Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.212...49n&link_type=abstract
Astrophysics and Space Science, vol. 212, nos. 1-2, p. 49-56
Astronomy and Astrophysics
Astrophysics
Planetary Evolution, Protoplanets, Radial Flow, Solar System Evolution, Stellar Envelopes, Astronomical Models, Coefficients, Dynamic Models, Gravitational Effects, Migration, T Tauri Stars, Time Dependence
Scientific paper
Planetesimals orbiting a protostar in a circumstellar disk are affected by gravitational interaction among themselves and by gas drag force due to disk gas. Within the Kyoto model of planetesimal accretion, the migration rate is interpreted as the inverse of the planetary formation time scale. Here, we study time scales of gravitiational interaction and gas drag force and their influence on planetesimal migration in detail. Evaluating observations of 86 T Tauri stars (Beckwith et al., 1990), we find the mean radial temperature profile of circumstellar disks. The disk mass is taken to be 0.01 solar mass in accordance with minimum mass models and observed T Tauri disks. The time scale of gravitational interaction between planetesimals is studied analogously to Chandrasekhar's stellar dynamics. Hence, Chandrasekhar's coefficient lambda, defined as the fraction between the mean separation of planetesimals and the impact parameter, plays an important role in determining the migration rate. We find ln lambda to lie between 5 and 10 within the protosolar disk. Our result is that, at the stage of disk evolution considered here, gas drag force affects the radial migration of planetesimals by a few orders of magnitude more than gravitational interaction.
Feitzinger Johannes Viktor
Neuhaeuser Ralph
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