Hostname: page-component-8448b6f56d-mp689 Total loading time: 0 Render date: 2024-04-20T11:27:03.268Z Has data issue: false hasContentIssue false
  • English
  • Français

Origin of the dusty disks around white dwarfs

Published online by Cambridge University Press:  01 October 2007

R. B. Dong ,
Y. Wang ,
D. N. C. Lin  and
X. W. Liu
R. B. Dong
Affiliation:
Department of Astronomy, Peking University, 100871, Beijing, China, email: rbdong@pku.edu.cn
Y. Wang
Affiliation:
Department of Astronomy, Peking University, 100871, Beijing, China, email: rbdong@pku.edu.cn
D. N. C. Lin
Affiliation:
Kavli Institute of Astronomy and Astrophysics, Peking University, 100871, Beijing, China email: liuxw@bac.pku.edu.cn Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA email: lin@ucolick.org
X. W. Liu
Affiliation:
Department of Astronomy, Peking University, 100871, Beijing, China, email: rbdong@pku.edu.cn Kavli Institute of Astronomy and Astrophysics, Peking University, 100871, Beijing, China email: liuxw@bac.pku.edu.cn
Rights & Permissions [Opens in a new window]

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.

Some circumstantial evidence for residual planetesimals is constructed based on the recent discovery of a dusty ring around a young white dwarf at the center of the Helix nebula (Su et al. 2007). This ring extends between about 35 and 150 AU from the nebula center, and have a total mass of about 0.13 M⊕. In this paper we propose that this ring is the by-product of planets and planetesimals' orbital evolution during the epoch when the central star rapidly lost most of its mass. We examine the dynamical evolution of planetary systems similar to the solar system (i.e. with gas giant planets and residual planetesimals) as their host stars evolve off the main sequence. During the process, some planetesimals will be captured by the gas giants into mean motion resonances and their mutual collisions will form a dust ring similar to that observed at the center of the Helix nebula.

Keywords

Giant planetplanetary formationdebris disksplanet dynamicsn-body simulation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 381 - 384
Copyright
Copyright © International Astronomical Union 2008

References

Adachi, I., Hayashi, C. & Nakazawa, K. 1976, Prog. of Theo. Phys., 56, 1756CrossRefGoogle Scholar
Artymowicz, P. 1993, ApJ, 419,155CrossRefGoogle Scholar
Bodenheimer, P., Lin, D. N. C. & Mardling, R. A. 2001, ApJ, 548, 466CrossRefGoogle Scholar
Bodenheimer, P., & Pollack, J.B. 1986, Icarus, 67, 391CrossRefGoogle Scholar
Burrows, A. et al. 2000, ApJ, 534, L97CrossRefGoogle Scholar
Bryden, G. et al. 2000, ApJ, 540, 1091Google Scholar
Dobbs-Dixon, I., Li, S.L., Lin, D. N. C., 2007, Tidal Barrier and the Asymptotic Mass of Proto Gas-Giant Planets, arXiv:astro-ph/0701269.Google Scholar
Frank, J., King, A. & Raine, D. 2002, Accretion power in Astrophysics, Cambridge university press.CrossRefGoogle Scholar
Franklin, F. A. et al. 1980, Icarus, 42, 271CrossRefGoogle Scholar
Garaud, P. & Lin, D. N. C. 2007, ApJ, 654, 606Google Scholar
Goldreich, P., Lithwick, Y. & Sari, R. 2004, ApJ, 614, 497CrossRefGoogle Scholar
Goldreich, P. & Tremaine, S. 1978, ApJ, 222, 850Google Scholar
Goldreich, P. & Tremaine, S. 1980, ApJ, 241, 425Google Scholar
Greenzweig, Y., & Lissauer, J. J. 1992, Icarus, 100, 440CrossRefGoogle Scholar
Guillot, T., Gautier, D., & Hubbard, W. B. 1997, Icarus, 130, 534CrossRefGoogle Scholar
Hasegawa, M., Nakazawa, K. 1990, A&A, 227, 619Google Scholar
Hayashi, C., Nakazawa, K. & Nakagawa, Y. 1985, in Protoplanets and Planets II ed. Balck, D. C. & Mathew, M. S. (Tucson: Univ. Arizona Press), 1100Google Scholar
Hayashi, C. 1981, Prog. Theor. Phys. Suppl., 70,35Google Scholar
Hayashi, C., Nakazawa, K., & Adachi, I. 1977, Publ. Astron. Soc. Japan. 29, 163Google Scholar
Hubickyj, O., Bodenheimer, P., & Lissauer, J. J. 2005, Icarus, 179, 415Google Scholar
Ida, S. & Lin, D. N. C. 1996, AJ, 112,1239CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2004, ApJ, 604,388CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2007, submitted to ApJGoogle Scholar
Ikoma, M., Nakazawa, K., Emori, H. 2000, ApJ 537, 1013CrossRefGoogle Scholar
Inaba, S. & Ikoma, M. 2003, A&A, 410, 711Google Scholar
Kokubo, E. & Ida, S. 1996, Icarus, 123, 180CrossRefGoogle Scholar
Kokubo, E. & Ida, S. 2000, Icarus, 143, 15Google Scholar
Kokubo, E. & Ida, S. 2002, ApJ, 581, 666Google Scholar
Koller, J., Li, H., & Lin, D. N. C 2003, ApJ 596, L91CrossRefGoogle Scholar
Kominami, J., & Ida, S. 2002, Icarus 157, 43Google Scholar
Laughlin, G., Steinacker, A. & Adams, R. 2004, ApJ, 608, 489Google Scholar
Levison, H. F. & Duncan, M. J. 1994, Icarus 108, 18Google Scholar
Lin, D. N. C, Bodenheimer, P. & Richardson, D. C. 1996, Nature, 380, 606CrossRefGoogle Scholar
Lin, D. N. C., Ida, S. 1997 ApJ 477, 781Google Scholar
Lin, D.N.C, & Papaloizou, J. C. B. 1979, MNRAS, 186, 799Google Scholar
Lin, D. N. C, & Papaloizou, J. C. B. 1986, ApJ, 309, 846Google Scholar
Lin, D. N. C, & Papaloizou, J. C. B. 1993, in: Levy, E. H. & Lunine, J. I. (eds.), Protostars and Planets III, (Tucson: Unv. Arizona), p. 749Google Scholar
Leinhardt, Z. & Richardson, D. C. 2005, ApJ, 625, 427CrossRefGoogle Scholar
Lissauer, J. J. 1987, Icarus, 69, 249CrossRefGoogle Scholar
Marcy, G., et al. 2005, Prog. Theor. Phys. Suppl., 158, 24CrossRefGoogle Scholar
Mizuno, H. 1980, Prog. Theor. Phys., 64, 544Google Scholar
Murray, C. D., & Dermott, S. F. 1999, Solar system Dynamcis, Cambridge Unversity.Google Scholar
Nelson, R. P. & Papaloizou, J. C. B. 2003, MNRAS, 339, 993CrossRefGoogle Scholar
Palmer, P. L., Lin, D. N. C. & Aarseth, S. J. 1993, ApJ, 403, 336CrossRefGoogle Scholar
Perri, F. & Cameron, A. G. W. 1974, Icarus 22, 416Google Scholar
Pollack, J. B. et al. 1996, Icarus, 124, 62Google Scholar
Rafikov, R. R. 2001, AJ, 122, 2713Google Scholar
Rice, W. K. M. & Armitage, P. J. 2003, ApJ, 598, L55Google Scholar
Safronov, V.S. 1969, Evolution of the Protoplanetary Cloud and Formation of the Earth and Planets (Moscow: Nauka)Google Scholar
Sato, B. et al. 2005, ApJ, 633, 465Google Scholar
Saumon, D. & Guillot, T. 2004, ApJ, 609, 1170Google Scholar
Shakura, N.I. & Sunyaev, R.A. 1973, AAp, 24, 337Google Scholar
Tanaka, H. & Ida, S. 1999, Icarus, 139,350Google Scholar
Tanaka, H., Takeuchi, T. & Ward, W. R. 2002, ApJ 565, 1257CrossRefGoogle Scholar
Ward, W. R. 1986, Icarus, 67,164CrossRefGoogle Scholar
Ward, W. R. 1989, ApJ, 336,526CrossRefGoogle Scholar
Ward, W. R. 1997, Icarus, 126,261Google Scholar
Wetherill, G. W & Stewart, G. R. 1989, Icarus, 77, 330Google Scholar
Wuchterl, G., Guillot, T., & Lissauer, J. J. 2000, in Protostars and Planets IV eds. Mannings, V., Boss, A.P. & Russell, S. S. (Tucson : Univ. Arizona Press), 1081Google Scholar
Zhou, J. L., Lin, D. N. C. & Sun, Y. S. 2007, ApJ, 666, 423.CrossRefGoogle Scholar