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Record Details

Record 1 of 16530
Terrestrial Planet Formation in Binary Star Systems
Author and Affiliation:
Lissauer, J. J.(NASA Ames Research Center, Moffett Field, CA, United States)
Quintana, E. V.(NASA Ames Research Center, Moffett Field, CA, United States)
Adams, F. C.(NASA Ames Research Center, Moffett Field, CA, United States)
Chambers, J. E.(NASA Ames Research Center, Moffett Field, CA, United States)
Abstract: 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 one or both components of various young close binary star systems. If planets form at the right places within such disks, they can remain dynamically stable for very long times. We have simulated the late stages of growth of terrestrial planets in both circumbinary disks around 'close' binary star systems with stellar separations ($a_B$) in the range 0.05 AU $\le a_B \le$ 0.4 AU and binary eccentricities in the range $0 \le e \le 0.8$ and circumstellar disks around individual stars with binary separations of tens of AU. The initial disk of planetary embryos is the same as that used for simulating the late stages of terrestrial planet growth within our Solar System and around individual stars in the Alpha Centauri system (Quintana et al. 2002, A.J., 576, 982); giant planets analogous to Jupiter and Saturn are included if their orbits are stable. The planetary systems formed around close binaries with stellar apastron distances less than or equal to 0.2 AU with small stellar eccentricities are very similar to those formed in the Sun-Jupiter-Saturn, whereas planetary systems formed around binaries with larger maximum separations tend to be sparser, with fewer planets, especially interior to 1 AU. Likewise, when the binary periastron exceeds 10 AU, terrestrial planets can form over essentially the entire range of orbits allowed for single stars with Jupiter-like planets, although fewer terrestrial planets tend to form within high eccentricity binary systems. As the binary periastron decreases, the radial extent of the terrestrial planet systems is reduced accordingly. When the periastron is 5 AU, the formation of Earth-like planets near 1 AU is compromised.
Publication Date: Jan 01, 2006
Document ID:
20060015679
(Acquired Jun 08, 2006)
Subject Category: ASTRONOMY
Document Type: Conference Paper
Meeting Information: American Astronomical Society meeting; 8-12 Jan. 2006; Washington, DC; United States
Meeting Sponsor: American Astronomical Society; United States
Contract/Grant/Task Num: 344-53-42
Financial Sponsor: NASA Ames Research Center; Moffett Field, CA, United States
Organization Source: NASA Ames Research Center; Moffett Field, CA, United States
Description: 1p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: No Copyright
NASA Terms: BINARY STARS; TERRESTRIAL PLANETS; PLANETARY EVOLUTION; STAR FORMATION; STELLAR ENVELOPES; PLANETARY SYSTEMS; GAS GIANT PLANETS; SOLAR SYSTEM; STELLAR ORBITS; SUN
Availability Source: Other Sources
Availability Notes: Abstract Only
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