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  • 1
    Publication Date: 2019
    Description: Abstract Rosetta observations of 67P/Churyumov‐Gerasimenko (67P) reveal that most changes occur in the fallback‐generated smooth terrains, vast deposits of granular material blanketing the comet's northern hemisphere. These changes express themselves both morphologically and spectrally across the nucleus, yet we lack a model that describes their formation and evolution. Here we present a self‐consistent model that thoroughly explains the activity and mass loss from Hapi's smooth terrains. Our model predicts the removal of dust via re‐radiated solar insolation localized within depression scarps that are substantially more ice‐rich than previously expected. We couple our model with numerous Rosetta observations to thoroughly capture the seasonal erosion of Hapi's smooth terrains, where local scarp retreat gradually removes the uppermost dusty mantle. As sublimation‐regolith interactions occur on rocky planets, comets, icy moons and KBOs, our coupled model and observations provide a foundation for future understanding of the myriad of sublimation‐carved worlds.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
    Publication Date: 2015-06-27
    Description: The OSIRIS experiment onboard the Rosetta spacecraft currently orbiting comet 67P/Churyumov-Gerasimenko has yielded unprecedented views of a comet's nucleus. We present here the first ever observations of meter-scale fractures on the surface of a comet. Some of these fractures form polygonal networks. We present an initial assessment of their morphology, topology, and regional distribution. Fractures are ubiquitous on the surface of the comet's nucleus. Furthermore, they occur in various settings and show different topologies suggesting numerous formation mechanisms, which include thermal insolation weathering, orbital-induced stresses, and possibly seasonal thermal contraction. However, we conclude that thermal insolation weathering is responsible for creating most of the observed fractures based on their morphology and setting in addition to thermal models that indicate diurnal temperature ranges exceeding 200 K and thermal gradients of ~15 K/min at perihelion are possible. Finally, we suggest that fractures could be a facilitator in surface evolution and long-term erosion.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
    Publication Date: 2010-06-10
    Description: The autism spectrum disorders (ASDs) are a group of conditions characterized by impairments in reciprocal social interaction and communication, and the presence of restricted and repetitive behaviours. Individuals with an ASD vary greatly in cognitive development, which can range from above average to intellectual disability. Although ASDs are known to be highly heritable ( approximately 90%), the underlying genetic determinants are still largely unknown. Here we analysed the genome-wide characteristics of rare (〈1% frequency) copy number variation in ASD using dense genotyping arrays. When comparing 996 ASD individuals of European ancestry to 1,287 matched controls, cases were found to carry a higher global burden of rare, genic copy number variants (CNVs) (1.19 fold, P = 0.012), especially so for loci previously implicated in either ASD and/or intellectual disability (1.69 fold, P = 3.4 x 10(-4)). Among the CNVs there were numerous de novo and inherited events, sometimes in combination in a given family, implicating many novel ASD genes such as SHANK2, SYNGAP1, DLGAP2 and the X-linked DDX53-PTCHD1 locus. We also discovered an enrichment of CNVs disrupting functional gene sets involved in cellular proliferation, projection and motility, and GTPase/Ras signalling. Our results reveal many new genetic and functional targets in ASD that may lead to final connected pathways.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC3021798/" target="_blank"〉〈img src="https://static.pubmed.gov/portal/portal3rc.fcgi/4089621/img/3977009" border="0"〉〈/a〉   〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC3021798/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pinto, Dalila -- Pagnamenta, Alistair T -- Klei, Lambertus -- Anney, Richard -- Merico, Daniele -- Regan, Regina -- Conroy, Judith -- Magalhaes, Tiago R -- Correia, Catarina -- Abrahams, Brett S -- Almeida, Joana -- Bacchelli, Elena -- Bader, Gary D -- Bailey, Anthony J -- Baird, Gillian -- Battaglia, Agatino -- Berney, Tom -- Bolshakova, Nadia -- Bolte, Sven -- Bolton, Patrick F -- Bourgeron, Thomas -- Brennan, Sean -- Brian, Jessica -- Bryson, Susan E -- Carson, Andrew R -- Casallo, Guillermo -- Casey, Jillian -- Chung, Brian H Y -- Cochrane, Lynne -- Corsello, Christina -- Crawford, Emily L -- Crossett, Andrew -- Cytrynbaum, Cheryl -- Dawson, Geraldine -- de Jonge, Maretha -- Delorme, Richard -- Drmic, Irene -- Duketis, Eftichia -- Duque, Frederico -- Estes, Annette -- Farrar, Penny -- Fernandez, Bridget A -- Folstein, Susan E -- Fombonne, Eric -- Freitag, Christine M -- Gilbert, John -- Gillberg, Christopher -- Glessner, Joseph T -- Goldberg, Jeremy -- Green, Andrew -- Green, Jonathan -- Guter, Stephen J -- Hakonarson, Hakon -- Heron, Elizabeth A -- Hill, Matthew -- Holt, Richard -- Howe, Jennifer L -- Hughes, Gillian -- Hus, Vanessa -- Igliozzi, Roberta -- Kim, Cecilia -- Klauck, Sabine M -- Kolevzon, Alexander -- Korvatska, Olena -- Kustanovich, Vlad -- Lajonchere, Clara M -- Lamb, Janine A -- Laskawiec, Magdalena -- Leboyer, Marion -- Le Couteur, Ann -- Leventhal, Bennett L -- Lionel, Anath C -- Liu, Xiao-Qing -- Lord, Catherine -- Lotspeich, Linda -- Lund, Sabata C -- Maestrini, Elena -- Mahoney, William -- Mantoulan, Carine -- Marshall, Christian R -- McConachie, Helen -- McDougle, Christopher J -- McGrath, Jane -- McMahon, William M -- Merikangas, Alison -- Migita, Ohsuke -- Minshew, Nancy J -- Mirza, Ghazala K -- Munson, Jeff -- Nelson, Stanley F -- Noakes, Carolyn -- Noor, Abdul -- Nygren, Gudrun -- Oliveira, Guiomar -- Papanikolaou, Katerina -- Parr, Jeremy R -- Parrini, Barbara -- Paton, Tara -- Pickles, Andrew -- Pilorge, Marion -- Piven, Joseph -- Ponting, Chris P -- Posey, David J -- Poustka, Annemarie -- Poustka, Fritz -- Prasad, Aparna -- Ragoussis, Jiannis -- Renshaw, Katy -- Rickaby, Jessica -- Roberts, Wendy -- Roeder, Kathryn -- Roge, Bernadette -- Rutter, Michael L -- Bierut, Laura J -- Rice, John P -- Salt, Jeff -- Sansom, Katherine -- Sato, Daisuke -- Segurado, Ricardo -- Sequeira, Ana F -- Senman, Lili -- Shah, Naisha -- Sheffield, Val C -- Soorya, Latha -- Sousa, Ines -- Stein, Olaf -- Sykes, Nuala -- Stoppioni, Vera -- Strawbridge, Christina -- Tancredi, Raffaella -- Tansey, Katherine -- Thiruvahindrapduram, Bhooma -- Thompson, Ann P -- Thomson, Susanne -- Tryfon, Ana -- Tsiantis, John -- Van Engeland, Herman -- Vincent, John B -- Volkmar, Fred -- Wallace, Simon -- Wang, Kai -- Wang, Zhouzhi -- Wassink, Thomas H -- Webber, Caleb -- Weksberg, Rosanna -- Wing, Kirsty -- Wittemeyer, Kerstin -- Wood, Shawn -- Wu, Jing -- Yaspan, Brian L -- Zurawiecki, Danielle -- Zwaigenbaum, Lonnie -- Buxbaum, Joseph D -- Cantor, Rita M -- Cook, Edwin H -- Coon, Hilary -- Cuccaro, Michael L -- Devlin, Bernie -- Ennis, Sean -- Gallagher, Louise -- Geschwind, Daniel H -- Gill, Michael -- Haines, Jonathan L -- Hallmayer, Joachim -- Miller, Judith -- Monaco, Anthony P -- Nurnberger, John I Jr -- Paterson, Andrew D -- Pericak-Vance, Margaret A -- Schellenberg, Gerard D -- Szatmari, Peter -- Vicente, Astrid M -- Vieland, Veronica J -- Wijsman, Ellen M -- Scherer, Stephen W -- Sutcliffe, James S -- Betancur, Catalina -- 075491/Z/04/Wellcome Trust/United Kingdom -- AS2077/Autism Speaks/ -- AS7462/Autism Speaks/ -- G0601030/Medical Research Council/United Kingdom -- HD055751/HD/NICHD NIH HHS/ -- HD055782/HD/NICHD NIH HHS/ -- HD055784/HD/NICHD NIH HHS/ -- HD35465/HD/NICHD NIH HHS/ -- MC_U137761446/Medical Research Council/United Kingdom -- MH061009/MH/NIMH NIH HHS/ -- MH06359/MH/NIMH NIH HHS/ -- MH066673/MH/NIMH NIH HHS/ -- MH080647/MH/NIMH NIH HHS/ -- MH081754/MH/NIMH NIH HHS/ -- MH52708/MH/NIMH NIH HHS/ -- MH55284/MH/NIMH NIH HHS/ -- MH57881/MH/NIMH NIH HHS/ -- MH66766/MH/NIMH NIH HHS/ -- NS026630/NS/NINDS NIH HHS/ -- NS042165/NS/NINDS NIH HHS/ -- NS049261/NS/NINDS NIH HHS/ -- P01 CA089392/CA/NCI NIH HHS/ -- P01 CA089392-08/CA/NCI NIH HHS/ -- P01 HD035465-01S1/HD/NICHD NIH HHS/ -- P01 NS026630/NS/NINDS NIH HHS/ -- P01 NS026630-15/NS/NINDS NIH HHS/ -- P50 HD055748/HD/NICHD NIH HHS/ -- P50 HD055748-01/HD/NICHD NIH HHS/ -- P50 HD055748-02/HD/NICHD NIH HHS/ -- P50 HD055748-03/HD/NICHD NIH HHS/ -- P50 HD055751/HD/NICHD NIH HHS/ -- P50 HD055751-01/HD/NICHD NIH HHS/ -- P50 HD055782/HD/NICHD NIH HHS/ -- P50 HD055782-04/HD/NICHD NIH HHS/ -- R01 DA013423/DA/NIDA NIH HHS/ -- R01 DA013423-05/DA/NIDA NIH HHS/ -- R01 DA019963/DA/NIDA NIH HHS/ -- R01 DA019963-01A2/DA/NIDA NIH HHS/ -- R01 DA019963-02/DA/NIDA NIH HHS/ -- R01 DA019963-03/DA/NIDA NIH HHS/ -- R01 MH052708-05/MH/NIMH NIH HHS/ -- R01 MH055284/MH/NIMH NIH HHS/ -- R01 MH055284-04/MH/NIMH NIH HHS/ -- R01 MH057881/MH/NIMH NIH HHS/ -- R01 MH057881-02/MH/NIMH NIH HHS/ -- R01 MH061009/MH/NIMH NIH HHS/ -- R01 MH061009-05/MH/NIMH NIH HHS/ -- R01 MH080647/MH/NIMH NIH HHS/ -- R01 MH080647-11/MH/NIMH NIH HHS/ -- R01 MH081754/MH/NIMH NIH HHS/ -- R01 MH081754-01/MH/NIMH NIH HHS/ -- R01 NS042165/NS/NINDS NIH HHS/ -- R01 NS042165-05/NS/NINDS NIH HHS/ -- R01 NS049261/NS/NINDS NIH HHS/ -- R01 NS049261-02/NS/NINDS NIH HHS/ -- U01 HG004422/HG/NHGRI NIH HHS/ -- U01 HG004422-02/HG/NHGRI NIH HHS/ -- U10 MH066766-05/MH/NIMH NIH HHS/ -- U19 HD035469/HD/NICHD NIH HHS/ -- U19 HD035469-06/HD/NICHD NIH HHS/ -- U19 HD035469-07/HD/NICHD NIH HHS/ -- U19 HD035469-08/HD/NICHD NIH HHS/ -- U19 HD035469-09/HD/NICHD NIH HHS/ -- U19 HD035469-10/HD/NICHD NIH HHS/ -- U54 MH066673/MH/NIMH NIH HHS/ -- U54 MH066673-05/MH/NIMH NIH HHS/ -- UL1 TR000448/TR/NCATS NIH HHS/ -- Canadian Institutes of Health Research/Canada -- Medical Research Council/United Kingdom -- England -- Nature. 2010 Jul 15;466(7304):368-72. doi: 10.1038/nature09146. Epub 2010 Jun 9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉The Centre for Applied Genomics and Program in Genetics and Genomic Biology, The Hospital for Sick Children, Toronto, Ontario M5G 1L7, Canada.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20531469" target="_blank"〉PubMed〈/a〉
    Keywords: Case-Control Studies ; Cell Movement ; Child ; Child Development Disorders, Pervasive/*genetics/pathology/*physiopathology ; Cytoprotection ; DNA Copy Number Variations/*genetics ; Europe/ethnology ; Gene Dosage/*genetics ; Genetic Predisposition to Disease/*genetics ; Genome-Wide Association Study ; Humans ; Signal Transduction ; Social Behavior
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 4
    Publication Date: 2010-10-15
    Description: The peculiar object P/2010 A2 was discovered in January 2010 and given a cometary designation because of the presence of a trail of material, although there was no central condensation or coma. The appearance of this object, in an asteroidal orbit (small eccentricity and inclination) in the inner main asteroid belt attracted attention as a potential new member of the recently recognized class of main-belt comets. If confirmed, this new object would expand the range in heliocentric distance over which main-belt comets are found. Here we report observations of P/2010 A2 by the Rosetta spacecraft. We conclude that the trail arose from a single event, rather than a period of cometary activity, in agreement with independent results. The trail is made up of relatively large particles of millimetre to centimetre size that remain close to the parent asteroid. The shape of the trail can be explained by an initial impact ejecting large clumps of debris that disintegrated and dispersed almost immediately. We determine that this was an asteroid collision that occurred around 10 February 2009.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Snodgrass, Colin -- Tubiana, Cecilia -- Vincent, Jean-Baptiste -- Sierks, Holger -- Hviid, Stubbe -- Moissl, Richard -- Boehnhardt, Hermann -- Barbieri, Cesare -- Koschny, Detlef -- Lamy, Philippe -- Rickman, Hans -- Rodrigo, Rafael -- Carry, Benoit -- Lowry, Stephen C -- Laird, Ryan J M -- Weissman, Paul R -- Fitzsimmons, Alan -- Marchi, Simone -- OSIRIS team -- England -- Nature. 2010 Oct 14;467(7317):814-6. doi: 10.1038/nature09453.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany. snodgrass@mps.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20944742" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 5
    Publication Date: 2015-07-03
    Description: Pits have been observed on many cometary nuclei mapped by spacecraft. It has been argued that cometary pits are a signature of endogenic activity, rather than impact craters such as those on planetary and asteroid surfaces. Impact experiments and models cannot reproduce the shapes of most of the observed cometary pits, and the predicted collision rates imply that few of the pits are related to impacts. Alternative mechanisms like explosive activity have been suggested, but the driving process remains unknown. Here we report that pits on comet 67P/Churyumov-Gerasimenko are active, and probably created by a sinkhole process, possibly accompanied by outbursts. We argue that after formation, pits expand slowly in diameter, owing to sublimation-driven retreat of the walls. Therefore, pits characterize how eroded the surface is: a fresh cometary surface will have a ragged structure with many pits, while an evolved surface will look smoother. The size and spatial distribution of pits imply that large heterogeneities exist in the physical, structural or compositional properties of the first few hundred metres below the current nucleus surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Vincent, Jean-Baptiste -- Bodewits, Dennis -- Besse, Sebastien -- Sierks, Holger -- Barbieri, Cesare -- Lamy, Philippe -- Rodrigo, Rafael -- Koschny, Detlef -- Rickman, Hans -- Keller, Horst Uwe -- Agarwal, Jessica -- A'Hearn, Michael F -- Auger, Anne-Therese -- Barucci, M Antonella -- Bertaux, Jean-Loup -- Bertini, Ivano -- Capanna, Claire -- Cremonese, Gabriele -- Da Deppo, Vania -- Davidsson, Bjorn -- Debei, Stefano -- De Cecco, Mariolino -- El-Maarry, Mohamed Ramy -- Ferri, Francesca -- Fornasier, Sonia -- Fulle, Marco -- Gaskell, Robert -- Giacomini, Lorenza -- Groussin, Olivier -- Guilbert-Lepoutre, Aurelie -- Gutierrez-Marques, P -- Gutierrez, Pedro J -- Guttler, Carsten -- Hoekzema, Nick -- Hofner, Sebastian -- Hviid, Stubbe F -- Ip, Wing-Huen -- Jorda, Laurent -- Knollenberg, Jorg -- Kovacs, Gabor -- Kramm, Rainer -- Kuhrt, Ekkehard -- Kuppers, Michael -- La Forgia, Fiorangela -- Lara, Luisa M -- Lazzarin, Monica -- Lee, Vicky -- Leyrat, Cedric -- Lin, Zhong-Yi -- Lopez Moreno, Jose J -- Lowry, Stephen -- Magrin, Sara -- Maquet, Lucie -- Marchi, Simone -- Marzari, Francesco -- Massironi, Matteo -- Michalik, Harald -- Moissl, Richard -- Mottola, Stefano -- Naletto, Giampiero -- Oklay, Nilda -- Pajola, Maurizio -- Preusker, Frank -- Scholten, Frank -- Thomas, Nicolas -- Toth, Imre -- Tubiana, Cecilia -- England -- Nature. 2015 Jul 2;523(7558):63-6. doi: 10.1038/nature14564.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; University of Maryland, Department of Astronomy, College Park, Maryland 20742-2421, USA. ; Scientific Support Office, European Space Research and Technology Centre/ESA, Keplerlaan 1, Postbus 299, 2201 AZ Noordwijk ZH, The Netherlands. ; University of Padova, Department of Physics and Astronomy, Vicolo dell'Osservatorio 3, 35122 Padova, Italy. ; Laboratoire d'Astrophysique de Marseille, UMR 7326, CNRS and Aix Marseille Universite, 13388 Marseille Cedex 13, France. ; 1] Centro de Astrobiologia, CSIC-INTA, 28850 Torrejon de Ardoz, Madrid, Spain [2] International Space Science Institute, Hallerstrasse 6, 3012 Bern, Switzerland. ; 1] Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden [2] PAS Space Research Center, Bartycka 18A, 00716 Warszawa, Poland. ; Institut fur Geophysik und extraterrestrische Physik (IGEP), Technische Universitat Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany. ; 1] University of Maryland, Department of Astronomy, College Park, Maryland 20742-2421, USA [2] Akademie der Wissenschaften zu Gottingen and Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Gottingen, Germany. ; LESIA-Observatoire de Paris, CNRS, Universite Pierre et Marie Curie, Universite Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France. ; LATMOS, CNRS/UVSQ/IPSL, 11 boulevard d'Alembert, 78280 Guyancourt, France. ; Centro di Ateneo di Studi ed Attivita Spaziali "Giuseppe Colombo" (CISAS), University of Padova, via Venezia 15, 35131 Padova, Italy. ; INAF, Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy. ; CNR-IFN UOS Padova LUXOR, via Trasea 7, 35131 Padova, Italy. ; Centro de Astrobiologia, CSIC-INTA, 28850 Torrejon de Ardoz, Madrid, Spain. ; Department of Industrial Engineering, University of Padova, via Venezia 1, 35131 Padova, Italy. ; University of Trento, via Mesiano 77, 38100 Trento, Italy. ; Physikalisches Institut der Universitat Bern, Sidlerstrasse 5, 3012 Bern, Switzerland. ; INAF Osservatorio Astronomico, via Tiepolo 11, 34014 Trieste, Italy. ; Planetary Science Institute, Tucson, Arizona 85719, USA. ; Instituto de Astrofisica de Andalucia (CSIC), Glorieta de la Astronomia s/n, 18008 Granada, Spain. ; Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Institut fur Planetenforschung, Rutherfordstrasse 2, 12489 Berlin, Germany. ; National Central University, Graduate Institute of Astronomy, 300 Chung-Da Rd, Chung-Li 32054, Taiwan. ; Operations Department, European Space Astronomy Centre/ESA, PO Box 78, 28691 Villanueva de la Canada, Madrid, Spain. ; The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK. ; University of Padova, Deptartment of Physics and Astronomy, via Marzolo 8, 35131 Padova, Italy. ; Solar System Exploration Research Virtual Institute, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, Colorado 80302, USA. ; Dipartimento di Geoscienze, University of Padova, via Giovanni Gradenigo 6, 35131 Padova, Italy. ; Institut fur Datentechnik und Kommunikationsnetze der Technische Universitat Braunschweig, Hans-Sommer-Strasse 66, 38106 Braunschweig, Germany. ; 1] Centro di Ateneo di Studi ed Attivita Spaziali "Giuseppe Colombo" (CISAS), University of Padova, via Venezia 15, 35131 Padova, Italy [2] CNR-IFN UOS Padova LUXOR, via Trasea 7, 35131 Padova, Italy [3] University of Padova, Department of Information Engineering, via Gradenigo 6/B, 35131 Padova, Italy. ; Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, 1525 Budapest, Hungary.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26135448" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2015-09-30
    Description: The factors shaping cometary nuclei are still largely unknown, but could be the result of concurrent effects of evolutionary and primordial processes. The peculiar bilobed shape of comet 67P/Churyumov-Gerasimenko may be the result of the fusion of two objects that were once separate or the result of a localized excavation by outgassing at the interface between the two lobes. Here we report that the comet's major lobe is enveloped by a nearly continuous set of strata, up to 650 metres thick, which are independent of an analogous stratified envelope on the minor lobe. Gravity vectors computed for the two lobes separately are closer to perpendicular to the strata than those calculated for the entire nucleus and adjacent to the neck separating the two lobes. Therefore comet 67P/Churyumov-Gerasimenko is an accreted body of two distinct objects with 'onion-like' stratification, which formed before they merged. We conclude that gentle, low-velocity collisions occurred between two fully formed kilometre-sized cometesimals in the early stages of the Solar System. The notable structural similarities between the two lobes of comet 67P/Churyumov-Gerasimenko indicate that the early-forming cometesimals experienced similar primordial stratified accretion, even though they formed independently.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Massironi, Matteo -- Simioni, Emanuele -- Marzari, Francesco -- Cremonese, Gabriele -- Giacomini, Lorenza -- Pajola, Maurizio -- Jorda, Laurent -- Naletto, Giampiero -- Lowry, Stephen -- El-Maarry, Mohamed Ramy -- Preusker, Frank -- Scholten, Frank -- Sierks, Holger -- Barbieri, Cesare -- Lamy, Philippe -- Rodrigo, Rafael -- Koschny, Detlef -- Rickman, Hans -- Keller, Horst Uwe -- A'Hearn, Michael F -- Agarwal, Jessica -- Auger, Anne-Therese -- Barucci, M Antonella -- Bertaux, Jean-Loup -- Bertini, Ivano -- Besse, Sebastien -- Bodewits, Dennis -- Capanna, Claire -- Da Deppo, Vania -- Davidsson, Bjorn -- Debei, Stefano -- De Cecco, Mariolino -- Ferri, Francesca -- Fornasier, Sonia -- Fulle, Marco -- Gaskell, Robert -- Groussin, Olivier -- Gutierrez, Pedro J -- Guttler, Carsten -- Hviid, Stubbe F -- Ip, Wing-Huen -- Knollenberg, Jorg -- Kovacs, Gabor -- Kramm, Rainer -- Kuhrt, Ekkehard -- Kuppers, Michael -- La Forgia, Fiorangela -- Lara, Luisa M -- Lazzarin, Monica -- Lin, Zhong-Yi -- Lopez Moreno, Jose J -- Magrin, Sara -- Michalik, Harald -- Mottola, Stefano -- Oklay, Nilda -- Pommerol, Antoine -- Thomas, Nicolas -- Tubiana, Cecilia -- Vincent, Jean-Baptiste -- England -- Nature. 2015 Oct 15;526(7573):402-5. doi: 10.1038/nature15511. Epub 2015 Sep 28.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Dipartimento di Geoscienze, University of Padova, via G. Gradenigo 6, 35131 Padova, Italy. ; Centro di Ateneo di Studi ed Attivita Spaziali "Giuseppe Colombo" (CISAS), University of Padova, via Venezia 15, 35131 Padova, Italy. ; CNR-IFN UOS Padova LUXOR, via Trasea 7, 35131 Padova, Italy. ; University of Padova, Department of Physics and Astronomy, Vicolo dell'Osservatorio 3, 35122 Padova, Italy. ; INAF, Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy. ; Aix Marseille Universite, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 38 rue Frederic Joliot-Curie, 13388 Marseille, France. ; Department of Information Engineering, University of Padova, via Gradenigo 6/B, 35131 Padova, Italy. ; The University of Kent, School of Physical Sciences, Canterbury, Kent CT2 7NZ, UK. ; Physikalisches Institut der Universitat Bern, Sidlerstrasse 5, 3012 Bern, Switzerland. ; Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Institut fur Planetenforschung, Rutherfordstrasse 2, 12489 Berlin, Germany. ; Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig Weg 3, 37077 Gottingen, Germany. ; Centro de Astrobiologia, CSIC-INTA, 28850 Torrejon de Ardoz, Madrid, Spain. ; International Space Science Institute, Hallerstrasse 6, 3012 Bern, Switzerland. ; Scientific Support Office, European Space Research and Technology Centre/ESA, Keplerlaan 1, Postbus 299, 2201 AZ Noordwijk ZH, The Netherlands. ; Department of Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden. ; PAS Space Research Center, Bartycka 18A, 00716 Warszawa, Poland. ; Institut fur Geophysik und extraterrestrische Physik (IGEP), Technische Universitat Braunschweig, Mendelssohnstrasse 3, 38106 Braunschweig, Germany. ; University of Maryland, Department of Astronomy, College Park, Maryland 20742-2421, USA. ; Akademie der Wissenschaften zu Gottingen and Max-Planck-Institut fur Sonnensystemforschung, Justus-von-Liebig Weg 3, 37077 Gottingen, Germany. ; LESIA-Observatoire de Paris, CNRS, Universite Pierre et Marie Curie, Universite Paris Diderot, 5 place J. Janssen, 92195 Meudon, France. ; LATMOS, CNRS/UVSQ/IPSL, 11 boulevard d'Alembert, 78280 Guyancourt, France. ; Department of Industrial Engineering, University of Padova, via Venezia 1, 35131 Padova, Italy. ; University of Trento, Via Mesiano 77, 38100 Trento, Italy. ; INAF-Osservatorio Astronomico, Via Tiepolo 11, 34014 Trieste, Italy. ; Planetary Science Institute, Tucson, Arizona 85719, USA. ; Instituto de Astrofisica de Andalucia (CSIC), Glorieta de la Astronomia s/n, 18008 Granada, Spain. ; National Central University, Graduate Institute of Astronomy, 300 Chung-Da Road, Chung-Li 32054 Taiwan. ; Operations Department, European Space Astronomy Centre/ESA, PO Box 78, 28691 Villanueva de la Canada, Madrid, Spain. ; Institut fur Datentechnik und Kommunikationsnetze der TU Braunschweig, Hans-Sommer Strasse 66, 38106 Braunschweig, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26416730" target="_blank"〉PubMed〈/a〉
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  • 7
    Publication Date: 2012-05-15
    Description: Vesta's surface is characterized by abundant impact craters, some with preserved ejecta blankets, large troughs extending around the equatorial region, enigmatic dark material, and widespread mass wasting, but as yet an absence of volcanic features. Abundant steep slopes indicate that impact-generated surface regolith is underlain by bedrock. Dawn observations confirm the large impact basin (Rheasilvia) at Vesta's south pole and reveal evidence for an earlier, underlying large basin (Veneneia). Vesta's geology displays morphological features characteristic of the Moon and terrestrial planets as well as those of other asteroids, underscoring Vesta's unique role as a transitional solar system body.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jaumann, R -- Williams, D A -- Buczkowski, D L -- Yingst, R A -- Preusker, F -- Hiesinger, H -- Schmedemann, N -- Kneissl, T -- Vincent, J B -- Blewett, D T -- Buratti, B J -- Carsenty, U -- Denevi, B W -- De Sanctis, M C -- Garry, W B -- Keller, H U -- Kersten, E -- Krohn, K -- Li, J-Y -- Marchi, S -- Matz, K D -- McCord, T B -- McSween, H Y -- Mest, S C -- Mittlefehldt, D W -- Mottola, S -- Nathues, A -- Neukum, G -- O'Brien, D P -- Pieters, C M -- Prettyman, T H -- Raymond, C A -- Roatsch, T -- Russell, C T -- Schenk, P -- Schmidt, B E -- Scholten, F -- Stephan, K -- Sykes, M V -- Tricarico, P -- Wagner, R -- Zuber, M T -- Sierks, H -- New York, N.Y. -- Science. 2012 May 11;336(6082):687-90. doi: 10.1126/science.1219122.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉German Aerospace Center, Institute of Planetary Research, Berlin, Germany. ralf.jaumann@dlr.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22582254" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
    Publication Date: 2003-04-12
    Description: DNA sequence and annotation of the entire human chromosome 7, encompassing nearly 158 million nucleotides of DNA and 1917 gene structures, are presented. To generate a higher order description, additional structural features such as imprinted genes, fragile sites, and segmental duplications were integrated at the level of the DNA sequence with medical genetic data, including 440 chromosome rearrangement breakpoints associated with disease. This approach enabled the discovery of candidate genes for developmental diseases including autism.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC2882961/" target="_blank"〉〈img src="https://static.pubmed.gov/portal/portal3rc.fcgi/4089621/img/3977009" border="0"〉〈/a〉   〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC2882961/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Scherer, Stephen W -- Cheung, Joseph -- MacDonald, Jeffrey R -- Osborne, Lucy R -- Nakabayashi, Kazuhiko -- Herbrick, Jo-Anne -- Carson, Andrew R -- Parker-Katiraee, Layla -- Skaug, Jennifer -- Khaja, Razi -- Zhang, Junjun -- Hudek, Alexander K -- Li, Martin -- Haddad, May -- Duggan, Gavin E -- Fernandez, Bridget A -- Kanematsu, Emiko -- Gentles, Simone -- Christopoulos, Constantine C -- Choufani, Sanaa -- Kwasnicka, Dorota -- Zheng, Xiangqun H -- Lai, Zhongwu -- Nusskern, Deborah -- Zhang, Qing -- Gu, Zhiping -- Lu, Fu -- Zeesman, Susan -- Nowaczyk, Malgorzata J -- Teshima, Ikuko -- Chitayat, David -- Shuman, Cheryl -- Weksberg, Rosanna -- Zackai, Elaine H -- Grebe, Theresa A -- Cox, Sarah R -- Kirkpatrick, Susan J -- Rahman, Nazneen -- Friedman, Jan M -- Heng, Henry H Q -- Pelicci, Pier Giuseppe -- Lo-Coco, Francesco -- Belloni, Elena -- Shaffer, Lisa G -- Pober, Barbara -- Morton, Cynthia C -- Gusella, James F -- Bruns, Gail A P -- Korf, Bruce R -- Quade, Bradley J -- Ligon, Azra H -- Ferguson, Heather -- Higgins, Anne W -- Leach, Natalia T -- Herrick, Steven R -- Lemyre, Emmanuelle -- Farra, Chantal G -- Kim, Hyung-Goo -- Summers, Anne M -- Gripp, Karen W -- Roberts, Wendy -- Szatmari, Peter -- Winsor, Elizabeth J T -- Grzeschik, Karl-Heinz -- Teebi, Ahmed -- Minassian, Berge A -- Kere, Juha -- Armengol, Lluis -- Pujana, Miguel Angel -- Estivill, Xavier -- Wilson, Michael D -- Koop, Ben F -- Tosi, Sabrina -- Moore, Gudrun E -- Boright, Andrew P -- Zlotorynski, Eitan -- Kerem, Batsheva -- Kroisel, Peter M -- Petek, Erwin -- Oscier, David G -- Mould, Sarah J -- Dohner, Hartmut -- Dohner, Konstanze -- Rommens, Johanna M -- Vincent, John B -- Venter, J Craig -- Li, Peter W -- Mural, Richard J -- Adams, Mark D -- Tsui, Lap-Chee -- 38103/Canadian Institutes of Health Research/Canada -- P01 GM061354/GM/NIGMS NIH HHS/ -- New York, N.Y. -- Science. 2003 May 2;300(5620):767-72. Epub 2003 Apr 10.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Genetics and Genomic Biology, The Hospital for Sick Children, Toronto, Ontario, Canada, M5G 1X8. steve@genet.sickkids.on.ca〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12690205" target="_blank"〉PubMed〈/a〉
    Keywords: Animals ; Autistic Disorder/genetics ; Chromosome Aberrations ; Chromosome Fragile Sites ; Chromosome Fragility ; Chromosome Mapping ; Chromosomes, Human, Pair 7/*genetics ; Computational Biology ; Congenital Abnormalities/genetics ; CpG Islands ; DNA, Complementary ; Databases, Genetic ; Euchromatin/genetics ; Expressed Sequence Tags ; Gene Duplication ; Genes, Overlapping ; Genetic Diseases, Inborn/genetics ; Genomic Imprinting ; Humans ; In Situ Hybridization, Fluorescence ; Limb Deformities, Congenital/genetics ; Mice ; Molecular Sequence Data ; Mutation ; Neoplasms/genetics ; Pseudogenes ; RNA/genetics ; Retroelements ; *Sequence Analysis, DNA ; Williams Syndrome/genetics
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  • 9
  • 10
    Publication Date: 2015-12-15
    Description: The dwarf planet (1) Ceres, the largest object in the main asteroid belt with a mean diameter of about 950 kilometres, is located at a mean distance from the Sun of about 2.8 astronomical units (one astronomical unit is the Earth-Sun distance). Thermal evolution models suggest that it is a differentiated body with potential geological activity. Unlike on the icy satellites of Jupiter and Saturn, where tidal forces are responsible for spewing briny water into space, no tidal forces are acting on Ceres. In the absence of such forces, most objects in the main asteroid belt are expected to be geologically inert. The recent discovery of water vapour absorption near Ceres and previous detection of bound water and OH near and on Ceres (refs 5-7) have raised interest in the possible presence of surface ice. Here we report the presence of localized bright areas on Ceres from an orbiting imager. These unusual areas are consistent with hydrated magnesium sulfates mixed with dark background material, although other compositions are possible. Of particular interest is a bright pit on the floor of crater Occator that exhibits probable sublimation of water ice, producing haze clouds inside the crater that appear and disappear with a diurnal rhythm. Slow-moving condensed-ice or dust particles may explain this haze. We conclude that Ceres must have accreted material from beyond the 'snow line', which is the distance from the Sun at which water molecules condense.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nathues, A -- Hoffmann, M -- Schaefer, M -- Le Corre, L -- Reddy, V -- Platz, T -- Cloutis, E A -- Christensen, U -- Kneissl, T -- Li, J-Y -- Mengel, K -- Schmedemann, N -- Schaefer, T -- Russell, C T -- Applin, D M -- Buczkowski, D L -- Izawa, M R M -- Keller, H U -- O'Brien, D P -- Pieters, C M -- Raymond, C A -- Ripken, J -- Schenk, P M -- Schmidt, B E -- Sierks, H -- Sykes, M V -- Thangjam, G S -- Vincent, J-B -- England -- Nature. 2015 Dec 10;528(7581):237-40. doi: 10.1038/nature15754.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max Planck Institute for Solar System Research, Goettingen, Germany. ; Planetary Science Institute, Tucson, Arizona, USA. ; University of Winnipeg, Winnipeg, Canada. ; Freie Universitaet Berlin, Berlin, Germany. ; Technische Universitaet Clausthal, Clausthal-Zellerfeld, Germany. ; University of California, Los Angeles (UCLA), Los Angeles, California, USA. ; Johns Hopkins University, Laurel, Maryland, USA. ; Royal Ontario Museum, Toronto, Canada. ; TU Braunschweig, Braunschweig, Germany. ; Brown University, Providence, Rhode Island, USA. ; Jet Propulsion Laboratory, Pasadena, California, USA. ; Lunar and Planetary Institute, Houston, Texas, USA. ; Georgia Institute of Technology, Atlanta, Georgia, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26659183" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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