Hostname: page-component-77c89778f8-vsgnj Total loading time: 0 Render date: 2024-07-19T06:14:38.397Z Has data issue: false hasContentIssue false
  • English
  • Français

Dust Particle Settling in Protoplanetary Disks around Young Stars in Binary Systems

Published online by Cambridge University Press:  26 May 2016

Y. Sato  and
Y. Nakagawa
Y. Sato
Affiliation:
Department of Physics, School of Science, Kwansei Gakuin University, 1-1-155, Uegahara, Nishinomiya, Hyogo, 662-8501, Japan
Y. Nakagawa
Affiliation:
Department of Earth and Planetary Sciences, Faculty of Science Kobe University, Kobe 657-8501, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We calculate the SEDs of young stars accompanied by protoplanetary disks, taking into account the effect of the settling of dust particles. Observed disk candidates contain significant number of binary or multiple systems. We compare our results with observed data and obtain many excellent fittings. From the results, it is found that in close binary systems the disk masses are relatively low and dust particles is hard to settle as compared with the cases of disks in wide binaries or around isolated stars. This is attributable to gravitational perturbation from the companion stars, which will disturb formation of planetary systems in close binary systems.

Type
Part IV: Protoplanetary and β Pic disks
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 365 - 367
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Miyake, K., & Nakagawa, Y. 1995, ApJ, 441, 361.Google Scholar
Kusaka, T., Nakano, T., & Hayashi, C. 1970, Prog. Theor. Phys., 44, 1580.CrossRefGoogle Scholar
Chiang, E. I., & Goldreich, P. 1997, ApJ, 490, 368.Google Scholar
Miyake, K., & Nakagawa, Y. 1993, ICARUS, 106, 20.CrossRefGoogle Scholar
Strom, K. M. et al. 1989, AJ, 97, 1451.Google Scholar
Osterloh, M., & Beckwith, S. V. W. 1995, ApJ, 439, 288.Google Scholar
Sato, Y., & Nakagawa, Y. 1999, Proc. of Star Formation 1999, 235.Google Scholar