PLANET FORMATION IN BINARY SYSTEMS: A SEPARATION-DEPENDENT MECHANISM?
نویسندگان
چکیده
منابع مشابه
Terrestrial Planet Formation in Binary Star Systems
More than half of all main sequence stars, and an even larger fraction of pre-main sequence stars, reside in binary/multiple star systems [1, 2]. Numerical simulations of the collapse of molecular cloud cores to form binary stars suggest that disks form within binary star systems [3]. The presence of disk material has been indirectly observed around one or both components of some young binary s...
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Recent radial velocity observations have indicated that Jovian-type planets can exist in moderately close binary star systems. Numerical simulations of the dynamical stability of terrestrial-class planets in such environments have shown that, in addition to their giant planets, these systems can also harbor Earth-like objects. In this paper, we study the late stage of terrestrial planet formati...
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We calculate herein the late stages of terrestrial planet accumulation around a solar type star that has a binary companion with semimajor axis larger than the terrestrial planet region. We perform more than one hundred simulations to survey binary parameter space and to account for sensitive dependence on initial conditions in these dynamical systems. As expected, sufficiently wide binaries le...
متن کاملTerrestrial Planet Formation Surrounding Close Binary Stars
Most stars reside in binary/multiple star systems; however, previous models of planet formation have studied growth of bodies orbiting an isolated single star. Disk material has been observed around both components of some young close binary star systems. Additionally, it has been shown that if planets form at the right places within such disks, they can remain dynamically stable for very long ...
متن کاملPlanet formation is unlikely in equal mass binary systems with a ∼ 50 AU
We show that planet formation via both gravitational collapse and core accretion is unlikely to occur in equal mass binary systems with moderate (∼ 50 AU) semimajor axes. Internal thermal energy generation in the disks is sufficient to heat the gas everywhere so that spiral structures quickly decay rather than grow or fragment. This same heating will inhibit dust coagulation because the tempera...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2010
ISSN: 2041-8205,2041-8213
DOI: 10.1088/2041-8205/709/2/l114