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  • 1
    Publication Date: 2019
    Description: Abstract Gas hydrates can form more or less at the same time as seafloor sediment. They can have the effect of significantly stiffening and strengthening deep‐ocean sediments. Subsequent increases in situ temperature or decreases in pressure may trigger hydrate dissociation, leading to large reductions in the strength and stiffness of the sediment and possible seafloor instability. Gas hydrate dissociation not only removes cementing. It also releases freshwater and significant amounts of trapped gas that are dependent on multiple factors such as type of sediment, available pore space, hydrate morphology, and hydrate saturation. The presence of pock marks in areas of known seabed instability suggests that hydrate dissociation may have been a factor in triggering failure at these locations. Having reviewed the mechanisms by which the strength and stiffness of seabed sediment may be changed during dissociation, this paper reports the results of laboratory testing to evaluate the effects of loss of hydrate cement on strength and stiffness, for a range of sand‐sized materials with differing particle size, specific surface area, and particle shape, using a laboratory gas hydrate triaxial apparatus. The results suggest that both the strength and the stiffness of hydrate‐cemented granular materials are affected significantly by the specific surface available for hydrate cementation and, to a certain extent, by the particle shape. Uniform coarse granular sediments of lower specific surface area can suffer significant loss of stiffness and strength upon hydrate dissociation, changing the sediment from dilative to contractive. Finer‐grained sediments appear less affected by dissociation.
    Print ISSN: 2169-9313
    Electronic ISSN: 2169-9356
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
    Publication Date: 2012-05-26
    Description: Metabolic reprogramming has been proposed to be a hallmark of cancer, yet a systematic characterization of the metabolic pathways active in transformed cells is currently lacking. Using mass spectrometry, we measured the consumption and release (CORE) profiles of 219 metabolites from media across the NCI-60 cancer cell lines, and integrated these data with a preexisting atlas of gene expression. This analysis identified glycine consumption and expression of the mitochondrial glycine biosynthetic pathway as strongly correlated with rates of proliferation across cancer cells. Antagonizing glycine uptake and its mitochondrial biosynthesis preferentially impaired rapidly proliferating cells. Moreover, higher expression of this pathway was associated with greater mortality in breast cancer patients. Increased reliance on glycine may represent a metabolic vulnerability for selectively targeting rapid cancer cell proliferation.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC3526189/" 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/PMC3526189/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Jain, Mohit -- Nilsson, Roland -- Sharma, Sonia -- Madhusudhan, Nikhil -- Kitami, Toshimori -- Souza, Amanda L -- Kafri, Ran -- Kirschner, Marc W -- Clish, Clary B -- Mootha, Vamsi K -- K08 HL107451/HL/NHLBI NIH HHS/ -- K08HL107451/HL/NHLBI NIH HHS/ -- R01 DK081457/DK/NIDDK NIH HHS/ -- R01 GM026875/GM/NIGMS NIH HHS/ -- R01DK081457/DK/NIDDK NIH HHS/ -- New York, N.Y. -- Science. 2012 May 25;336(6084):1040-4. doi: 10.1126/science.1218595.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Broad Institute, Cambridge, MA 02142, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22628656" target="_blank"〉PubMed〈/a〉
    Keywords: Breast Neoplasms/genetics/metabolism/pathology ; Cell Cycle ; Cell Line ; Cell Line, Tumor ; *Cell Proliferation ; Cell Transformation, Neoplastic ; Chromatography, Liquid ; Culture Media ; Gene Expression ; Gene Expression Profiling ; Glycine/biosynthesis/*metabolism ; Humans ; Metabolic Networks and Pathways/genetics ; Metabolome ; Mitochondria/enzymology/metabolism ; Neoplasms/genetics/*metabolism/*pathology ; Purines/biosynthesis ; Tandem Mass Spectrometry
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 3
    Publication Date: 2010-12-15
    Description: The carbon-to-oxygen ratio (C/O) in a planet provides critical information about its primordial origins and subsequent evolution. A primordial C/O greater than 0.8 causes a carbide-dominated interior, as opposed to the silicate-dominated composition found on Earth; the atmosphere can also differ from those in the Solar System. The solar C/O is 0.54 (ref. 3). Here we report an analysis of dayside multi-wavelength photometry of the transiting hot-Jupiter WASP-12b (ref. 6) that reveals C/O 〉/= 1 in its atmosphere. The atmosphere is abundant in CO. It is depleted in water vapour and enhanced in methane, each by more than two orders of magnitude compared to a solar-abundance chemical-equilibrium model at the expected temperatures. We also find that the extremely irradiated atmosphere (T 〉 2,500 K) of WASP-12b lacks a prominent thermal inversion (or stratosphere) and has very efficient day-night energy circulation. The absence of a strong thermal inversion is in stark contrast to theoretical predictions for the most highly irradiated hot-Jupiter atmospheres.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Madhusudhan, Nikku -- Harrington, Joseph -- Stevenson, Kevin B -- Nymeyer, Sarah -- Campo, Christopher J -- Wheatley, Peter J -- Deming, Drake -- Blecic, Jasmina -- Hardy, Ryan A -- Lust, Nate B -- Anderson, David R -- Collier-Cameron, Andrew -- Britt, Christopher B T -- Bowman, William C -- Hebb, Leslie -- Hellier, Coel -- Maxted, Pierre F L -- Pollacco, Don -- West, Richard G -- England -- Nature. 2011 Jan 6;469(7328):64-7. doi: 10.1038/nature09602. Epub 2010 Dec 8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA. nmadhu@mit.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21150901" 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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  • 4
    Publication Date: 2010-04-24
    Description: The nearby extrasolar planet GJ 436b-which has been labelled as a 'hot Neptune'-reveals itself by the dimming of light as it crosses in front of and behind its parent star as seen from Earth. Respectively known as the primary transit and secondary eclipse, the former constrains the planet's radius and mass, and the latter constrains the planet's temperature and, with measurements at multiple wavelengths, its atmospheric composition. Previous work using transmission spectroscopy failed to detect the 1.4-mum water vapour band, leaving the planet's atmospheric composition poorly constrained. Here we report the detection of planetary thermal emission from the dayside of GJ 436b at multiple infrared wavelengths during the secondary eclipse. The best-fit compositional models contain a high CO abundance and a substantial methane (CH(4)) deficiency relative to thermochemical equilibrium models for the predicted hydrogen-dominated atmosphere. Moreover, we report the presence of some H(2)O and traces of CO(2). Because CH(4) is expected to be the dominant carbon-bearing species, disequilibrium processes such as vertical mixing and polymerization of methane into substances such as ethylene may be required to explain the hot Neptune's small CH(4)-to-CO ratio, which is at least 10(5) times smaller than predicted.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stevenson, Kevin B -- Harrington, Joseph -- Nymeyer, Sarah -- Madhusudhan, Nikku -- Seager, Sara -- Bowman, William C -- Hardy, Ryan A -- Deming, Drake -- Rauscher, Emily -- Lust, Nate B -- England -- Nature. 2010 Apr 22;464(7292):1161-4. doi: 10.1038/nature09013.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Planetary Sciences Group, Department of Physics, University of Central Florida, Orlando, Florida 32816, USA. kevin218@knights.ucf.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20414304" 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: 2014-09-26
    Description: Transmission spectroscopy has so far detected atomic and molecular absorption in Jupiter-sized exoplanets, but intense efforts to measure molecular absorption in the atmospheres of smaller (Neptune-sized) planets during transits have revealed only featureless spectra. From this it was concluded that the majority of small, warm planets evolve to sustain atmospheres with high mean molecular weights (little hydrogen), opaque clouds or scattering hazes, reducing our ability to observe the composition of these atmospheres. Here we report observations of the transmission spectrum of the exoplanet HAT-P-11b (which has a radius about four times that of Earth) from the optical wavelength range to the infrared. We detected water vapour absorption at a wavelength of 1.4 micrometres. The amplitude of the water absorption (approximately 250 parts per million) indicates that the planetary atmosphere is predominantly clear down to an altitude corresponding to about 1 millibar, and sufficiently rich in hydrogen to have a large scale height (over which the atmospheric pressure varies by a factor of e). The spectrum is indicative of a planetary atmosphere in which the abundance of heavy elements is no greater than about 700 times the solar value. This is in good agreement with the core-accretion theory of planet formation, in which a gas giant planet acquires its atmosphere by accreting hydrogen-rich gas directly from the protoplanetary nebula onto a large rocky or icy core.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fraine, Jonathan -- Deming, Drake -- Benneke, Bjorn -- Knutson, Heather -- Jordan, Andres -- Espinoza, Nestor -- Madhusudhan, Nikku -- Wilkins, Ashlee -- Todorov, Kamen -- England -- Nature. 2014 Sep 25;513(7519):526-9. doi: 10.1038/nature13785.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉1] Department of Astronomy, University of Maryland, College Park, Maryland 20742-2421, USA [2] Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, 7820436 Macul, Santiago, Chile [3] Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA. ; 1] Department of Astronomy, University of Maryland, College Park, Maryland 20742-2421, USA [2] NASA Astrobiology Institute's Virtual Planetary Laboratory, Seattle, Washington 98195, USA. ; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA. ; Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, 7820436 Macul, Santiago, Chile. ; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. ; Department of Astronomy, University of Maryland, College Park, Maryland 20742-2421, USA. ; Department of Physics, ETH Zurich, 8049 Zurich, Switzerland.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25254473" 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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  • 6
    Publication Date: 2014-10-11
    Description: Exoplanets that orbit close to their host stars are much more highly irradiated than their solar system counterparts. Understanding the thermal structures and appearances of these planets requires investigating how their atmospheres respond to such extreme stellar forcing. We present spectroscopic thermal emission measurements as a function of orbital phase ("phase-curve observations") for the highly irradiated exoplanet WASP-43b spanning three full planet rotations using the Hubble Space Telescope. With these data, we construct a map of the planet's atmospheric thermal structure, from which we find large day-night temperature variations at all measured altitudes and a monotonically decreasing temperature with pressure at all longitudes. We also derive a Bond albedo of 0.18(-0.12)(+0.07) and an altitude dependence in the hot-spot offset relative to the substellar point.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stevenson, Kevin B -- Desert, Jean-Michel -- Line, Michael R -- Bean, Jacob L -- Fortney, Jonathan J -- Showman, Adam P -- Kataria, Tiffany -- Kreidberg, Laura -- McCullough, Peter R -- Henry, Gregory W -- Charbonneau, David -- Burrows, Adam -- Seager, Sara -- Madhusudhan, Nikku -- Williamson, Michael H -- Homeier, Derek -- New York, N.Y. -- Science. 2014 Nov 14;346(6211):838-41. doi: 10.1126/science.1256758. Epub 2014 Oct 9.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA. NASA Sagan Fellow. kbs@uchicago.edu. ; CASA, Department of Astrophysical and Planetary Sciences, University of Colorado, 389-UCB, Boulder, CO 80309, USA. ; Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA. ; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA. ; Department of Planetary Sciences and Lunar and Planetary Laboratory, The University of Arizona, Tucson, AZ 85721, USA. ; Space Telescope Science Institute, Baltimore, MD 21218, USA. Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA. ; Center for Excellence in Information Systems, Tennessee State University, Nashville, TN 37209, USA. ; Department of Astronomy, Harvard University, Cambridge, MA 02138, USA. ; Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA. ; Department of Earth, Atmospheric, and Planetary Sciences, Department of Physics, Massachusetts Institute of Technology, 54-1718, 77 Massachusetts Avenue, Cambridge, MA 02139, USA. ; Institute of Astronomy, University of Cambridge, Cambridge CB3 OHA, UK. ; Centre de Recherche Astrophysique de Lyon, UMR 5574, CNRS, Universite de Lyon, Ecole Normale Superieure de Lyon, 46 Allee d'Italie, F-69364 Lyon Cedex 07, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25301972" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 7
    Publication Date: 2016-03-31
    Description: Over the past decade, observations of giant exoplanets (Jupiter-size) have provided key insights into their atmospheres, but the properties of lower-mass exoplanets (sub-Neptune) remain largely unconstrained because of the challenges of observing small planets. Numerous efforts to observe the spectra of super-Earths--exoplanets with masses of one to ten times that of Earth--have so far revealed only featureless spectra. Here we report a longitudinal thermal brightness map of the nearby transiting super-Earth 55 Cancri e (refs 4, 5) revealing highly asymmetric dayside thermal emission and a strong day-night temperature contrast. Dedicated space-based monitoring of the planet in the infrared revealed a modulation of the thermal flux as 55 Cancri e revolves around its star in a tidally locked configuration. These observations reveal a hot spot that is located 41 +/- 12 degrees east of the substellar point (the point at which incident light from the star is perpendicular to the surface of the planet). From the orbital phase curve, we also constrain the nightside brightness temperature of the planet to 1,380 +/- 400 kelvin and the temperature of the warmest hemisphere (centred on the hot spot) to be about 1,300 kelvin hotter (2,700 +/- 270 kelvin) at a wavelength of 4.5 micrometres, which indicates inefficient heat redistribution from the dayside to the nightside. Our observations are consistent with either an optically thick atmosphere with heat recirculation confined to the planetary dayside, or a planet devoid of atmosphere with low-viscosity magma flows at the surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Demory, Brice-Olivier -- Gillon, Michael -- de Wit, Julien -- Madhusudhan, Nikku -- Bolmont, Emeline -- Heng, Kevin -- Kataria, Tiffany -- Lewis, Nikole -- Hu, Renyu -- Krick, Jessica -- Stamenkovic, Vlada -- Benneke, Bjorn -- Kane, Stephen -- Queloz, Didier -- England -- Nature. 2016 Apr 14;532(7598):207-9. doi: 10.1038/nature17169. Epub 2016 Mar 30.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astrophysics Group, Cavendish Laboratory, JJ Thomson Avenue, Cambridge CB3 0HE, UK. ; Institut d'Astrophysique et de Geophysique, Universite of Liege, allee du 6 Aout 17, 4000 Liege, Belgium. ; Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139, USA. ; Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK. ; NaXys, Department of Mathematics, University of Namur, 8 Rempart de la Vierge, 5000 Namur, Belgium. ; University of Bern, Center for Space and Habitability, Sidlerstrasse 5, CH-3012, Bern, Switzerland. ; Astrophysics Group, School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL, UK. ; Space Telescope Science Institute, Baltimore, Maryland 21218, USA. ; Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA. ; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA. ; Spitzer Science Center, MS 220-6, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, California 91125, USA. ; Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Avenue, San Francisco, California 94132, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/27027283" 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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  • 8
    Publication Date: 2016-11-01
    Description: Homologous DNA recombination (HR) by the RAD51 recombinase enables error-free DNA break repair. To execute HR, RAD51 first forms a presynaptic filament on single-stranded (ss) DNA, which catalyses pairing with homologous double-stranded (ds) DNA. Here, we report a structure for the presynaptic human RAD51 filament at 3.5–5.0Å resolution using electron cryo-microscopy. RAD51 encases ssDNA in a helical filament of 103Å pitch, comprising 6.4 protomers per turn, with a rise of 16.1Å and a twist of 56.2°. Inter-protomer distance correlates with rotation of an α-helical region in the core catalytic domain that is juxtaposed to ssDNA, suggesting how the RAD51–DNA interaction modulates protomer spacing and filament pitch. We map Fanconi anaemia-like disease-associated RAD51 mutations, clarifying potential phenotypes. We predict binding sites on the presynaptic filament for two modules present in each BRC repeat of the BRCA2 tumour suppressor, a critical HR mediator. Structural modelling suggests that changes in filament pitch mask or expose one binding site with filament-inhibitory potential, rationalizing the paradoxical ability of the BRC repeats to either stabilize or inhibit filament formation at different steps during HR. Collectively, our findings provide fresh insight into the structural mechanism of HR and its dysregulation in human disease.
    Print ISSN: 0305-1048
    Electronic ISSN: 1362-4962
    Topics: Biology
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  • 9
    Publication Date: 2020-06-28
    Print ISSN: 0021-8979
    Electronic ISSN: 1089-7550
    Topics: Physics
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  • 10
    Publication Date: 2015-11-21
    Description: Considerable progress has been made in recent years in observations of atmospheric signatures of giant exoplanets, but processes in rocky exoplanets remain largely unknown due to major challenges in observing small planets. Numerous efforts to observe spectra of super-Earths, exoplanets with masses of 1–10 Earth masses, have thus far revealed only featureless spectra. In this paper, we report a 4 detection of variability in the dayside thermal emission from the transiting super-Earth 55 Cancri e. Dedicated space-based monitoring of the planet in the mid-infrared over eight eclipses revealed the thermal emission from its dayside atmosphere varying by a factor of 3.7 between 2012 and 2013. The amplitude and trend of the variability are not explained by potential influence of star spots or by local thermal or compositional changes in the atmosphere over the short span of the observations. The possibility of large-scale surface activity due to strong tidal interactions possibly similar to Io, or the presence of circumstellar/circumplanetary material appear plausible and motivate future long-term monitoring of the planet.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
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