@inproceedings{oai:jaxa.repo.nii.ac.jp:00020653,
 author = {森脇, 一匡 and 中川, 義次 and Moriwaki, Kazumasa and Nakagawa, Yoshitsugu},
 book = {第36回月・惑星シンポジウム, Proceedings of the 36th ISAS Lunar and Planetary Symposium},
 month = {Nov},
 note = {Until recently, it had been believed that only single solar-type stars might harbor planetary systems. On the other hand, circumbinary disks have been detected by mm/sub-mm wavelength observation. Planets may be formed also in such disks. The conditions for planetesimal accretion in a circumbinary disk are investigated. The binary system gives stronger gravitational perturbation against planetesimals orbiting nearer to the binary. Therefore, the relative velocities between planetesimals will be larger, and when they exceed the escape velocity, it is impossible for the planetesimals to accumulate into a planet. Long-term numerical integrations of binary and planetesimal orbital motions are performed, and the upper limit of planetesimal semimajor axes is found where the velocity dispersion of the planetesimals exceeds the escape velocity. That is, when the binary semimajor axis is set to 1 AU, the eccentricity to 0.1 and the total mass to 1 solar mass, the planetesimals are prevented from accreting when they orbit in a zone within 13 AU from the barycenter of the binary system. In regions outer than 13 AU, planetesimals can accrete. Also derived is an analytic expression of the eccentricity of a planetesimal excited by the gravitational perturbation of the binary., 資料番号: AA0046650004},
 pages = {13--16},
 publisher = {宇宙航空研究開発機構宇宙科学研究本部, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS)},
 title = {A planetesimal accretion zone in a circumbinary disk},
 year = {2003}
}