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  • Articles  (48)
  • Springer Nature  (20)
  • Oxford University Press  (13)
  • Nature Publishing Group (NPG)  (10)
  • American Geophysical Union  (5)
  • 2010-2014  (35)
  • 1975-1979  (13)
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  • Articles  (48)
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  • 1
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    Lactate, a product of glycolytic metabolism, inhibits histone deacetylase activity and promotes changes in gene expression (2012)
    Oxford University Press
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    Publication Date: 2012-06-06
    Description: Chemical inhibitors of histone deacetylase (HDAC) activity are used as experimental tools to induce histone hyperacetylation and deregulate gene transcription, but it is not known whether the inhibition of HDACs plays any part in the normal physiological regulation of transcription. Using both in vitro and in vivo assays, we show that lactate, which accumulates when glycolysis exceeds the cell’s aerobic metabolic capacity, is an endogenous HDAC inhibitor, deregulating transcription in an HDAC-dependent manner. Lactate is a relatively weak inhibitor (IC 50 40 mM) compared to the established inhibitors trichostatin A and butyrate, but the genes deregulated overlap significantly with those affected by low concentrations of the more potent inhibitors. HDAC inhibition causes significant up and downregulation of genes, but genes that are associated with HDAC proteins are more likely to be upregulated and less likely to be downregulated than would be expected. Our results suggest that the primary effect of HDAC inhibition by endogenous short-chain fatty acids like lactate is to promote gene expression at genes associated with HDAC proteins. Therefore, we propose that lactate may be an important transcriptional regulator, linking the metabolic state of the cell to gene transcription.
    Print ISSN: 0305-1048
    Electronic ISSN: 1362-4962
    Topics: Biology
    Published by Oxford University Press
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  • 2
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    Stellar rotational periods in the planet hosting open cluster Praesepe (2014)
    Oxford University Press
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    Publication Date: 2014-06-20
    Description: By using the dense coverage of the extrasolar planet survey project HATNet (Hungarian-made Automated Telescope Network), we Fourier analyse 381 high-probability members of the nearby open cluster Praesepe (Beehive/M44/NGC 2632). In addition to the detection of 10 variables (of Scuti and other types), we identify 180 rotational variables (including the two known planet hosts). This sample increases the number of known rotational variables in this cluster for spectral classes earlier than M by more than a factor of 3. These stars closely follow a colour/magnitude–period relation from early F to late K stars. We approximate this relation by polynomials for an easier reference to the rotational characteristics in different colours. The total (peak-to-peak) amplitudes of the large majority (94 per cent) of these variables span the range of 0.005–0.04 mag. The periods cover a range from 2.5 to 15 d. These data strongly confirm that Praesepe and the Hyades have the same gyrochronological ages. Regarding the two planet hosts, Pr0211 (the one with the shorter orbital period) has a rotational period that is ~2 d shorter than the one expected from the main rotational pattern in this cluster. This, together with other examples discussed in the paper, may hint that star–planet interaction via tidal dissipation can be significant in some cases in the rotational evolution of stars hosting hot Jupiters.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 3
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    Sensitivity to perturbations in vivo implies high noise and suggests rate coding in cortex (2010)
    Nature Publishing Group (NPG)
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    Publication Date: 2010-07-03
    Description: It is well known that neural activity exhibits variability, in the sense that identical sensory stimuli produce different responses, but it has been difficult to determine what this variability means. Is it noise, or does it carry important information-about, for example, the internal state of the organism? Here we address this issue from the bottom up, by asking whether small perturbations to activity in cortical networks are amplified. Based on in vivo whole-cell patch-clamp recordings in rat barrel cortex, we find that a perturbation consisting of a single extra spike in one neuron produces approximately 28 additional spikes in its postsynaptic targets. We also show, using simultaneous intra- and extracellular recordings, that a single spike in a neuron produces a detectable increase in firing rate in the local network. Theoretical analysis indicates that this amplification leads to intrinsic, stimulus-independent variations in membrane potential of the order of +/-2.2-4.5 mV-variations that are pure noise, and so carry no information at all. Therefore, for the brain to perform reliable computations, it must either use a rate code, or generate very large, fast depolarizing events, such as those proposed by the theory of synfire chains. However, in our in vivo recordings, we found that such events were very rare. Our findings are thus consistent with the idea that cortex is likely to use primarily a rate code.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC2898896/" 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/PMC2898896/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉London, Michael -- Roth, Arnd -- Beeren, Lisa -- Hausser, Michael -- Latham, Peter E -- G0500244/Medical Research Council/United Kingdom -- R01 MH062447-08/MH/NIMH NIH HHS/ -- R01 MH62447/MH/NIMH NIH HHS/ -- Medical Research Council/United Kingdom -- Wellcome Trust/United Kingdom -- England -- Nature. 2010 Jul 1;466(7302):123-7. doi: 10.1038/nature09086.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Wolfson Institute for Biomedical Research and Department of Neuroscience, Physiology and Pharmacology, University College London, Gower Street, London WC1E 6BT, UK.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20596024" target="_blank"〉PubMed〈/a〉
    Keywords: Action Potentials/physiology ; Animals ; Artifacts ; Cerebral Cortex/cytology/*physiology ; *Models, Neurological ; Neurons/metabolism ; Patch-Clamp Techniques ; Probability ; Rats ; Rats, Sprague-Dawley ; Stochastic Processes
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 4
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    Two Earth-sized planets orbiting Kepler-20 (2011)
    Nature Publishing Group (NPG)
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    Publication Date: 2011-12-22
    Description: Since the discovery of the first extrasolar giant planets around Sun-like stars, evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered has a radius 1.42 times that of the Earth's radius (R( plus sign in circle)), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03R( plus sign in circle)) and the other smaller than the Earth (0.87R( plus sign in circle)), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets. The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Fressin, Francois -- Torres, Guillermo -- Rowe, Jason F -- Charbonneau, David -- Rogers, Leslie A -- Ballard, Sarah -- Batalha, Natalie M -- Borucki, William J -- Bryson, Stephen T -- Buchhave, Lars A -- Ciardi, David R -- Desert, Jean-Michel -- Dressing, Courtney D -- Fabrycky, Daniel C -- Ford, Eric B -- Gautier, Thomas N 3rd -- Henze, Christopher E -- Holman, Matthew J -- Howard, Andrew -- Howell, Steve B -- Jenkins, Jon M -- Koch, David G -- Latham, David W -- Lissauer, Jack J -- Marcy, Geoffrey W -- Quinn, Samuel N -- Ragozzine, Darin -- Sasselov, Dimitar D -- Seager, Sara -- Barclay, Thomas -- Mullally, Fergal -- Seader, Shawn E -- Still, Martin -- Twicken, Joseph D -- Thompson, Susan E -- Uddin, Kamal -- England -- Nature. 2011 Dec 20;482(7384):195-8. doi: 10.1038/nature10780.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA. ffressin@cfa.harvard.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22186831" 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
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    An abundance of small exoplanets around stars with a wide range of metallicities (2012)
    Nature Publishing Group (NPG)
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    Publication Date: 2012-06-23
    Description: The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a 'fossil' record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets, supporting the model that planets form by accumulation of dust and ice particles. Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets. However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission, including objects that are comparable in size to the terrestrial planets in the Solar System. We find that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. This observation suggests that terrestrial planets may be widespread in the disk of the Galaxy, with no special requirement of enhanced metallicity for their formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Buchhave, Lars A -- Latham, David W -- Johansen, Anders -- Bizzarro, Martin -- Torres, Guillermo -- Rowe, Jason F -- Batalha, Natalie M -- Borucki, William J -- Brugamyer, Erik -- Caldwell, Caroline -- Bryson, Stephen T -- Ciardi, David R -- Cochran, William D -- Endl, Michael -- Esquerdo, Gilbert A -- Ford, Eric B -- Geary, John C -- Gilliland, Ronald L -- Hansen, Terese -- Isaacson, Howard -- Laird, John B -- Lucas, Philip W -- Marcy, Geoffrey W -- Morse, Jon A -- Robertson, Paul -- Shporer, Avi -- Stefanik, Robert P -- Still, Martin -- Quinn, Samuel N -- England -- Nature. 2012 Jun 13;486(7403):375-7. doi: 10.1038/nature11121.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark. buchhave@astro.ku.dk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22722196" 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
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    A sub-Mercury-sized exoplanet (2013)
    Nature Publishing Group (NPG)
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    Publication Date: 2013-02-22
    Description: Since the discovery of the first exoplanets, it has been known that other planetary systems can look quite unlike our own. Until fairly recently, we have been able to probe only the upper range of the planet size distribution, and, since last year, to detect planets that are the size of Earth or somewhat smaller. Hitherto, no planets have been found that are smaller than those we see in the Solar System. Here we report a planet significantly smaller than Mercury. This tiny planet is the innermost of three that orbit the Sun-like host star, which we have designated Kepler-37. Owing to its extremely small size, similar to that of the Moon, and highly irradiated surface, the planet, Kepler-37b, is probably rocky with no atmosphere or water, similar to Mercury.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Barclay, Thomas -- Rowe, Jason F -- Lissauer, Jack J -- Huber, Daniel -- Fressin, Francois -- Howell, Steve B -- Bryson, Stephen T -- Chaplin, William J -- Desert, Jean-Michel -- Lopez, Eric D -- Marcy, Geoffrey W -- Mullally, Fergal -- Ragozzine, Darin -- Torres, Guillermo -- Adams, Elisabeth R -- Agol, Eric -- Barrado, David -- Basu, Sarbani -- Bedding, Timothy R -- Buchhave, Lars A -- Charbonneau, David -- Christiansen, Jessie L -- Christensen-Dalsgaard, Jorgen -- Ciardi, David -- Cochran, William D -- Dupree, Andrea K -- Elsworth, Yvonne -- Everett, Mark -- Fischer, Debra A -- Ford, Eric B -- Fortney, Jonathan J -- Geary, John C -- Haas, Michael R -- Handberg, Rasmus -- Hekker, Saskia -- Henze, Christopher E -- Horch, Elliott -- Howard, Andrew W -- Hunter, Roger C -- Isaacson, Howard -- Jenkins, Jon M -- Karoff, Christoffer -- Kawaler, Steven D -- Kjeldsen, Hans -- Klaus, Todd C -- Latham, David W -- Li, Jie -- Lillo-Box, Jorge -- Lund, Mikkel N -- Lundkvist, Mia -- Metcalfe, Travis S -- Miglio, Andrea -- Morris, Robert L -- Quintana, Elisa V -- Stello, Dennis -- Smith, Jeffrey C -- Still, Martin -- Thompson, Susan E -- England -- Nature. 2013 Feb 28;494(7438):452-4. doi: 10.1038/nature11914. Epub 2013 Feb 20.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, California 94035, USA. thomas.barclay@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23426260" 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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  • 7
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    Transiting circumbinary planets Kepler-34 b and Kepler-35 b (2012)
    Nature Publishing Group (NPG)
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    Publication Date: 2012-01-13
    Description: Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars (binaries). Although long anticipated, the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than approximately 1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Welsh, William F -- Orosz, Jerome A -- Carter, Joshua A -- Fabrycky, Daniel C -- Ford, Eric B -- Lissauer, Jack J -- Prsa, Andrej -- Quinn, Samuel N -- Ragozzine, Darin -- Short, Donald R -- Torres, Guillermo -- Winn, Joshua N -- Doyle, Laurance R -- Barclay, Thomas -- Batalha, Natalie -- Bloemen, Steven -- Brugamyer, Erik -- Buchhave, Lars A -- Caldwell, Caroline -- Caldwell, Douglas A -- Christiansen, Jessie L -- Ciardi, David R -- Cochran, William D -- Endl, Michael -- Fortney, Jonathan J -- Gautier, Thomas N 3rd -- Gilliland, Ronald L -- Haas, Michael R -- Hall, Jennifer R -- Holman, Matthew J -- Howard, Andrew W -- Howell, Steve B -- Isaacson, Howard -- Jenkins, Jon M -- Klaus, Todd C -- Latham, David W -- Li, Jie -- Marcy, Geoffrey W -- Mazeh, Tsevi -- Quintana, Elisa V -- Robertson, Paul -- Shporer, Avi -- Steffen, Jason H -- Windmiller, Gur -- Koch, David G -- Borucki, William J -- England -- Nature. 2012 Jan 11;481(7382):475-9. doi: 10.1038/nature10768.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, California 92182, USA. wfw@sciences.sdsu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22237021" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment/chemistry ; *Planets ; Space Flight ; Spacecraft ; Stars, Celestial
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 8
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    Three regimes of extrasolar planet radius inferred from host star metallicities (2014)
    Nature Publishing Group (NPG)
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    Publication Date: 2014-05-30
    Description: Approximately half of the extrasolar planets (exoplanets) with radii less than four Earth radii are in orbits with short periods. Despite their sheer abundance, the compositions of such planets are largely unknown. The available evidence suggests that they range in composition from small, high-density rocky planets to low-density planets consisting of rocky cores surrounded by thick hydrogen and helium gas envelopes. Here we report the metallicities (that is, the abundances of elements heavier than hydrogen and helium) of more than 400 stars hosting 600 exoplanet candidates, and find that the exoplanets can be categorized into three populations defined by statistically distinct ( approximately 4.5sigma) metallicity regions. We interpret these regions as reflecting the formation regimes of terrestrial-like planets (radii less than 1.7 Earth radii), gas dwarf planets with rocky cores and hydrogen-helium envelopes (radii between 1.7 and 3.9 Earth radii) and ice or gas giant planets (radii greater than 3.9 Earth radii). These transitions correspond well with those inferred from dynamical mass estimates, implying that host star metallicity, which is a proxy for the initial solids inventory of the protoplanetary disk, is a key ingredient regulating the structure of planetary systems.〈br /〉〈br /〉〈a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC4048851/" 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/PMC4048851/" target="_blank"〉This paper as free author manuscript - peer-reviewed and accepted for publication〈/a〉〈br /〉〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Buchhave, Lars A -- Bizzarro, Martin -- Latham, David W -- Sasselov, Dimitar -- Cochran, William D -- Endl, Michael -- Isaacson, Howard -- Juncher, Diana -- Marcy, Geoffrey W -- 616027/European Research Council/International -- England -- Nature. 2014 May 29;509(7502):593-5. doi: 10.1038/nature13254.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉1] Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA [2] Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark. ; Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark. ; Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA. ; McDonald Observatory, The University of Texas, Austin, Texas 78712, USA. ; University of California, Berkeley, California 94720, USA. ; 1] Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, DK-1350 Copenhagen, Denmark [2] Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24870544" 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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  • 9
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    A closely packed system of low-mass, low-density planets transiting Kepler-11 (2011)
    Nature Publishing Group (NPG)
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    Publication Date: 2011-02-05
    Description: When an extrasolar planet passes in front of (transits) its star, its radius can be measured from the decrease in starlight and its orbital period from the time between transits. Multiple planets transiting the same star reveal much more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets observed as multiples has implications for the planarity of planetary systems. But few stars have more than one known transiting planet, and none has more than three. Here we report Kepler spacecraft observations of a single Sun-like star, which we call Kepler-11, that reveal six transiting planets, five with orbital periods between 10 and 47 days and a sixth planet with a longer period. The five inner planets are among the smallest for which mass and size have both been measured, and these measurements imply substantial envelopes of light gases. The degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end of planet formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Lissauer, Jack J -- Fabrycky, Daniel C -- Ford, Eric B -- Borucki, William J -- Fressin, Francois -- Marcy, Geoffrey W -- Orosz, Jerome A -- Rowe, Jason F -- Torres, Guillermo -- Welsh, William F -- Batalha, Natalie M -- Bryson, Stephen T -- Buchhave, Lars A -- Caldwell, Douglas A -- Carter, Joshua A -- Charbonneau, David -- Christiansen, Jessie L -- Cochran, William D -- Desert, Jean-Michel -- Dunham, Edward W -- Fanelli, Michael N -- Fortney, Jonathan J -- Gautier, Thomas N 3rd -- Geary, John C -- Gilliland, Ronald L -- Haas, Michael R -- Hall, Jennifer R -- Holman, Matthew J -- Koch, David G -- Latham, David W -- Lopez, Eric -- McCauliff, Sean -- Miller, Neil -- Morehead, Robert C -- Quintana, Elisa V -- Ragozzine, Darin -- Sasselov, Dimitar -- Short, Donald R -- Steffen, Jason H -- England -- Nature. 2011 Feb 3;470(7332):53-8. doi: 10.1038/nature09760.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Ames Research Center, Moffett Field, California 94035, USA. jack.lissauer@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21293371" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
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    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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  • 10
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    An Earth-sized planet with an Earth-like density (2013)
    Nature Publishing Group (NPG)
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    Publication Date: 2013-11-01
    Description: Recent analyses of data from the NASA Kepler spacecraft have established that planets with radii within 25 per cent of the Earth's (R Earth symbol) are commonplace throughout the Galaxy, orbiting at least 16.5 per cent of Sun-like stars. Because these studies were sensitive to the sizes of the planets but not their masses, the question remains whether these Earth-sized planets are indeed similar to the Earth in bulk composition. The smallest planets for which masses have been accurately determined are Kepler-10b (1.42 R Earth symbol) and Kepler-36b (1.49 R Earth symbol), which are both significantly larger than the Earth. Recently, the planet Kepler-78b was discovered and found to have a radius of only 1.16 R Earth symbol. Here we report that the mass of this planet is 1.86 Earth masses. The resulting mean density of the planet is 5.57 g cm(-3), which is similar to that of the Earth and implies a composition of iron and rock.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Pepe, Francesco -- Cameron, Andrew Collier -- Latham, David W -- Molinari, Emilio -- Udry, Stephane -- Bonomo, Aldo S -- Buchhave, Lars A -- Charbonneau, David -- Cosentino, Rosario -- Dressing, Courtney D -- Dumusque, Xavier -- Figueira, Pedro -- Fiorenzano, Aldo F M -- Gettel, Sara -- Harutyunyan, Avet -- Haywood, Raphaelle D -- Horne, Keith -- Lopez-Morales, Mercedes -- Lovis, Christophe -- Malavolta, Luca -- Mayor, Michel -- Micela, Giusi -- Motalebi, Fatemeh -- Nascimbeni, Valerio -- Phillips, David -- Piotto, Giampaolo -- Pollacco, Don -- Queloz, Didier -- Rice, Ken -- Sasselov, Dimitar -- Segransan, Damien -- Sozzetti, Alessandro -- Szentgyorgyi, Andrew -- Watson, Christopher A -- England -- Nature. 2013 Nov 21;503(7476):377-80. doi: 10.1038/nature12768. Epub 2013 Oct 30.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Observatoire Astronomique de l'Universite de Geneve, 51 chemin des Maillettes, 1290 Versoix, Switzerland.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24172902" target="_blank"〉PubMed〈/a〉
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    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
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