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  • 1
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    The early evolution of the inner solar system: a meteoritic perspective (2001)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2001-07-07
    Description: Formation of the solar system may have been triggered by a stellar wind. From then on, the solar system would have followed a conventional evolutionary path, including the formation of a disk and bipolar jets. The now extinct short-lived radionuclides beryllium-10 and, possibly, manganese-53 that were present in meteorites probably resulted from energetic particle irradiation within the solar system. Calcium-aluminum-rich inclusions (the oldest known solar system solids) and chondrules could have been produced by the bipolar jets, but it is more likely that they formed during localized events in the asteroid belt. The chondritic meteorites formed within the temperature range (100 to 400 kelvin) inferred for the midplane of classical T Tauri disks at 2 to 3 astronomical units from their central stars. However, these meteorites may retain a chemical memory of earlier times when midplane temperatures were much higher. Dissipation of the solar nebula occurred within a few million years of solar system formation, whereas differentiation of asteroidal-sized bodies occurred within 5 to 15 million years. The terrestrial planets took approximately 100 million years to form. Consequently, they would have accreted already differentiated bodies, and their final assembly was not completed until after the solar nebula had dispersed. This implies that water-bearing asteroids and/or icy planetesimals that formed near Jupiter are the likely sources of Earth's water.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉O'D Alexander, C M -- Boss, A P -- Carlson, R W -- New York, N.Y. -- Science. 2001 Jul 6;293(5527):64-8.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, N.W., Washington, DC 20015, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/11441173" 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
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Kepler-47: a transiting circumbinary multiplanet system (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-08-31
    Description: We report the detection of Kepler-47, a system consisting of two planets orbiting around an eclipsing pair of stars. The inner and outer planets have radii 3.0 and 4.6 times that of Earth, respectively. The binary star consists of a Sun-like star and a companion roughly one-third its size, orbiting each other every 7.45 days. With an orbital period of 49.5 days, 18 transits of the inner planet have been observed, allowing a detailed characterization of its orbit and those of the stars. The outer planet's orbital period is 303.2 days, and although the planet is not Earth-like, it resides within the classical "habitable zone," where liquid water could exist on an Earth-like planet. With its two known planets, Kepler-47 establishes that close binary stars can host complete planetary systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Orosz, Jerome A -- Welsh, William F -- Carter, Joshua A -- Fabrycky, Daniel C -- Cochran, William D -- Endl, Michael -- Ford, Eric B -- Haghighipour, Nader -- MacQueen, Phillip J -- Mazeh, Tsevi -- Sanchis-Ojeda, Roberto -- Short, Donald R -- Torres, Guillermo -- Agol, Eric -- Buchhave, Lars A -- Doyle, Laurance R -- Isaacson, Howard -- Lissauer, Jack J -- Marcy, Geoffrey W -- Shporer, Avi -- Windmiller, Gur -- Barclay, Thomas -- Boss, Alan P -- Clarke, Bruce D -- Fortney, Jonathan -- Geary, John C -- Holman, Matthew J -- Huber, Daniel -- Jenkins, Jon M -- Kinemuchi, Karen -- Kruse, Ethan -- Ragozzine, Darin -- Sasselov, Dimitar -- Still, Martin -- Tenenbaum, Peter -- Uddin, Kamal -- Winn, Joshua N -- Koch, David G -- Borucki, William J -- New York, N.Y. -- Science. 2012 Sep 21;337(6101):1511-4. Epub 2012 Aug 28.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Astronomy Department, San Diego State University, 5500 Campanile Drive, San Diego, CA 92182, USA. orosz@sciences.sdsu.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22933522" 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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  • 3
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    Stellar cosmogony: formation and evolution of low mass stars (1989)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1989-06-30
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Boss, A P -- New York, N.Y. -- Science. 1989 Jun 30;244(4912):1598.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17817283" 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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  • 4
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    Proximity of jupiter-like planets to low-mass stars (1995)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1995-01-20
    Description: The sensitivities of astrometric and radial velocity searches for extrasolar planets are strongly dependent on planetary masses and orbits. Because most nearby stars are less massive than the sun, the first detection is likely to be of a Jupiter-mass planet orbiting a low-mass star, with a possible theoretical expectation being that Jupiter-like planets will be found much closer [inside the Earth-sun separation of 1 astronomical unit (AU)] to these low-luminosity stars than Jupiter is to the sun (5.2 AU). However, radiative hydrodynamic models of protoplanetary disks around low-mass stars (of 0.1 to 1 solar mass) show that Jupiter-like planets should form at distances (approximately 4 to 5 AU) that are only weakly dependent on the stellar mass.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Boss, A P -- New York, N.Y. -- Science. 1995 Jan 20;267(5196):360-2.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17837483" 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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  • 5
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    A well-defined planet (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-11-26
    Description: 〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Boss, Alan P -- New York, N.Y. -- Science. 2011 Nov 25;334(6059):1057. doi: 10.1126/science.334.6059.1057-a.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22116861" 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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  • 6
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    High temperatures in the early solar nebula (1988)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1988-07-29
    Description: One fundamental controversy about terrestrial planet and asteroid formation is the discrepancy between meteoritical evidence for high temperatures (1500 K to 2000 K) in the inner solar nebula, and much lower theoretical temperature predictions on the basis of models of viscous accretion disks that neglect compressional heating of infalling gas. It is shown here that rigorous numerical calculations of the collapse of a rotating, three-dimensional presolar nebula are capable of producing temperatures on the order of 1500 K in the asteroid region (2.5 astronomical units), in either nearly axisymmetric or strongly nonaxisymmetric nebula models. The latter models may permit significant thermal cycling of solid components in the early inner solar nebula.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Boss, A P -- New York, N.Y. -- Science. 1988 Jul 29;241(4865):565-7.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17774577" 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
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    The origin of the moon (1986)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 1986-01-24
    Description: The origin of the moon is considered within the theory of formation of the terrestrial planets by accumulation of planetesimals. The theory predicts the occurrence of giant impacts, suggesting that the moon formed after a roughly Mars-sized body impacted on the protoearth. The impact blasted portions of the protoearth and the impacting body into geocentric orbit, forming a prelunar disk from which the moon later accreted. Although other mechanisms for formation of the moon appear to be dynamically impossible or implausible, fundamental questions must be answered before a giant impact origin can be considered both possible and probable.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Boss, A P -- New York, N.Y. -- Science. 1986 Jan 24;231(4736):341-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17735007" 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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  • 8
    Electronic Resource
    Electronic Resource
    The effect of rotation on the hydrodynamics of stellar collapse (1980)
    Springer
    Space science reviews 27 (1980), S. 555-561 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Summary Using values of d, γmin, and γmax that Van Riper (1978) has found most promising for a hydrodynamic envelope ejection, we have shown that even a small amount of rotation in the initial core can stop its collapse before nuclear densities are reached. We expected χi 〉 0.02 to produce significant deviations from a spherically symmetric collapse, but have found that χi as much as ten times smaller than this will not allow the core to reach densities as high as in the spherical collapse. In no case, however, does the core flatten very much, nor does the value of β become very large. Low final β's preclude the formation of an axisymmetric torus. They also indicate that deformation of an iron core into a triaxial configuration or fragmentation of the core during its collapse is an extremely unlikely event. (Note: Classically, β must exceed 0.27 before a dynamic instability to non-axisymmetric perturbations is encountered.) The small degree of flattening of the core also suggests that the reduced moment of inertia I of the core will always be relatively small in magnitude and hence that the third time derivative of I, which is proportional to the energy emitted in gravity wave radiation, will not be very significant. Numerically calculated estimates of I- during some of these model evolutions supports this suspicion. If the γmin and used here are found to be realistic values after the detailed physics of the core collapse is well understood, it is clear that gravitational radiation from a core collapse will be difficult to measure. Finally, we should point out that it is the relatively large values of Ymin (near 4/3) combined with values of d near unity that (a) prevented the core from flattening significantly in these models and (b) prevented the core from reaching high β configurations. If “realistic” values of either one (or both) of these parameters are found to be much smaller in more complete models of the core collapse, then the core will have to become flatter (and denser) before pressure gradients will support it along the rotation axis. All of the conclusions drawn here would be modified accordingly under those circumstances. It should also be noted that in general relativistic models, the critical Γ for spherical collapse is somewhat larger than 4/3 (Van Riper, 1979). Therefore, we predict that when fully general relativistic core collapses are performed including rotation, a given choice of γmin and βi will produce a slightly flatter and slightly denser core than the corresponding model that has been presented here.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00168349
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  • 9
    Electronic Resource
    Electronic Resource
    Collapse, equilibrium, and fragmentation of rotating, adiabatic clouds (1980)
    Springer
    Space science reviews 27 (1980), S. 255-259 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Numerical calculations of the collapse of adiabatic clouds from uniform density and rotation initial conditions show that when restricted to axisymmetry, the clouds form either near-equilibrium spheroids or rings. Rings form in the collapse of low thermal energy clouds and have β = T/ ¦W¦≳ 0.43. When the axisymmetric constraint is removed and an initial m=2 density variation is introduced, clouds either collapse to form near-equilibrium ellipsoids or else fragment into binary systems through a bar phase. Ellipsoids form in the collapse of high thermal energy clouds and have 3 ≲ 0.27. The results are consistent with the critical values of β for instabilities in Maclaurin spheroids, and suggest that protostellar clouds may undergo a dynamic fragmentation in the nonisothermal collapse regime.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00168306
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  • 10
    Electronic Resource
    Electronic Resource
    NASA and the Search for Extrasolar Planets (1998)
    Springer
    Earth, moon and planets 81 (1998), S. 35-38 
    Details
    ISSN: 1573-0794
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1006380328814
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