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  • Lunar and Planetary Science and Exploration  (61)
  • Adult
  • 2005-2009  (78)
  • 2006  (78)
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  • 2005-2009  (78)
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  • 1
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    Common Kibra alleles are associated with human memory performance (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publikationsdatum: 2006-10-21
    Beschreibung: Human memory is a polygenic trait. We performed a genome-wide screen to identify memory-related gene variants. A genomic locus encoding the brain protein KIBRA was significantly associated with memory performance in three independent, cognitively normal cohorts from Switzerland and the United States. Gene expression studies showed that KIBRA was expressed in memory-related brain structures. Functional magnetic resonance imaging detected KIBRA allele-dependent differences in hippocampal activations during memory retrieval. Evidence from these experiments suggests a role for KIBRA in human memory.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Papassotiropoulos, Andreas -- Stephan, Dietrich A -- Huentelman, Matthew J -- Hoerndli, Frederic J -- Craig, David W -- Pearson, John V -- Huynh, Kim-Dung -- Brunner, Fabienne -- Corneveaux, Jason -- Osborne, David -- Wollmer, M Axel -- Aerni, Amanda -- Coluccia, Daniel -- Hanggi, Jurgen -- Mondadori, Christian R A -- Buchmann, Andreas -- Reiman, Eric M -- Caselli, Richard J -- Henke, Katharina -- de Quervain, Dominique J-F -- P30AG19610/AG/NIA NIH HHS/ -- R01MH057899/MH/NIMH NIH HHS/ -- U01-HL086528-01/HL/NHLBI NIH HHS/ -- U24NS051872/NS/NINDS NIH HHS/ -- New York, N.Y. -- Science. 2006 Oct 20;314(5798):475-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Division of Psychiatry Research, University of Zurich, Zurich 8057, Switzerland. papas@bli.unizh.ch〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17053149" target="_blank"〉PubMed〈/a〉
    Schlagwort(e): Adolescent ; Adult ; Alleles ; Animals ; Attention ; Brain/*physiology ; Brain Chemistry ; Calcium-Binding Proteins/genetics ; Cohort Studies ; Female ; Gene Expression ; Genotype ; Haplotypes ; Hippocampus/chemistry/*physiology ; Humans ; Intracellular Signaling Peptides and Proteins ; Magnetic Resonance Imaging ; Male ; Membrane Proteins/genetics ; *Memory ; Mice ; Middle Aged ; Phosphoproteins ; *Polymorphism, Single Nucleotide ; Proteins/analysis/*genetics/*physiology ; Reverse Transcriptase Polymerase Chain Reaction ; Switzerland ; United States
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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  • 2
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    MC1R germline variants confer risk for BRAF-mutant melanoma (2006)
    American Association for the Advancement of Science (AAAS)
    Details
    Publikationsdatum: 2006-07-01
    Beschreibung: Germline variants in MC1R, the gene encoding the melanocortin-1 receptor, and sun exposure increase risk for melanoma in Caucasians. The majority of melanomas that occur on skin with little evidence of chronic sun-induced damage (non-CSD melanoma) have mutations in the BRAF oncogene, whereas in melanomas on skin with marked CSD (CSD melanoma) these mutations are less frequent. In two independent Caucasian populations, we show that MC1R variants are strongly associated with BRAF mutations in non-CSD melanomas. In this tumor subtype, the risk for melanoma associated with MC1R is due to an increase in risk of developing melanomas with BRAF mutations.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Landi, Maria Teresa -- Bauer, Jurgen -- Pfeiffer, Ruth M -- Elder, David E -- Hulley, Benjamin -- Minghetti, Paola -- Calista, Donato -- Kanetsky, Peter A -- Pinkel, Daniel -- Bastian, Boris C -- K07 CA80700/CA/NCI NIH HHS/ -- P01 CA025874-25-A1/CA/NCI NIH HHS/ -- R01 CA5558/CA/NCI NIH HHS/ -- R01 CA94963/CA/NCI NIH HHS/ -- R33 CA95300/CA/NCI NIH HHS/ -- New York, N.Y. -- Science. 2006 Jul 28;313(5786):521-2. Epub 2006 Jun 29.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Division of Cancer Epidemiology and Genetics, National Cancer Institute, NIH, Bethesda, MD 20892, USA. landim@mail.nih.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16809487" target="_blank"〉PubMed〈/a〉
    Schlagwort(e): Adolescent ; Adult ; Aged ; Alleles ; Case-Control Studies ; Female ; Genetic Predisposition to Disease ; Genetic Variation ; *Germ-Line Mutation ; Humans ; Italy ; Male ; Melanoma/classification/*genetics/pathology ; Middle Aged ; Mutation ; Odds Ratio ; Proto-Oncogene Proteins B-raf/*genetics ; Receptor, Melanocortin, Type 1/*genetics ; Skin/pathology/*radiation effects ; Skin Neoplasms/classification/*genetics/pathology ; Sunlight/*adverse effects ; United States
    Print ISSN: 0036-8075
    Digitale ISSN: 1095-9203
    Thema: Biologie , Chemie und Pharmazie , Informatik , Medizin , Allgemeine Naturwissenschaft , Physik
    Publiziert von American Association for the Advancement of Science (AAAS)
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  • 3
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    Ar-Ar Ages of Nakhlites Y000593, NWA998, and Nakhla and CRE Age of NWA998. (2006)
    In:  CASI
    Details
    Publikationsdatum: 2019-07-13
    Beschreibung: The seven known Martian nakhlites are Nakhla, Lafayette, Governador Valadares, and four recent finds from hot and cold deserts: MIL03346 from the Transantarctic Mountains, a paired group from the Yamato Mountains (Y000593, Y000749, and Y000802; 1), and two from Morocco (NWA998 and NWA817; 2). Radiometric ages (Sm-Nd, Rb-Sr, U-Pb, and Ar-Ar) for the first three nakhlites, along with Chassigny, fall in the range of 1.19-1.37 Gyr and may suggest a common formation age (e.g., 3). These meteorites also show very similar cosmic-ray (space) exposure ages, which suggests a single ejection event from Mars (3). The ages for nakhlites are different from those of Martian shergottites, whose radiometric ages vary by nearly a factor of three (approximately 165-475 Myr) and whose space exposure ages vary over a factor of approximately 20 (3). Shergottite ages suggest that multiple locations on the Martian surface have been sampled, whereas nakhlite data imply that only one Mars surface location has been sampled. Because older Martian surfaces are expected to be more abundant, it seems surprising that all nakhlites would represent only one Martian impact event. To address this issue, we are measuring the Ar-39-Ar-40 ages of Y-000593, NWA-998, Nakhla, and MIL-03346, and the space (CRE) exposure age of NWA998.
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: Lunar and Planetary Science Conference; Mar 14, 2005 - Mar 18, 2005; League City, TX; United States
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  • 4
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    Ar-39-Ar-40 Evidence for Early Impact Events on the LL Parent Body (2006)
    In:  Other Sources
    Details
    Publikationsdatum: 2019-07-13
    Beschreibung: We determined Ar-39-Ar-40 ages of eight LL chondrites, and one igneous inclusion from an LL chondrite, with the object of understanding the thermal history of the LL-chondrite parent body. The meteorites in this study have a range of petrographic types from LL3.3 to LL6, and shock stages from S1 to S4. These meteorites reveal a range of K-Ar ages from 23.66 to 24.50 Ga, and peak ages from 23.74 to 24.55 Ga. Significantly, three of the eight chondrites (LL4, 5, 6) have K-Ar ages of -4.27 Ga. One of these (MIL99301) preserves an Ar-39-Ar-40 age of 4.23 +/- 0.03 Ga from low-temperature extractions, and an older age of 4.52 +/- 0.08 Ga from the highest temperature extractions. In addition, an igneous-textured impact melt DOM85505,22 has a peak Ar-39-Ar-40 age of 〉= 4.27 Ga. We interpret these results as evidence for impact events that occurred at about 4.27 Ga on the LL parent body that produced local impact melts, reset the Ar-39-Ar-40 ages of some meteorites, and exhumed (or interred) others, resulting in a range of cooling ages. The somewhat younger peak age of 3.74 Ga from GR095658 (LL3.3) suggests an additional impact event close to timing of impact-reset ages of some other ordinary chondrites between 3.6-3.8 Ga. The results from MIL99301 suggest that some apparently unshocked (Sl) chondrites may have substantially reset Ar-39-Ar-40 ages. A previous petrographic investigation of MIL99301 suggested that reheating to temperatures less than or equal to type 4 petrographic conditions (600C) caused fractures in olivine to anneal, resulting in a low apparent shock stage of S1 (unshocked). The Ar-39-Ar-40 age spectrum of MIL99301 is consistent with this interpretation. Older ages from high-T extractions may date an earlier impact event at 4.52 +/- 0.08 Ga, whereas younger ages from lower-T extractions date a later impact event at 4.23 Ar-39-Ar-40 0.03 Ga that may have caused annealing of feldspar and olivine
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: Geochimica et Cosmochimica Acta; 68; 18; 3779-3790
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  • 5
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    Characterization and Petrologic Interpretation of Olivine-Rich Basalts at Gusev Crater, Mars (2006)
    In:  CASI
    Details
    Publikationsdatum: 2019-07-12
    Beschreibung: Rocks on the floor of Gusev crater are basalts of uniform composition and mineralogy. Olivine, the only mineral to have been identified or inferred from data by all instruments on the Spirit rover, is especially abundant in these rocks. These picritic basalts are similar in many respects to certain Martian meteorites (olivine-phyric shergottites). The olivine megacrysts in both have intermediate compositions, with modal abundances ranging up to 20-30%. Associated minerals in both include low-calcium and high-calcium pyroxenes, plagioclase of intermediate composition, iron-titanium-chromium oxides, and phosphate. These rocks also share minor element trends, reflected in their nickel-magnesium and chromium-magnesium ratios. Gusev basalts and shergottites appear to have formed from primitive magmas produced by melting an undepleted mantle at depth and erupted without significant fractionation. However, apparent differences between Gusev rocks and shergottites in their ages, plagioclase abundances, and volatile contents preclude direct correlation. Orbital determinations of global olivine distribution and compositions by thermal emission spectroscopy suggest that olivine-rich rocks may be widespread. Because weathering under acidic conditions preferentially attacks olivine and disguises such rocks beneath alteration rinds, picritic basalts formed from primitive magmas may even be a common component of the Martian crust formed during ancient and recent times.
    Schlagwort(e): Lunar and Planetary Science and Exploration
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  • 6
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    Asteroid-Meteorite Links: The Vesta Conundrum(s) (2006)
    In:  CASI
    Details
    Publikationsdatum: 2018-06-11
    Beschreibung: Although a direct link between the HED meteorites and the asteroid 4 Vesta is generally acknowledged, several issues continue to be actively examined that tie Vesta to early processes in the solar system. Vesta is no longer the only basaltic asteroid in the Main belt. In addition to the Vestoids of the Vesta family, the small asteroid Magnya is basaltic but appears to be unrelated to Vesta. Similarly, diversity now identified in the collection of basaltic meteorites requires more than one basaltic parent body, consistent with the abundance of differentiated parent bodies implied by iron meteorites. The timing of the formation of the Vestoids (and presumably the large crater at the south pole of Vesta) is unresolved. Peaks in Ar-Ar dates of eucrites suggest this impact event could be related to a possible late heavy bombardment at least 3.5 Gyr ago. On the other hand, the optically fresh appearance of both Vesta and the Vestoids requires either a relatively recent resurfacing event or that their surfaces do not weather in the same manner thought to occur on other asteroids such as the ordinary chondrite parent body. Diversity across the surface of Vesta has been observed with HST and there are hints of compositional variations (possibly involving minor olivine) in near-infrared spectra.
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: IAU
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  • 7
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    Elemental Compositions of Comet 81P/Wild 2 Samples Collected by Stardust (2006)
    In:  CASI
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    Publikationsdatum: 2018-06-11
    Beschreibung: We measured the chemical compositions of material from 23 particles in aerogel and residue in 7 craters in aluminum foil, collected during passage of the Stardust spacecraft through the coma of Comet 81P/Wild 2. These particles are chemically heterogeneous at the largest size-scale analyzed, ~180 nanograms. The mean chemical composition of this Wild 2 material agrees with the CI meteorite composition for the refractory elements Mg, Si, Cr, Fe, and Ni to 35%, and for Ca and Mn to 50%. The data suggest the moderately volatile elements Cu, Zn, and Ga may be enriched in this Wild 2 material.
    Schlagwort(e): Lunar and Planetary Science and Exploration
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  • 8
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    Titan Ion Composition at Magnetosphere-Ionosphere Transition Region (2006)
    In:  Other Sources
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    Publikationsdatum: 2019-07-19
    Beschreibung: Using Cassini Plasma Spectrometer (CAPS) Ion Mass Spectrometer (IMS) ion composition data, we will investigate the compositional changes at the transition region between Saturn's magnetospheric flow and Titan's upper ionosphere. It is this region where scavenging of Titan's upper ionosphere can occur, where it is then dragged away by the magnetospheric flow as cold plasma for Saturn's magnetosphere. This cold plasma may form plumes as originally proposed by (1) during the Voyager 1 epoch. This source of cold plasma may have a unique compositional signature such as methane group ions. Water group ions that are observed in Saturn's outer magnetosphere (2,3) are relatively hot and probably come from the inner magnetosphere where they are born from fast neutrals escaping Enceladus (4) and picked up in the outer magnetosphere as hot plasma (5). This scenario will be complicated by pickup methane ions within Titan's mass loading region, as originally predicted by (6) based on Voyager 1 data and observationally confirmed by (3,7) using CAPS IMS data. But, CH4(+) ions or their fragments can only be produced as pickup ions from Titan's exosphere which can extend beyond the transition region of concern here, while CH5(+) ions can be scavenged from Titan's ionosphere. We will investigate these possibilities.
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: 38th Annual Division of Planetary Sciences Meeting; Oct 09, 2006 - Oct 13, 2006; Pasadena, CA; United States
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  • 9
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    Is the tail of 73P-B/Schwassman-Wachman 1 chasing its Remnant Nucleus? (2006)
    In:  Other Sources
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    Publikationsdatum: 2019-07-19
    Beschreibung: We report on imaging observations of comets 73P-B/Schwassmann-Wachmann 1 and 73P-C/Schwassmann-Wachmann 1 at the IRTF with SpeX (J, K) and MRSI (10 micron narrow band filter set) on 2006 Apr 17-19 UT and 2006 Jun 18-19, and at the VLT with VISIR (1 0 micron narrow band filters, 20 micron) on 2006 Apr 17 UT. Compared to when the comet was in the midst of breaking up in mid-April, in June the tail of 73P-B is much fainter and there is a compact coma detected well separated and ahead of its tail, and fainter than the tail. The width of the tail in J, K, and 10 micron images indicates that the pieces that were shed in April must still be outgassing and releasing small particles into the tail-shaped coma; small grains have relatively short lifetimes in the coma due to radiation pressure. The trailing tail is now well separated from the faint "leader of the pack" compact coma that we suppose is a remaining piece of the nucleus. It will be interesting to see post-perihelion if this "leading compact coma" object continues to gain distance on the debris and continues to weakly outgas and shed small grains. One wonders if it expended its volatiles (available to the surface) in breaking up; a short-lived release of volatiles occurred in the Deep Impact event with comet 9P/Tempel 1. 73P-C is extended with a more elongated coma structure closer to perihelion compared to 2006 Apr 18- 19 UT. The SEDs from 2006 Apr and Jun from SpeX-MIRSI (IRTF) are compared with VISIR (VLT) SEDs from 2006 Apr. Information on the heliocentric dependence of the activity and dust release yields insights into the origin of activity and the relationship between activity and grain size distribution/mineralogy.
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: Europlanet 2006; Oct 18, 2006 - Oct 22, 2006; Lindau; Germany
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  • 10
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    Laboratory Measurements of Optical and Physical Properties of Individual Lunar Dust Grains (2006)
    In:  Other Sources
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    Publikationsdatum: 2019-07-18
    Beschreibung: The lunar surface is covered with a thick layer of sub-micron/micron size dust grains formed by meteoritic impact over billions of years. The fine dust grains are levitated and transported on the lunar surface, and transient dust clouds over the lunar horizon were observed by experiments during the Apollo 17 mission. Theoretical models suggest that the dust grains on the lunar surface are charged by the solar UV radiation as well as the solar wind. Even without any physical activity, the dust grains are levitated by electrostatic fields and transported away from the surface in the near vacuum environment of the Moon. The current dust charging and levitation models, however, do not fully explain the observed phenomena. Since the abundance of dust on the Moon's surface with its observed adhesive characteristics has the potential of severe impact on human habitat and operations and lifetime of a variety of equipment, it is necessary to investigate the charging properties and the lunar dust phenomena in order to develop appropriate mitigating strategies. Photoelectric emission induced by the solar UV radiation with photon energies higher than the work function of the grain materials is recognized to be the dominant process for charging of the lunar dust, and requires measurements of the photoelectric yields to determine the charging and equilibrium potentials of individual dust grains. In this paper, we present the first laboratory measurements of the photoelectric yields of individual sub-micron/micron size dust grains selected from sample returns of Apollo 17, and Luna 24 missions, as well as similar size dust grains from the JSC-1 simulants. The experimental results were obtained on a laboratory facility based on an electrodynamic balance that permits a variety of experiments to be conducted on individual sub-micron/micron size dust grains in simulated space environments. The photoelectric emission measurements indicate grain size dependence with the yield increasing by an order of magnitude for grains of radii sub-micron size to several micron radii, at which it reaches asymptotic values. The yield for large size grains is found to be more than an order of magnitude higher than the bulk measurements on lunar fines reported in the literature.
    Schlagwort(e): Lunar and Planetary Science and Exploration
    Materialart: 36th COSPAR Scientific Assembly; Jul 16, 2006 - Jul 23, 2006; Beijing; China
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