for 37 years, died Nov. 1.
Howard F. Kester, of the Town of Tonawanda, WWII veteran, machinist for 40 years for Buxton Machine & Tool Co., died Nov. 4.
Michael H. Kondol, died Nov. 5.
Dorothy (Kreiter) Krytus, died Nov. 4.
Sarah J. (Marchese) Koester, of Alden, died Nov. 5.
Mary B. (Giambrone) LoTempio, of Elma, died Nov. 3.
Anthony Manzella, 94, died Nov. 3.
Petrolia (Huff) Mason, of Lackawanna and Rockaway Beach, died Nov. 4.
Claude R. "Bob" McCubbin, of Sheldon, died Nov. 5.
Richard D. Moore Sr., of Cheektowaga, died Nov. 2.
Gail M. (Crowl) O'Brien, died Oct. 11.
Mary (Alaimo) Palamara, died Nov. 2.
Robert E. Petschke, of Hamburg, died Nov. 3.
Debra Remson, died Nov. 3.
Louise A. Smith, died Oct. 30.
Pamela L. (Krzywicki) Smith, died Nov. 4.
Dorothy A. (Zangl) Stotz, of Orchard Park, died Nov. 5.
Richard J. Sullivan, 54, of Cheektowaga, died Nov. 4.
Sylvia (Wain) Szabad, of Grand Island, died Nov. 4.
Frank J. Voll Jr., of Akron, Army veteran of Vietnam War, died Nov. 2.
John Charles Welkner, 84, retired electrical engineer, died Nov. 5.


text:
Cheer on the top 25 sports movies ever
Posted: 2:17 AM EDT Aug 17, 2011 Updated: 10:44 AM EDT Jun 03, 2016
Take a look at our picks for the top 25 sports movies of all time.
The views expressed are not those of this company or its affiliated companies. Please note by clicking on "Post" you acknowledge that you have read and agree to the TERMS OF USE and the comment you are posting is in compliance with such terms. Your comments may be used on air. Please be polite. Inappropriate posts and those containing links to other sites may be removed by the moderator. Desktop and mobile versions of this site use independent comment threads.


text:
Coast to Coast Tickets is the place for great deals on concert, sports and theater tickets!Follow @CTCTickets
|Sorry, no Relentless Garage Event tickets are available at this time.
|London, ENG
|20-22 Highbury Corner
London, ENG N5 1BU (mapquest in new window)
Please Note: Relentless Garage tickets may be sold for more than the price listed on the ticket. Unless specifically stated, we are not affiliated with any official Relentless Garage website, any Relentless Garage box office or any Relentless Garage fan clubs, partners, or sponsors.
Coast to Coast Tickets is the place for great deals on concert, sports and theater tickets!Follow @CTCTickets
If you would like to attend an event at Relentless Garage, Coast To Coast Tickets can get you in the door and into great seats. Whether the entertainment du jour is a live music concert, theater performance, or sporting event, we offer a variety of seating options and excellent customer service. Order online or contact us toll-free to order your tickets for Relentless Garage today.
|Atlanta Austin Baltimore Boston Charlotte Chicago Cincinnati Cleveland Columbus Dallas Denver Detroit Houston Indianapolis
|Kansas City Las Vegas Los Angeles Louisville Memphis Miami Minneapolis Nashville New Jersey New Orleans New York Oakland Orlando Philadelphia
|Phoenix Pittsburgh Portland Raleigh Sacramento San Antonio San Diego San Francisco Seattle St. Louis Tampa Washington D.C.
Sign up for email updates


text:
Create Account
our secrets
shop by solution
Argan & Hamaam
Africa's Essential Oils
face care
bath rituals
body treatments
hair herbals
hand + foot
organic mama + baby
Kalahari Oontanga Oil
Item ID:
Your Price:
100% Pure, Natural & Virgin
This is a
oil from the Kalahari Desert. The women grow these melons and sell the seeds, a vital form of income for them. You get a
oil which actually
the skin. It is light enough to wear under make-up, but strong enough to make skin smooth and glowing. For those with oily skin Oontanga oil is actually known to balance the skin so that skin doesn't produce a surplus of oil. too. Scroll down to read more.
Size: 2 oz.
Kalahari Oontanga Oil
100% Pure, Natural & Virgin
This is a
oil from the Kalahari Desert. The women grow these melons and sell the seeds, a vital form of income for them. You get a
oil which actually
the skin. It is light enough to wear under make-up, but strong enough to make skin smooth and glowing. For those with oily skin Oontanga oil is actually known to balance the skin so that skin doesn't produce a surplus of oil. too. Scroll down to read more.
Size: 2 oz.
Write a Review
Argan Oil & Acacia Honey Facial Wash (Api-Therapy)
With a multitude of uses, Kalahari Ootanga Oil (locally referred to as tsamma) is a must have in every beauty cabinet. Basking under the intense sun of the Kalahari Desert, seeds of water-laden, indigenous watermelons, tsamma melons, intensify in their hydroxyl radical-scavenging anti-oxidant powers. The results is a powerful oil, nongreasy and nonclogging, that penetrates skin's surface to eradicate toxins and debris while offering gentle, yet effective moisturization.
The only source of income for many, these amazing little seeds are grown and harvested by women indigenous to the harsh, barren desert. Women living in straw huts dance with praises each time their seeds are collected, and they receive their only income. The seeds are then driven miles away where they are cold pressed at an oil mill in another part of Namibia before being air shipped to Shea Terra Organics.
Contains only: 100% pure oontanga oil
Your skin changes daily. Pollutants that it comes across, sun exposure level, your vitamin and mineral intake, the quality and amount of your water, and so on all affect and change your skin. Likewise, the skin oils that you use should change from time to time. What works for you one week might not work for you the next week. Plus, your skin benefits from the different nutrients that comes with changing up your oils. If one week your face feels a little oily, use a lighter oil and vice versa.
Daily usage
: Massage few drops into each of the five facial points. Lightly massage under eye.
Make-up removal
: Rub oil into make-up and use organic facial tissue to remove.
100% natural
skin drying and damaging alcohol free
all natural make-up removal
can be used on oily skin
Send us your questions, and you might see them posted here.
Customer Reviews
Average Rating
Light Oil - Great for Summer
My skin suffered after trying a cleanser (not from Shea Terra Organics) that caused me to break out. I purchased the Oontanga Oil to help bring my skin back into balance. The oil, along with a Shea Terra cleanser, has calmed my skin, and I love the nourishing, light feel of the oil. It doesn't have much of a scent at all, and absorbs into the skin quickly. Even if you're not having problems with your skin, this is a nice oil for summer or for those who live in hot climates year-round.
Reviewed by:
Valerie Nance
from PA.
on 5/25/2016
Easily Absorbs into Skin
I wish I would have discovered this oil earlier when the Summer was here, but I am glad I discovered it now. Now that I am getting older, I know I need extra help in keeping my skin healthy, but oils on my oily skin was always a problem until now. This oil easily absorbs in your skin and I like how light it feels. It really does help with the oil production. A little drop goes a long way.
Reviewed by:
Shelly Eure
from Jamaica, NY.
on 1/15/2016
Super good stuff
I used this after I wash my face with black soap as a moisterizer. I have oily acne prone skin and this stuff is wonderful. It sinks right in and makes my skin soft and has actually helped keep my skin from getting more oily as the day goes along. I have since purchased the black seed and calendula cream as my moisterizer since I was running low on this, I now use the last little bit to mix into my foundation to give my skin a dewy look and to keep it moisturized and to help keep my skin from turning into an oil slick.
Reviewed by:
sierra hedrick
from Oklahoma.
on 11/4/2015
Great as a cleanser
I have been using this for months as a cleanser and it is fantastic. Cleanses very well and is super moisturizing. Cut my routine down greatly by using this product for several purposes. Makes my skin look hydrated and less breakouts overall. Just ordered my second bottle.can't live with out it!
Reviewed by:
Lauren LaDeau
from New York.
on 9/8/2015
Lovely for oily/acne-prone skin!
I "dipped my toe" in the world of using oils on oily/acne-prone skin without much knowledge of what KIND of oil would most benefit my skin type. For my oily skin, this Kalahari Ooganga Oil (prehistoric watermelon seed oil) is wonderful! Because oily/acne-prone skin lacks omega 6 EFA's this oil, very high in Linoleic acid (68%) is outstanding! Quality of the product, promptness of the order system...5 stars!! LOVE this oil!!
Reviewed by:
Amy Odom
from Illinois.
on 1/28/2015
Really good for oily skin
I have oily skin and I love the Tamanu E cream. When sheaterra first sold this oil last year, I decided to give it a try. Unlike Tamanu cream, I didn't see my facial skin get any better the next day. I gave up on it after 3 days until the winter came. Argan oil was too heavy for my skin, so I decided to try this oil again for a week long. The result was wonderful. The oil absorbs very well in and I can use it during day time. After a week, I no longer have tiny acne around my nose and on my chin. It has removed sebum and I don't have a shiny face during day time. I have been using it daily since. I definitely recommend this product and suggest you give it enough time for it to work its magic. Will repurchase.
Reviewed by:
Trang Phan
from Maryland.
on 1/18/2015
I love the way this smells and feels. I generally use the organic Argan Oil and this is similar. Absorbs really quickly. It may become my new favorite!
Reviewed by:
Martha Roth
from New York City.
on 7/11/2014


text: A potter's wheel is a stone disk90 cm in diameter with a mass of 120kg. If the potter's foot pushes at the outer edge of the initiallystationary wheel with a 76 N force forone-eighth of a revolution, what will be the final speed? Use thework-energy theorem. answer = ______ rad/s


text:
Essential sounds for the season
Everyone from Cee Lo Green to Lady Antebellum to SpongeBob SquarePants has released songs for the holiday season this year, and so has local soul singer E'ssential, who put her own R&B spin on Christmas standards with her new EP "E'ssential Soul Christmas."
"I wanted a pure album as far as what Christmas is to me," said E'ssential, 30, a.k.a. Elaine Joplin. "Christmas is not about Santa Claus. For me, Jesus is the reason for the season. So I wanted to celebrate the actual reason for Christmas and do it with soul." »Read Full Article
Singing, acting both stellar in 'Figaro'
Actors are taught to act and opera singers are taught to sing - and all too rarely do the twain really meet.
The Florentine Opera Company's production of Mozart's "The Marriage of Figaro," directed by Candace Evans, cast that notion aside Friday evening with a spot-on blend of absolutely sterling singing and audience-connected acting. »Read Full Article
Theatre Gigante taps dark, creative energy in 'Electra'
While her father is out of town on business, her mother takes a lover. When her father comes home, Mom and her new consort stab him. She herself is thrown out of the house. Her baby brother now lives in exile.
No wonder Electra has a complex. The question is whether her righteous anger regarding the murder of her father (Agamemnon) can justify plotting with her brother (Orestes) to murder Mom (Clytemnestra) and Mom's new squeeze (Aegisthus). »Read Full Article
UWM work exhibited at Cannes film fest
Fourteen films by students, faculty and alumni of the University of Wisconsin-Milwaukee Department of Film, Video, Animation and New Genres have been accepted into the short-film showcase at this year's Cannes International Film Festival, which kicks off Wednesday on the French Riviera.
The total is more than double the number of short films that made it into the Cannes Court Métrage Short Film Corner last year. »Read Full Article


text:
Simple Wordpress Website Designer (responsive)
This project received 22 bids from talented freelancers with an average bid price of $147 USD.Get free quotes for a project like this
Project Budget$30 - $50 USD
Total Bids22
Project Description
I am looking for a Wordpress Designer having a skilled and Quality Wordpress ,Php,
Responsive work in all device
Theme is loaded and looking for long term Relation..
No Milestone
Preference : Low Bidder
Looking to make some money?
- Set your budget and the timeframe
- Outline your proposal
- Get paid for your work
Hire Freelancers who also bid on this project
Looking for work?
Work on projects like this and make money from home!Sign Up Now
- Forbes
- The New York Times
- Time
- Wall Street Journal
- Times Online


text:
morine charles has not received any gifts yet
Give a Gift
Join The 7th Generation Project
Welcome toThe 7th Generation Project
Sign Upor Sign In
Posted by Andrew McMurray on August 20, 2012 at 8:30
Posted by Aoife Raleigh on July 22, 2011 at 1:32
Posted by Ada Ketchie on February 17, 2011 at 5:33
Posted by Rachel Craig on February 8, 2011 at 12:30 — 1 Comment
Posted by Rachel Craig on January 16, 2011 at 5:32
Sen. Warren Calls for Wells Fargo CEO to Resign & Face Investigation Amid Growing Scandal
Protests over Tulsa & Charlotte Police Killings Stem from Economic Policies That Perpetuate Racism
Moral Mondays Leader Rev. Barber: Release Video of Keith Scott Shooting, It Belongs to the Public
Get Badge
© 2016 Created by Zand Craig.
Powered by
Badges |
Report an Issue |
Terms of Service
Please check your browser settings or contact your system administrator.


text:
$11.19Draw out the best in your children—by understanding the way they learn. If you're frustrated that your child isn't learning the way you did, chances are they are too! In this practical resource, Cynthia Ulrich Tobias explains that understanding how you both learn can make all the difference.Using expertise in education and learning styles, Tobias offers practical guidance for teaching to your
How to Help Your Child Love LearningIncludes tips for home schoolers. What do you do when your child hates school? When little Sarah cries herself to sleep at night, when Johnny has tummy aches in the morning, something is clearly wrong. An occasional problem at school is one thing. But what do you do when school is the problem? When your child hates school because school doesn't like your child, you've got to act. Don't let a one
Bringing Out the Best in Your Child
80 Ways to Focus on Every Kid's StrengthsSometimes the traits and behaviors that seem most frustrating and annoying in our children are indicators of positive strengths and future success. Stubbornness can be steadfastness. A strong will may exhibit leadership material. Arguing may indicate negotiating skills. When we identify the behavior in each child and see beyond it to the positive strength it contains, we will then be able to help
Middle School: The Inside Story
What Kids Tell Us, But Don't Tell YouRemember middle school? Many parents would rather not. It's often a rough ride, filled with insecurity, peer pressure, awkwardness, and world-rocking change. This book provides practical, hands-on advice for helping your child through this minefield—with information about what he or she is really going through, but isn't likely to share.Best-selling learning-styles expert Cynthia Tobias and
Let Go of Who You Think You're Supposed to Be and Embrace Who You Are"This important book is about the lifelong journey from ?What will people think?' to ?I am enough.' Brown's unique ability to blend original research with honest storytelling makes reading The Gifts of Imperfection like having a long, uplifting conversation with a very wise friend who offers compassion, wisdom, and great advice." --Harriet Lerner, New York Times best-selling author of The Dance of
Discover and Use the Remarkable Connection Between Personality and Habits to Bec ome an Outstanding ManagerIn his internationally acclaimed book, Smart Thinking, which examines the gap between innate intelligence and acquired mental skills, Art Markman presented a three-part formula to show readers how to develop "smart habits", how to acquire high quality knowledge, and how to use that knowledge when it's needed. Now, Markman takes his scientifically-based formula one step further to demonstrate the
$12.99Read Heidi Grant Halvorson's blogs and other content on the Penguin Community. Just in time for New Year's resolutions, learn how to reach your goals-finally-by overcoming the many hurdles that have defeated you before. Most of us have no idea why we fail to reach our goals. Now Dr. Heidi Grant Halvorson, a rising star in the field of social psychology shows us how to overcome the hurdles that
Adopting a Child With a Trauma and Attachment Disruption History"If you have the love in your heart and the courage to adopt a child from a traumatized background, then you must have this book." -- Robert Rich, PhD, anxietyanddepression-help.com This booklet is a fact-filled resource for adoptive parents who have a child with trauma and attachment disruption experiences. Fraser provides tips and strategies that can be considered before placement as well as
Solving the Procrastination Puzzle
A Concise Guide to Strategies for ChangeThe new edition of the self-published hit, offering powerful strategies to end procrastination!Why do we sabotage our own best intentions? How can we eliminate procrastination from our lives for good? Based on current psychological research and supplemented with clear strategies for change, this concise guide will help readers finally break free from self-destructive ideas and habits, and move
Change Your Thoughts, Change Your Life With NLPInterested in NLP? …Are you stuck in a rut...the same fears...the same stress...and the same job?Do you want to excel at life...but don't know how to break your old cycles of behavior? If so, then you've found the right book!Most people don't realize how much we talk to ourselves...And the effect this "self-talk" has on our lives. Humans have a near constant stream of thoughts going through their


text:
Most Cited Planetary and Space Science Articles
The most cited articles published since 2011, extracted from Scopus.
Map-projection-independent crater size-frequency determination in GIS environments - New software tool for ArcGIST. Kneissl | S. Van Gasselt | G. Neukum
Volume 59, Issues 11-12, September 2011, Pages 1243-1254
Statistical analysis of crater size-frequency distributions (CSFDs) of impact craters on planetary surfaces is a well-established method to derive absolute ages on the basis of remotely-sensed image data. Although modelling approaches and the derivation of absolute ages from a given CSFD have been described and discussed in considerable depth since the late 1960s, there is no standardised methodology or guideline for the measurement of impact-crater diameters and area sizes that are both needed to determine absolute ages correctly. Distortions of distances (i.e., diameters) and areas within different map projections are considerable error sources during crater and area measurements. In order to address this problem and to minimize such errors, a software extension for Environmental Systems Research Institute's (ESRI's) ArcMap (ArcGIS) has been developed measuring CSFDs on planetary surfaces independently of image and data frame map projections, which can also be theoretically transferred to every Geographic Information System (GIS) capable of working with different map projections. Using this new approach each digitized impact crater is internally projected to a stereographic map projection with the crater's central-point set as the projection center. In this projection, the circle is defined without any distortion of its shape (i.e., conformality). Using a sinusoidal map projection with a center longitude set to the crater's central-point, the diameter of the impact crater is measured along this central meridian which is true-scale and does not show any distortion. The crater is re-projected to the map projection of the current data frame and stored as vector geometry with attributes. Output from this workflow comprises correct impact-crater diameters and area sizes in sinusoidal map projections and can be used for further processing, i.e. absolute age determinations (e.g., using the software CraterStats). The ArcMap toolbar CraterTools developed in this context significantly helps to improve and simplify the crater size-frequency (CSF) measurement process. For GIS-based measurements, we strongly recommend our procedure as the standard method for determining CSFDs on planetary surfaces to minimize map distortion effects for further analysis. © 2010 Elsevier Ltd. All rights reserved.
Density of asteroidsB. Carry
Volume 73, Issue 1, December 2012, Pages 98-118
The small bodies of our solar system are the remnants of the early stages of planetary formation. A considerable amount of information regarding the processes that occurred during the accretion of the early planetesimals is still present among this population. A review of our current knowledge of the density of small bodies is presented here. Density is indeed a fundamental property for the understanding of their composition and internal structure. Intrinsic physical properties of small bodies are sought by searching for relationships between the dynamical and taxonomic classes, size, and density. Mass and volume estimates for 287 small bodies (asteroids, comets, and transneptunian objects) are collected from the literature. The accuracy and biases affecting the methods used to estimate these quantities are discussed and best-estimates are strictly selected. Bulk densities are subsequently computed and compared with meteorite density, allowing to estimate the macroporosity (i.e., amount of voids) within these bodies. Dwarf-planets apparently have no macroporosity, while smaller bodies (<400km) can have large voids. This trend is apparently correlated with size: C- and S-complex asteroids tend to have larger density with increasing diameter. The average density of each Bus-DeMeo taxonomic classes is computed (DeMeo et al., 2009; Icarus 202). S-complex asteroids are more dense on average than those in the C-complex that in turn have a larger macroporosity, although both complexes partly overlap. Within the C-complex asteroids, B-types stand out in albedo, reflectance spectra, and density, indicating a unique composition and structure. Asteroids in the X-complex span a wide range of densities, suggesting that many compositions are included in the complex. Comets and TNOs have high macroporosity and low density, supporting the current models of internal structures made of icy aggregates. Although the number of density estimates sky-rocketed during last decade from a handful to 287, only a third of the estimates are more precise than 20%. Several lines of investigation to refine this statistic are contemplated, including observations of multiple systems, 3-D shape modeling, and orbital analysis from Gaia astrometry. © 2012 Elsevier Ltd. All rights reserved.
JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter systemO. Grasset | M. K. Dougherty | A. Coustenis | E. J. Bunce | C. Erd | D. Titov | M. Blanc | A. Coates | P. Drossart | L. N. Fletcher | H. Hussmann | R. Jaumann | N. Krupp | J. P. Lebreton | O. Prieto-Ballesteros | P. Tortora | F. Tosi | T. Van Hoolst
Volume 78, Issue , April 2013, Pages 1-21
Past exploration of Jupiter's diverse satellite system has forever changed our understanding of the unique environments to be found around gas giants, both in our solar system and beyond. The detailed investigation of three of Jupiter's Galilean satellites (Ganymede, Europa, and Callisto), which are believed to harbour subsurface water oceans, is central to elucidating the conditions for habitability of icy worlds in planetary systems in general. The study of the Jupiter system and the possible existence of habitable environments offer the best opportunity for understanding the origins and formation of the gas giants and their satellite systems. The JUpiter ICy moons Explorer (JUICE) mission, selected by ESA in May 2012 to be the first large mission within the Cosmic Vision Program 2015-2025, will perform detailed investigations of Jupiter and its system in all their inter-relations and complexity with particular emphasis on Ganymede as a planetary body and potential habitat. The investigations of the neighbouring moons, Europa and Callisto, will complete a comparative picture of the Galilean moons and their potential habitability. Here we describe the scientific motivation for this exciting new European-led exploration of the Jupiter system in the context of our current knowledge and future aspirations for exploration, and the paradigm it will bring in the study of giant (exo) planets in general. © 2012 Elsevier Ltd.
Optical measurements of the Moon as a tool to study its surfaceY. Shkuratov | V. Kaydash | V. Korokhin | Y. Velikodsky | N. Opanasenko | G. Videen
Volume 59, Issue 13, October 2011, Pages 1326-1371
This survey is a general overview of modern optical studies of the Moon and their diagnostic meaning. It includes three united parts: phase photometry, spectrophotometry, and polarimetry. The first one is devoted to the progress in the photometry of the Moon, which includes absolute albedo determination to refine the albedo scale (e.g.; to connect lunar observations and the data of lunar sample measurements) and mapping the parameters of a lunar photometric function (e.g.; the phase-angle ratios method) with the aim of making qualitative estimates of regolith structure variations. This part also includes observations of the lunar opposition effect as well as photogrammetry and photoclinometry techniques. In particular, available data show that because of the low albedo of the lunar surface, the coherent backscattering enhancement hardly influences the lunar opposition spike, with the exception of the brightest lunar areas measured in the NIR. The second part is devoted to chemical/mineral mapping of the Moons surface using spectrophotometric measurements. This section also includes analyses related to the detection of water ice or hydroxyl, prognoses of maturity, and helium-3 abundance mapping. In particular, we examine the relationship between superficial OH/H2O compounds spectrally detected recently and bulk water ice found earlier by the Lunar Prospector GRS and LRO LEND, assuming that the compounds are delivered to cold traps (permanently shadowed regions) with electrostatically levitated dust saturated by solar wind hydrogen. Significant problems arise with the determination of TiO2 content, as the correlation between this parameter and the color ratio C(750/415 nm) is very non-linear and not universal for different composition types of the lunar surface; a promising way to resolve this problem is to use color ratios in the UV spectral range. The third part is devoted to mapping of polarization parameters of the lunar surface, which enable estimates of the average size of regolith particles and their optical inhomogeneity. This includes considerations of the Umov effect and results of spectropolarimetry, negative polarization imagery, and measurements of other polarimetric parameters, including the third Stokes parameter. Although these three research divisions have not been developed equally and the numbers of proper references are very different, we try to keep a balance between them, depicting a uniform picture. It should be emphasized that many results presented in this review can be applied to other atmosphereless celestial bodies as well. © 2011 Elsevier Ltd. All rights reserved.
New views of the lunar plasma environmentJ. S. Halekas | Y. Saito | G. T. Delory | W. M. Farrell
Volume 59, Issue 14, November 2011, Pages 1681-1694
A rich set of new measurements has greatly expanded our understanding of the Moonplasma interaction over the last sixteen years, and helped demonstrate the fundamentally kinetic nature of many aspects thereof. Photon and charged particle impacts act to charge the lunar surface, forming thin Debye-scale plasma sheaths above both sunlit and shadowed hemispheres. These impacts also produce photoelectrons and secondary electrons from the surface, as well as ions from the surface and exosphere, all of which in turn feed back into the plasma environment. The solar wind interacts with sub-ion-inertial-scale crustal magnetic fields to form what may be the smallest magnetospheres in the solar system. Proton gyro-motion, solar wind pickup of protons scattered from the dayside surface, and plasma expansion into vacuum each affect the dynamics and structure of different portions of the lunar plasma wake. The Moon provides us with a basic plasma physics laboratory for the study of fundamental processes, some of which we cannot easily observe elsewhere. At the same time, the Moon provides us with a test bed for the study of processes that also operate at many other solar system bodies. We have learned much about the Moonplasma interaction, with implications for other space and planetary environments. However, many fundamental problems remain unsolved, including the details of the coupling between various parts of the plasma environment, as well as between plasma and the surface, neutral exosphere, and dust. In this paper, we describe our current understanding of the lunar plasma environment, including illustrative new results from Lunar Prospector and Kaguya, and outstanding unsolved problems. © 2010 Elsevier Ltd.
Dipolarization fronts in the magnetotail plasma sheetA. Runov | V. Angelopoulos | M. Sitnov | V. A. Sergeev | R. Nakamura | Y. Nishimura | H. U. Frey | J. P. McFadden | D. Larson | J. Bonnell | K. H. Glassmeier | U. Auster | M. Connors | C. T. Russell | H. J. Singer
Volume 59, Issue 7, May 2011, Pages 517-525
We present a THEMIS study of a dipolarization front associated with a bursty bulk flow (BBF) that was observed in the central plasma sheet sequentially at X=-20.1, -16.7, and -11.0RE. Simultaneously, the THEMIS ground network observed the formation of a northsouth auroral form and intensification of westward auroral zone currents. Timing of the signatures in space suggests earthward propagation of the front at a velocity of 300 km/s. Spatial profiles of current and electron density on the front reveal a spatial scale of 500 km, comparable to an ion inertial length and an ion thermal gyroradius. This kinetic-scale structure traveled a macroscale distance of 10RE in about 4 min without loss of coherence. The dipolarization front, therefore, is an example of space plasma cross-scale coupling. THEMIS observations at different geocentric distances are similar to recent particle-in-cell simulations demonstrating the appearance of dipolarization fronts on the leading edge of plasma fast flows in the vicinity of a reconnection site. Dipolarization fronts, therefore, may be interpreted as remote signatures of transient reconnection. © 2010 Elsevier Ltd. All rights reserved.
Applications of a new set of methane line parameters to the modeling of Titan's spectrum in the 1.58 μm windowCatherine De Bergh | Régis Courtin | Bruno Bézard | Athéna Coustenis | Emmanuel Lellouch | Mathieu Hirtzig | Pascal Rannou | Pierre Drossart | Alain Campargue | Samir Kassi | Le Wang | Vincent Boudon | Andrei Nikitin | Vladimir Tyuterev
Volume 61, Issue 1, February 2012, Pages 85-98
In this paper we apply a recently released set of methane line parameters (Wang et al.; 2011) to the modeling of Titan spectra in the 1.58 μm window at both low and high spectral resolution. We first compare the methane absorption based on this new set of methane data to that calculated from the methane absorption coefficients derived in situ from DISR/Huygens (Tomasko et al.; 2008a; Karkoschka and Tomasko, 2010) and from the band models of Irwin et al. (2006) and Karkoschka and Tomasko (2010). The Irwin et al. (2006) band model clearly underestimates the absorption in the window at temperaturepressure conditions representative of Titan's troposphere, while the Karkoschka and Tomasko (2010) band model gives an acceptable agreement in the whole window, overestimating the absorption by about 15% in the range 63006500 cm -1. We also find that the transmittance of Titan's atmosphere is in excellent agreement with that calculated from the Tomasko et al. (2008a) coefficients after reducing them by about 7%. Synthetic spectra computed with spectral resolutions of 1.2 cm -1 (R∼5400) and 0.35 cm -1 (R∼18000) are then compared with two high-resolution Earth-based measurements of Titan's albedo obtained in 1982 and 1993 (with KPNO/FTS and IRTF/CSHELL). The new set of methane line parameters leads to an excellent match of all the CH 3D and CH 4 absorption features in these spectra, and permits us to derive a ratio of CH 3D/CH 4=(4.5±1.0)×10 -4 hence a D/H ratio in methane for Titan of (1.13±0.25)×10 -4 and a CO mole fraction of 40±10 ppm (from the KPNO/FTS dataset) and 51±7 ppm (from the IRTF/CSHELL dataset). We also infer constraints on the far-wing lineshape of methane lines of the 2ν 3 band. We finally present two other examples of models of Titan's spectrum using the new line parameters, one potentially useful for future higher-resolution (R=40,000) observations, another one applicable to the ongoing low-resolution (R∼100) observations by Cassini VIMS. We show that the aerosol model of Tomasko et al. (2008b) produces too much intensity at low phase angle compared to a VIMS spectrum recorded near the Huygens site and we propose a slightly revised model that reproduces this observation. © 2011 Elsevier Ltd. All rights reserved.
High resolution Vesta High Altitude Mapping Orbit (HAMO) Atlas derived from Dawn framing camera imagesTh Roatsch | E. Kersten | K. D. Matz | F. Preusker | F. Scholten | R. Jaumann | C. A. Raymond | C. T. Russell
Volume 73, Issue 1, December 2012, Pages 283-286
The Dawn framing camera (FC) acquired about 2500 clear filter images of Vesta with a resolution of about 70 m/pixels during the High Altitude Mapping Orbit (HAMO) in fall 2011. We ortho-rectified these images and produced a global high resolution controlled mosaic of Vesta. This global mosaic is the baseline for a high resolution Vesta atlas that consists of 15 tiles mapped at a scale of 1:500,000. The nomenclature used in this atlas was proposed by the Dawn team and was approved by the International Astronomical Union (IAU). The whole atlas is available to the public through the Dawn GIS web page [http://dawn-gis.dlr. de/atlas]. © 2012 Elsevier Ltd. All rights reserved.
The lunar dust environmentEberhard Grün | Mihaly Horanyi | Zoltan Sternovsky
Volume 59, Issue 14, November 2011, Pages 1672-1680
Each year the Moon is bombarded by about 106 kg of interplanetary micrometeoroids of cometary and asteroidal origin. Most of these projectiles range from 10 nm to about 1 mm in size and impact the Moon at 1072 km/s speed. They excavate lunar soil about 1000 times their own mass. These impacts leave a crater record on the surface from which the micrometeoroid size distribution has been deciphered. Much of the excavated mass returns to the lunar surface and blankets the lunar crust with a highly pulverized and impact gardened regolith of about 10 m thickness. Micron and sub-micron sized secondary particles that are ejected at speeds up to the escape speed of 2300 m/s form a perpetual dust cloud around the Moon and, upon re-impact, leave a record in the microcrater distribution. Such tenuous clouds have been observed by the Galileo spacecraft around all lunar-sized Galilean satellites at Jupiter. The highly sensitive Lunar Dust Experiment (LDEX) onboard the LADEE mission will shed new light on the lunar dust environment. LADEE is expected to be launched in early 2013. Another dust related phenomenon is the possible electrostatic mobilization of lunar dust. Images taken by the television cameras on Surveyors 5, 6, and 7 showed a distinct glow just above the lunar horizon referred to as horizon glow (HG). This light was interpreted to be forward-scattered sunlight from a cloud of dust particles above the surface near the terminator. A photometer onboard the Lunokhod-2 rover also reported excess brightness, most likely due to HG. From the lunar orbit during sunrise the Apollo astronauts reported bright streamers high above the lunar surface, which were interpreted as dust phenomena. The Lunar Ejecta and Meteorites (LEAM) Experiment was deployed on the lunar surface by the Apollo 17 astronauts in order to characterize the lunar dust environment. Instead of the expected low impact rate from interplanetary and interstellar dust, LEAM registered hundreds of signals associated with the passage of the terminator, which swamped any signature of primary impactors of interplanetary origin. It was suggested that the LEAM events are consistent with the sunrise/sunset-triggered levitation and transport of charged lunar dust particles. Currently no theoretical model explains the formation of a dust cloud above the lunar surface but recent laboratory experiments indicate that the interaction of dust on the lunar surface with solar UV and plasma is more complex than previously thought. © 2011 Elsevier Ltd.
Titan's internal structure and the evolutionary consequencesA. D. Fortes
Volume 60, Issue 1, January 2012, Pages 10-17
Titan's moment of inertia (MoI), estimated from the quadrupole gravity field measured by the Cassini spacecraft, is 0.342, which has been interpreted as evidence of a partially differentiated internal mass distribution. It is shown here that the observed MoI is equally consistent with a fully differentiated internal structure comprising a shell of water ice overlying a low-density silicate core; depending on the chemistry of Titan's subsurface ocean, the core radius is between 1980 and 2120 km, and its uncompressed density is 25702460 kg m -3, suggestive of a hydrated CI carbonaceous chondrite mineralogy. Both the partially differentiated and fully differentiated hydrated core models constrain the deep interior to be several hundred degrees cooler than previously thought. I propose that Titan has a warm wet core below, or buffered at, the high-pressure dehydration temperature of its hydrous constituents, and that many of the gases evolved by thermochemical and radiogenic processes in the core (such as CH 4 and 40Ar, respectively) diffuse into the icy mantle to form clathrate hydrates, which in turn may provide a comparatively impermeable barrier to further diffusion. Hence we should not necessarily expect to see a strong isotopic signature of serpentinization in Titan's atmosphere. © 2011 Elsevier Ltd. All rights reserved.
Characteristics of the dustplasma interaction near Enceladus' South PoleMuhammad Shafiq | J. E. Wahlund | M. W. Morooka | W. S. Kurth | W. M. Farrell
Volume 59, Issue 1, January 2011, Pages 17-25
We present RPWS Langmuir probe data from the third Enceladus flyby (E3) showing the presence of dusty plasma near Enceladus' South Pole. There is a sharp rise in both the electron and ion number densities when the spacecraft traverses through Enceladus plume. The ion density near Enceladus is found to increase abruptly from about 102 cm-3 before the closest approach to 105 cm-3 just 30 s after the closest approach, an amount two orders of magnitude higher than the electron density. Assuming that the inconsistency between the electron and ion number densities is due to the presence of dust particles that are collecting the missing electron charges, we present dusty plasma characteristics down to sub-micron particle sizes. By assuming a differential dust number density for a range in dust sizes and by making use of Langmuir probe data, the dust densities for certain lower limits in dust size distribution were estimated. In order to achieve the dust densities of micrometer and larger sized grains comparable to the ones reported in the literature, we show that the power law size distribution must hold down to at least 0.03 μm such that the total differential number density is dominated by the smallest sub-micron sized grains. The total dust number density in Enceladus' plume is of the order of 102 cm-3 reducing to 1 cm-3 in the E-ring. The dust density for micrometer and larger sized grains is estimated to be about 10-4 cm-3 in the plume while it is about 10-610-7 cm-3 in the E-ring. Dust charge for micron sized grains is estimated to be about eight thousand electron charges reducing to below one hundred electron charges for 0.03 μm sized grains. The effective dusty plasma Debye length is estimated and compared with inter-grain distance as well as the electron Debye length. The maximum dust charging time of 1.4 h is found for 0.03 μm sized grains just 1 min before the closest approach. The charging time decreases substantially in the plume where it is only a fraction of a second for 1 μm sized grains, 1 s for 0.1 μm sized grains and about 10 s for 0.03 μm sized grains. © 2010 Elsevier Ltd. All rights reserved.
Mapping methane in Martian atmosphere with PFS-MEX dataA. Geminale | V. Formisano | G. Sindoni
Volume 59, Issues 2-3, February 2011, Pages 137-148
In this study we map the methane gas in the Martian atmosphere. The main goal of this work is to show the methane behaviour across the planet seasonally. To this aim, we analyze the strongest methane band in the short wavelength channel of the Planetary Fourier Spectrometer (PFS) on board ESA Mars Express (MeX) spacecraft. The optical line depth is used to derive the column density of methane. The maps thus obtained show the spatial variability of this non-condensable gas and how the gas is transported in the atmosphere due to the cycle of carbon dioxide. Moreover, the increase of methane over the north polar cap during local summer, which cannot be explained by global circulation, strongly suggests that there could be methane reservoir associated with the polar cap. © 2010 Elsevier Ltd.
A reanalysis of the Apollo light scattering observations, and implications for lunar exospheric dustDavid A. Glenar | Timothy J. Stubbs | James E. McCoy | Richard R. Vondrak
Volume 59, Issue 14, November 2011, Pages 1695-1707
Conspicuous excess brightness, exceeding that expected from coronal and zodiacal light (CZL), was observed above the lunar horizon in the Apollo 15 coronal photographic sequence acquired immediately after orbital sunset (surface sunrise). This excess brightness systematically faded as the Command Module moved farther into shadow, eventually becoming indistinguishable from the CZL background. These observations have previously been attributed to scattering by ultrafine dust grains (radius ∼0.1 microns) in the lunar exosphere, and used to obtain coarse estimates of dust concentration at several altitudes and an order-of-magnitude estimate of ∼10-9 g cm-2 for the column mass of dust near the terminator, collectively referred to as model 0. We have reanalyzed the Apollo 15 orbital sunset sequence by incorporating the known sightline geometries in a Mie-scattering simulation code, and then inverting the measured intensities to retrieve exospheric dust concentration as a function of altitude and distance from the terminator. Results are presented in terms of monodisperse (single grain size) dust distributions. For a grain radius of 0.10 microns, our retrieved dust concentration near the terminator (∼0.010 cm-3) is in agreement with model 0 at z=10 km, as is the dust column mass (∼36×10-10 g cm-2), but the present results indicate generally larger dust scale heights, and much lower concentrations near 1 km (<0.08 cm-3 vs. a few times 0.1 cm -3 for model 0"). The concentration of dust at high altitudes (z>50 km) is virtually unconstrained by the measurements. The dust exosphere extends into shadow a distance somewhere between 100 and 200 km from the terminator, depending on the uncertain contribution of CZL to the total brightness. These refined estimates of the distribution and concentration of exospheric dust above the lunar sunrise terminator should place new and more rigorous constraints on exospheric dust transport models, as well as provide valuable support for upcoming missions such as the Lunar Atmosphere and Dust Environment Explorer (LADEE). © 2010 Elsevier Ltd.
The geomorphology of (21) Lutetia: Results from the OSIRIS imaging system onboard ESA's Rosetta spacecraftN. Thomas | C. Barbieri | H. U. Keller | P. Lamy | H. Rickman | R. Rodrigo | H. Sierks | K. P. Wenzel | G. Cremonese | L. Jorda | M. Küppers | S. Marchi | F. Marzari | M. Massironi | F. Preusker | F. Scholten | K. Stephan | M. A. Barucci | S. Besse | M. R. El-Maarry | S. Fornasier | O. Groussin | S. F. Hviid | D. Koschny | E. Kührt | E. Martellato | R. Moissl | C. Snodgrass | C. Tubiana | J. B. Vincent
Volume 66, Issue 1, June 2012, Pages 96-124
The surface of (21) Lutetia is highly complex with significant interactions between ancient and more recent structures. This work attempts to summarize the surface geomorphology observed using the high resolution images from OSIRIS, the imaging system onboard the European Space Agency's Rosetta spacecraft. A wide range of surface morphologies are seen including heavily cratered terrain, extensive sets of lineaments, young impact craters, and a ridge, the height of which is more than 1/5th of the mean radius of the body. Very young and very old terrains (as inferred from crater densities) are seen in close proximity. The longest continuous lineament is over 80 km long. The lineaments show regional-dependent organization and structure. Several categories of lineament can be described. Lineaments radial to impact craters as seen on other asteroidal bodies are mostly absent. Although the lineaments may be of seismic origin (and possibly the result of several impact-induced events), impacts producing recent large craters place constraints on seismic phenomena. In particular, stronger attenuation of shocks than seen on other asteroidal bodies seems to be required. Inhomogeneous energy transport, possibly matching observed inhomogeneous ejecta deposition may offer explanations for some of the observed phenomena. Some impact craters show unusual forms, which are probably the result of impact into a surface with relief comparable to the resultant crater diameter and/or oblique impact. There is evidence that re-surfacing through landslides has occurred at several places on the object. © 2011 Elsevier Ltd.
The global distribution of pyroclastic deposits on Mercury: The view from MESSENGER flybys 13Laura Kerber | James W. Head | David T. Blewett | Sean C. Solomon | Lionel Wilson | Scott L. Murchie | Mark S. Robinson | Brett W. Denevi | Deborah L. Domingue
Volume 59, Issue 15, December 2011, Pages 1895-1909
We present a global survey of candidate pyroclastic deposits on Mercury, derived from images obtained during MESSENGER flybys 13 that provided near-global coverage at resolutions between 5 and 0.5 km/pixel. Thirty-five deposits were identified and characterized and are located principally on the floors of craters, along rims of craters, and along the edge of the Caloris basin. Deposits are commonly centered on rimless, often irregularly shaped pits, mostly between 5 and 45 km in diameter. The deposits identified are generally similar in morphology and absolute reflectance to lunar pyroclastic deposits. Spectrally the deposits appear brighter and redder than background Mercury terrain. On the basis of the available coverage, the candidate pyroclastic deposits appear to be essentially globally distributed. The diameters of the deposits, when mapped to lunar gravity conditions, are larger than their lunar counterparts, implying that more abundant volatiles were present during the typical eruptive process than on the Moon. These observations indicate that if these deposits resulted from hawaiian-style eruptions, the volatile contents required would be between ∼1600 and 16,000 ppm CO or an equivalent value of H2O, CO2, SO2, or H2S (for a more oxidizing interior), or N2, S2, CS2, S 2Cl, Cl, Cl2, or COS (for a more reducing interior). These abundances are much greater than those predicted by existing models for Mercurys formation. An apparent lack of small deposits, compared with the Moon, may be due to resolution effects, a topic that can be further assessed during the orbital phase of the MESSENGER mission. These results provide a framework within which orbital observations by MESSENGER and the future BepiColombo mission can be analyzed. © 2011 Elsevier Ltd. All rights reserved.
Determining the local abundance of Martian methane and its 13C/12C and D/H isotopic ratios for comparison with related gas and soil analysis on the 2011 Mars Science Laboratory (MSL) missionChristopher R. Webster | Paul R. Mahaffy
Volume 59, Issues 2-3, February 2011, Pages 271-283
Understanding the origin of Martian methane will require numerous complementary measurements from both in situ and remote sensing investigations and laboratory work to correlate planetary surface geophysics with atmospheric dynamics and chemistry. Three instruments (Quadrupole Mass Spectrometer (QMS), Gas Chromatograph (GC) and Tunable Laser Spectrometer (TLS)) with sophisticated sample handling and processing capability make up the Sample Analysis at Mars (SAM) analytical chemistry suite on NASAs 2011 Mars Science Laboratory (MSL) Mission. Leveraging off the SAM sample and gas processing capability that includes methane enrichment, TLS has unprecedented sensitivity for measuring absolute methane (parts-per-trillion), water, and carbon dioxide abundances in both the Martian atmosphere and evolved from heated soil samples. In concert with a wide variety of associated trace gases (e.g. SO2, H 2S, NH3, higher hydrocarbons, organics, etc.) and other isotope ratios measured by SAM, TLS will focus on determining the absolute abundances of methane, water and carbon dioxide, and their isotope ratios: 13C/12C and D/H in methane; 13C/12C and 18O/17O/16O in carbon dioxide; and 18O/17O/16O and D/H in water. Measurements near the MSL landing site will be correlated with satellite (Mars Express, Mars 2016) and ground-based observations. © 2010 Elsevier Ltd.
Confirmation of sublunarean voids and thin layering in mare depositsM. S. Robinson | J. W. Ashley | A. K. Boyd | R. V. Wagner | E. J. Speyerer | B. Ray Hawke | H. Hiesinger | C. H. Van Der Bogert
Volume 69, Issue 1, August 2012, Pages 18-27
Typical flow thicknesses of lunar mare basalts were not well constrained in the past, because as craters and rilles age, downslope movement of loose material tends to mix and bury stratigraphy, obscuring the three dimensional nature of the maria. New Lunar Reconnaissance Orbiter Camera high resolution images unambiguously reveal thicknesses of mare basalt layers exposed in impact craters, rilles, and steep-walled pits. Pits up to one hundred meters deep present relatively unmodified, near-vertical sections of mare in three cases, and many young impact craters also expose well preserved sections of mare. Oblique views of each pit and many of these craters reveal multiple layers, 3 to 14 m thick, indicating that eruptions typically produced a series of ∼10 m thick flows (or flow lobes) rather than flows many tens to hundreds of meters thick. Additionally, these images unambiguously show that the floors of two pits extend beneath the mare surfaces, thus revealing sublunarean voids of unknown lateral extent. We also document the occurrence of pits that may be expressions of collapse into subsurface voids in non-mare impact melt deposits. These voids are compelling targets for future human and robotic exploration, with potential as temporary shelters, habitations, or geologic museums. © 2012 Elsevier Ltd. All rights reserved.
The science process for selecting the landing site for the 2011 mars science laboratoryJohn A. Grant | Matthew P. Golombek | John P. Grotzinger | Sharon A. Wilson | Michael M. Watkins | Ashwin R. Vasavada | Jennifer L. Griffes | Timothy J. Parker
Volume 59, Issues 11-12, September 2011, Pages 1114-1127
The process of identifying the landing site for NASA's 2011 Mars Science Laboratory (MSL) began in 2005 by defining science objectives, related to evaluating the potential habitability of a location on Mars, and engineering parameters, such as elevation, latitude, winds, and rock abundance, to determine acceptable surface and atmospheric characteristics. Nearly 60 candidate sites were considered at a series of open workshops in the years leading up to the launch. During that period, iteration between evolving engineering constraints and the relative science potential of candidate sites led to consensus on four final sites. The final site will be selected in the Spring of 2011 by NASA's Associate Administrator for the Science Mission Directorate. This paper serves as a record of landing site selection activities related primarily to science, an inventory of the number and variety of sites proposed, and a summary of the science potential of the highest ranking sites. © 2010 Elsevier Ltd. All rights reserved.
MA130301GT catalogue of Martian impact craters and advanced evaluation of crater detection algorithms using diverse topography and image datasetsGoran Salamunićcar | Sven Lonarić | Pedro Pina | Loureno Bandeira | Jos Saraiva
Volume 59, Issue 1, January 2011, Pages 111-131
Recently, all the craters from the major currently available manually assembled catalogues have been merged into the catalogue with 57 633 known Martian impact craters (MA57633GT). In addition, the work on crater detection algorithm (CDA), developed to search for still uncatalogued impact craters using 1/128° MOLA data, resulted in MA115225GT. In parallel with this work another CDA has been developed which resulted in the Stepinski catalogue containing 75 919 craters (MA75919T). The new MA130301GT catalogue presented in this paper is the result of: (1) overall merger of MA115225GT and MA75919T; (2) 2042 additional craters found using ShenCastan based CDA from the previous work and 1/128° MOLA data; and (3) 3129 additional craters found using CDA for optical images from the previous work and selected regions of 1/256° MDIM, 1/256° THEMIS-DIR, and 1/256° MOC datasets. All craters from MA130301GT are manually aligned with all used datasets. For all the craters that originate from the used catalogues (Barlow, Rodionova, Boyce, Kuzmin, Stepinski) we integrated all the attributes available in these catalogues. With such an approach MA130301GT provides everything that was included in these catalogues, plus: (1) the correlation between various morphological descriptors from used catalogues; (2) the correlation between manually assigned attributes and automated depth/diameter measurements from MA75919T and our CDA; (3) surface dating which has been improved in resolution globally; (4) average errors and their standard deviations for manually and automatically assigned attributes such as position coordinates, diameter, depth/diameter ratio, etc.; and (5) positional accuracy of features in the used datasets according to the defined coordinate system referred to as MDIM 2.1, which incorporates 1232 globally distributed ground control points, while our catalogue contains 130 301 cross-references between each of the used datasets. Global completeness of MA130301GT is up to ∼D<2 km (it contains 85 783 such craters, while the smallest D is 0.924 km). This is a considerable improvement in comparison with the completeness of the Rodionova (∼10 km), Barlow (∼5 km) and Stepinski (∼3 km) catalogues. An accompanying result to the new catalogue is a contribution to the evaluation of CDAsthe following methods have been developed: (1) a new context-aware method for the advanced automated registration of craters with GT catalogues; (2) a new method for manual registration of newly found craters into GT catalogues; and (3) additional new accompanying methods for objective evaluation of CDAs using different datasets including optical images. © 2010 Elsevier Ltd. All rights reserved.
MESSENGER observations of the plasma environment near MercuryJim M. Raines | James A. Slavin | Thomas H. Zurbuchen | George Gloeckler | Brian J. Anderson | Daniel N. Baker | Haje Korth | Stamatios M. Krimigis | Ralph L. McNutt
Volume 59, Issue 15, December 2011, Pages 2004-2015
The MESSENGER Fast Imaging Plasma Spectrometer (FIPS) measured the bulk plasma characteristics of Mercurys magnetosphere and solar wind environment during the spacecrafts first two flybys of the planet on 14 January 2008 (M1) and 6 October 2008 (M2), producing the first measurements of thermal ions in Mercurys magnetosphere. In this work, we identify major features of the Mercury magnetosphere in the FIPS proton data and describe the data analysis process used for recovery of proton density (np) and temperature (T p) with a forward modeling technique, required because of limitations in measurement geometry. We focus on three regions where the magnetospheric flow speed is likely to be low and meets our criteria for the recovery process: the M1 plasma sheet and the M1 and M2 dayside and nightside boundary-layer regions. Interplanetary magnetic field (IMF) conditions were substantially different between the two flybys, with intense reconnection signatures observed by the Magnetometer during M2 versus a relatively quiet magnetosphere during M1. The recovered ion density and temperature values for the M1 quiet-time plasma sheet yielded np∼110 cm-3, Tp∼2× 106 K, and plasma β∼2. The nightside boundary-layer proton densities during M1 and M2 were similar, at np∼45 cm -3, but the temperature during M1 (Tp∼48×10 6 K) was 50% less than during M2 (Tp∼8×10 6 K), presumably due to reconnection in the tail. The dayside boundary layer observed during M1 had a density of ∼16 cm-3 and temperature of 2×106 K, whereas during M2 this region was less dense and hotter (np∼8 cm-3 and T p∼10×106 K), again, most likely due to magnetopause reconnection. Overall, the southward interplanetary magnetic field during M2 clearly produced higher Tp in the dayside and nightside magnetosphere, as well as higher plasma β in the nightside boundary, ∼20 during M2 compared with ∼2 during M1. The proton plasma pressure accounts for only a fraction (24% for M1 and 64% for M2) of the drop in magnetic pressure upon entry into the dayside boundary layer. This result suggests that heavy ions of planetary origin, not considered in this analysis, may provide the missing pressure. If these planetary ions were hot due to pickup in the magnetosheath, the required density for pressure balance would be an ion density of ∼1 cm-3 for an ion temperature of ∼108 K. © 2011 Elsevier Ltd. All rights reserved.
Titan's global crater population: A new assessmentC. D. Neish | R. D. Lorenz
Volume 60, Issue 1, January 2012, Pages 26-33
We report a revised crater population for Titan using Cassini RADAR data through January 2010 (flyby T65), and make a size-dependent correction for the incomplete coverage (∼33%) using a Monte-Carlo model. Qualitatively, Titan's landscape is more heavily cratered than Earth, but much less than Mars or Ganymede: the area fraction covered by craters is in fact comparable with that of Venus. Quantitative efforts to interpret crater densities for Titan as surface age have been confounded by widely divergent crater production rates proposed in the literature. We elucidate the specific model assumptions that lead to these differences (assumed projectile density, scaling function for simple crater diameter, and complex crater size exponent) and suggest these are reasonable bounding models, with the Korycansky and Zahnle (2005) model representing a crater retention age of ∼1 Ga, and the Artemieva and Lunine (2005) model representing a crater retention age of ∼200 Ma. These estimates are consistent with models of Titan's evolution that predict a thickening of its crust 0.31.2 Gyr ago. © 2011 Elsevier Ltd. All rights reserved.
New indication for a dichotomy in the interior structure of Uranus and Neptune from the application of modified shape and rotation dataN. Nettelmann | R. Helled | J. J. Fortney | R. Redmer
Volume 77, Issue , March 2013, Pages 143-151
Since the Voyager fly-bys of Uranus and Neptune, improved gravity field data have been derived from long-term observations of the planets' satellite motions, and modified shape and solid-body rotation periods were suggested. A faster rotation period (-40 min) for Uranus and a slower rotation period (+1h20) of Neptune compared to the Voyager data were found to minimize the dynamical heights and wind speeds. We apply the improved gravity data, the modified shape and rotation data, and the physical LM-R equation of state to compute adiabatic three-layer structure models, where rocks are confined to the core, and homogeneous thermal evolution models of Uranus and Neptune. We present the full range of structure models for both the Voyager and the modified shape and rotation data. In contrast to previous studies based solely on the Voyager data or on empirical EOS, we find that Uranus and Neptune may differ to an observationally significant level in their atmospheric heavy element mass fraction Z1 and nondimensional moment of inertia, λ. For Uranus, we find Z1≤8% and λ=0.2224(1), while for Neptune Z1≤65% and λ=0.2555(2) when applying the modified shape and rotation data, while for the unmodified data we compute Z1≤17% and λ=0.230(1) for Uranus and Z1≤54% and λ=0.2410(8) for Neptune. In each of these cases, solar metallicity models ( Z1=0.015) are still possible. The cooling times obtained for each planet are similar to recent calculations with the Voyager rotation periods: Neptune's luminosity can be explained by assuming an adiabatic interior while Uranus cools far too slowly. More accurate determinations of these planets' gravity fields, shapes, rotation periods, atmospheric heavy element abundances, and intrinsic luminosities are essential for improving our understanding of the internal structure and evolution of icy planets. © 2012 Elsevier Ltd.
Back to the Moon: The scientific rationale for resuming lunar surface explorationI. A. Crawford | M. Anand | C. S. Cockell | H. Falcke | D. A. Green | R. Jaumann | M. A. Wieczorek
Volume 74, Issue 1, December 2012, Pages 3-14
The lunar geological record has much to tell us about the earliest history of the Solar System, the origin and evolution of the Earth-Moon system, the geological evolution of rocky planets, and the near-Earth cosmic environment throughout Solar System history. In addition, the lunar surface offers outstanding opportunities for research in astronomy, astrobiology, fundamental physics, life sciences and human physiology and medicine. This paper provides an interdisciplinary review of outstanding lunar science objectives in all of these different areas. It is concluded that addressing them satisfactorily will require an end to the 40-year hiatus of lunar surface exploration, and the placing of new scientific instruments on, and the return of additional samples from, the surface of the Moon. Some of these objectives can be achieved robotically (e.g., through targeted sample return, the deployment of geophysical networks, and the placing of antennas on the lunar surface to form radio telescopes). However, in the longer term, most of these scientific objectives would benefit significantly from renewed human operations on the lunar surface. For these reasons it is highly desirable that current plans for renewed robotic surface exploration of the Moon are developed in the context of a future human lunar exploration programme, such as that proposed by the recently formulated Global Exploration Roadmap. © 2012 Elsevier Ltd. All rights reserved.
Global geological map of VenusMikhail A. Ivanov | James W. Head
Volume 59, Issue 13, October 2011, Pages 1559-1600
The surface area of Venus (∼460×106 km2) is ∼90% of that of the Earth. Using Magellan radar image and altimetry data, supplemented by Venera-15/16 radar images, we compiled a global geologic map of Venus at a scale of 1:10 M. We outline the history of geological mapping of the Earth and planets to illustrate the importance of utilizing the dual stratigraphic classification approach to geological mapping. Using this established approach, we identify 13 distinctive units on the surface of Venus and a series of structures and related features. We present the history and evolution of the definition and characterization of these units, explore and assess alternate methods and approaches that have been suggested, and trace the sequence of mapping from small areas to regional and global scales. We outline the specific defining nature and characteristics of these units, map their distribution, and assess their stratigraphic relationships. On the basis of these data, we then compare local and regional stratigraphic columns and compile a global stratigraphic column, defining rock-stratigraphic units, time-stratigraphic units, and geological time units. We use superposed craters, stratigraphic relationships and impact crater parabola degradation to assess the geologic time represented by the global stratigraphic column. Using the characteristics of these units, we interpret the geological processes that were responsible for their formation. On the basis of unit superposition and stratigraphic relationships, we interpret the sequence of events and processes recorded in the global stratigraphic column. The earliest part of the history of Venus (Pre-Fortunian) predates the observed surface geological features and units, although remnants may exist in the form of deformed rocks and minerals. We find that the observable geological history of Venus can be subdivided into three distinctive phases. The earlier phase (Fortunian Period, its lower stratigraphic boundary cannot be determined with the available data sets) involved intense deformation and building of regions of thicker crust (tessera). This was followed by the Guineverian Period. Distributed deformed plains, mountain belts, and regional interconnected groove belts characterize the first part and the vast majority of coronae began to form during this time. The second part of the Guineverian Period involved global emplacement of vast and mildly deformed plains of volcanic origin. A period of global wrinkle ridge formation largely followed the emplacement of these plains. The third phase (Atlian Period) involved the formation of prominent rift zones and fields of lava flows unmodified by wrinkle ridges that are often associated with large shield volcanoes and, in places, with earlier-formed coronae. Atlian volcanism may continue to the present. About 70% of the exposed surface of Venus was resurfaced during the Guineverian Period and only about 16% during the Atlian Period. Estimates of model absolute ages suggest that the Atlian Period was about twice as long as the Guineverian and, thus, characterized by significantly reduced rates of volcanism and tectonism. The three major phases of activity documented in the global stratigraphy and geological map, and their interpreted temporal relations, provide a basis for assessing the geodynamical processes operating earlier in Venus history that led to the preserved record. © 2011 Elsevier Ltd. All rights reserved.
The cratering history of asteroid (21) LutetiaS. Marchi | M. Massironi | J. B. Vincent | A. Morbidelli | S. Mottola | F. Marzari | M. Küppers | S. Besse | N. Thomas | C. Barbieri | G. Naletto | H. Sierks
Volume 66, Issue 1, June 2012, Pages 87-95
The European Space Agency's Rosetta spacecraft passed by the main belt asteroid (21) Lutetia on 10th July 2010. With its ∼100km size, Lutetia is one of the largest asteroids ever imaged by a spacecraft. During the flyby, the on-board OSIRIS imaging system acquired spectacular images of Lutetia's northern hemisphere revealing a complex surface scarred by numerous impact craters, reaching the maximum dimension of about 55 km. In this paper, we assess the cratering history of the asteroid. For this purpose, we apply current models describing the formation and evolution of main belt asteroids, that provide the rate and velocity distributions of impactors. These models, coupled with appropriate crater scaling laws, allow us to interpret the observed crater size-frequency distribution (SFD) and constrain the cratering history. Thanks to this approach, we derive the crater retention age of several regions on Lutetia, namely the time lapsed since their formation or global surface reset. We also investigate the influence of various factors - like Lutetia's bulk structure and crater obliteration - on the observed crater SFDs and the estimated surface ages. From our analysis, it emerges that Lutetia underwent a complex collisional evolution, involving major local resurfacing events till recent times. The difference in crater density between the youngest and oldest recognized units implies a difference in age of more than a factor of 10. The youngest unit (Beatica) has an estimated age of tens to hundreds of Myr, while the oldest one (Achaia) formed during a period when the bombardment of asteroids was more intense than the current one, presumably around 3.6 Gyr ago or older. © 2011 Elsevier Ltd.


text:
Game pieces from the Monopoly Game add a custom look to your game night party!
These Monopoly Game Piece Standee feature a silver ship, thimble and shoe printed on a red background. Each 2 feet 10 inch high x 2 feet 5 inch wide free-standing Hasbro Monopoly Game Pieces are made of cardboard and printed on one side only. Line a walkway or scatter around the dance floor for added flair at your game night party. Sold as a set of three. Easy assembly.
The MONOPOLY name and logo, the distinctive design of the game board, the four corner squares, the MR. MONOPOLY name and character, as well as each of the distinctive elements of the board and the playing pieces are trademarks of Hasbro for its property trading game and game equipment. ©1935, 201_Hasbro. All Rights Reserved.
Please allow ample time for delivery. Our ship date for this product is noted in your shopping cart. Many items are shipped separately, so please allow extra time for these items to arrive. Shipping charges are based on the value of the merchandise and not the number of shipments. For additional shipping information, contact our Customer Service Department at (email@example.com or 1-800-227-2789).
Do you have questions about this product?
Get answers from real customers and in-house experts with AnswerBox.
Q:is it possible to speak to someone? Is there a wholesale division for party planners?
1 answer
A:Our customer service is 1-800-227-2789. We do have a wholesale program - the link is at the bottom of the homepage for an application.


text:
Manchester Metropolitan University was awarded university status in 1992 and is part of the largest higher education campus in the UK and one of the most extensive education centres in Europe.
With a history dating back 150 years, we have a combination of the traditional and the contemporary that sets the University apart and gives us our distinct character.
We are one of the UK's most consistently popular Universities*, we have:
MMU is one of the top performing new universities in the UK in terms of its research profile. Our work informs curriculum developments, shapes business and professional practice and influences policy-making, both nationally and internationally.
100% of impact in Health, Education, Sociology, English and History was rated world-leading or internationally-excellent. We are the top 'new' university for the power of health research and 12th out of 94 for UK universities overall. We are in the top 20 UK universities for the quality of our Sociology research. We are ranked 16th out of 82 UK universities for the quality of our impact in History research.*
*Research Excellence Framework 2014 Results
We pride ourselves on training the future talent of the region as 70% of our graduates stay and work in the North West.
We work in partnership across the region, with 45% of our courses having links with our community. We provide a range of services to the local community including real-world research, events and sporting facilities.
MMU's contribution to local industry takes many forms; providing continuing professional development courses, working with businesses in Knowledge Transfer Partnerships and providing work-ready graduates with the skills and expertise that will add value to your business.
Many organisations offer scholarships or grants. Some of these might help you to study for a Master at Manchester Metropolitan University!
At Manchester Met, we have a student support officer based in each faculty. This officer is available throughout the year to provide advice and guidance on any aspect of University life, including finding your way around campus and Manchester, presentation skills, exam tips and dealing with stress.
The accommodation at Manchester Metropolitan University offers a comfortable space in which students from varying backgrounds and studying a variety of courses live in a mutually-supportive environment. Your accommodation will allow you the space to live comfortably and meet other students from across the university.Here at Manchester Metropolitan University we want you to benefit from you university residential experience, as this can be just as important as your academic pursuits.
There isn't a single aspect of the University that doesn't rely on IT Services. We invest millions on technology designed to make your life easier and improve your experience studying here at Manchester Metropolitan.Our services include:
Our services include:
Manchester Metropolitan University is based on 2 campuses – one in Manchester and one in Crewe, Cheshire.Travelling to the Manchester and Cheshire campuses couldn't be easier. The region is well served by motorways, good public transport and Manchester International Airport is just 10 miles (16km) south of the city centre, with fast and frequent rail links to both Manchester and Cheshire.
We have several fantastic sports facilities right on our doorstep, offering a great range of health and fitness activities and exclusive membership deals for students and members of staff at Manchester Metropolitan University.
The Students' Union commits to representing all students and strives to ensure that the needs and views of students are at the heart of everything the University does.
The Institute of Biomedical Science accredits our MSc and BSc degrees in Biomedical Science and certain routes within the BSc Healthcare Science degree. BSc (Hons) Healthcare Science is also accredited by Health Education England, the Registration Council for Clinical Physiologists and the Health and Care Professions Council.
Together with the ISIC Association and British Council IELTS, StudyPortals offers you the chance to receive up to £10000 to expand your horizon and study abroad. We want to ultimately encourage you to study abroad in order to experience and explore new countries, cultures and languages.


text:
(forgot?) or Register
Comment Tweets gives you the ability to take the URL of a tweet and add it to the conversation on your blog.
Download Version 2.2.0
Requires: 3.4.1 or higher
Compatible up to: 4.2.10
Last Updated: 1 year ago
Active Installs:
Got something to say? Need help?
Translate Comment Tweets
0 people say it works.
0 people say it's broken.
Log in to vote.