Skip to main content Accessibility help
×
Home

N-body Simulations of Planet Formation

  • Shigeru Ida (a1), Eiichiro Kokubo (a2) and Junko Kominami (a1)

Abstract

Accretion from many small planetesimals to planets is reviewed. Solid protoplanets accrete through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.1-0.2 Earth mass, which suggests giant impacts among the protoplanets in the final stage of terrestrial planet formation. On the other hand, the isolation mass in Jupiter's and Saturn's orbits is about a few to 5 Earth masses, which may be massive enough to trigger gas accretion onto the cores. The isolation mass in Uranus and Neptune's orbits is as large as their present cores. Extending the above arguments to extrasolar planetary systems that are formed from disks with various initial masses, we also discuss diversity of extrasolar planetary systems.

    • Send article to Kindle

      To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

      Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

      Find out more about the Kindle Personal Document Service.

      N-body Simulations of Planet Formation
      Available formats
      ×

      Send article to Dropbox

      To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

      N-body Simulations of Planet Formation
      Available formats
      ×

      Send article to Google Drive

      To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

      N-body Simulations of Planet Formation
      Available formats
      ×

Copyright

References

Hide All
Adachi, I., Hayashi, C., & Nakazawa, K. 1976, Prog. Theor. Phys., 56, 1756
Agnor, C. B., Canup, R. M., & Levison, H. F. 1999, Icarus, 142, 219
Beckwith, S. V. W. & Sargent, A. I. 1993, in Protostars and Planets III, ed. Levy, E. H. & Lunine, J. I. (Tuscon: Univ. of Arizona Press), 521; 1996, Nature, 383, 139
Bodenheimer, P. & Pollack, J. B. 1986, Icarus, 67, 391
Chambers, J. E. & Wetherill, G. W. 1998, Icarus, 136, 30
Chambers, J. E., Wetherill, G. W., & Boss, A. P. 1996, Icarus, 119, 261
Hayashi, C. 1981, Prog. Theor. Phys. Suppl., 70, 35
Hayashi, C., Nakazawa, K., & Nakagawa, Y. 1985 in Protostars and Planets II, ed. Black, D. C. & Matthews, M. S. (Tuscon: Univ. of Arizona Press), 1100
Ida, S. & Kokubo, E. 2001, in ASP Conf. Series, Planetary Systems in the Universe: Observation, Formation and Evolution, eds. Penny, A.J., Artymowicz, P., Lagrange, A.-M., and Russell, S.S. (San Francisco, ASP), in press
Ida, S. & Makino, J. 1992, Icarus, 96, 107; 1993, Icarus, 106, 210
Ikoma, M., Nakazawa, K., & Emori, H. 2000, ApJ, 537, 1013
Ito, T. & Tanikawa, K. 1999, Icarus, 139, 336
Iwasaki, K, Tanaka, H., Nakazawa, K., & Emori, H. 2001a, PASJ, 53, 321; 2001b, submitted to PASJ
Kokubo, E. & Ida, S 1995, Icarus, 114, 247; 1996, Icarus, 123, 180; 1998, Icarus, 131, 171; 2000, Icarus, 143, 15
Lin, D. N. C. & Ida, S. 1997, ApJ, 477, 781
Lin, D. N. C., Bodenheimer, P., & Richardson, D. 1996, Nature, 380, 606
Lin, D. N. C. & Papaloizou, J. C. B. 1993, in Protostars and Planets III, ed. Levy, E. H. & Lunine, J. I. (Tuscon: Univ. of Arizona Press), 749
Mizuno, H. 1981, Prog. Theor. Phys., 64, 544
Nagasawa, M, Tanaka, H. & Ida, S. 2000, AJ, 119, 1480
Safronov, V. 1969, Evolution of the protoplanetary cloud and formation of the earth and planets (Moscow: Nauka Press)
Stewart, G. R. & Wetherill, G. W. 1988, Icarus, 74, 542
Strom, S. E., Edwards, S., & Skrutski, M. F. 1993, in Protostars and Planets III eds. Levy, E.H. & Lunine, J.I. (Tucson: Univ. of Arizona Press), 837
Ward, W. R. 1986, Icarus, 67, 164; 1993, Icarus, 106, 274; 1997 Icarus, 126, 261
Weidenschilling, S. J. 1984, Icarus, 60, 553
Weidenschilling, S. J. & Marzari, F. 1996, Nature, 384, 619
Wetherill, G. W. 1980, ARA&A, 18, 77
Wetherill, G. W. & Stewart, G. R. 1989, Icarus, 77, 330
Zuckerman, B., Forveille, T. & Kastner, J. H. 1995, Nature, 373, 494

Metrics

Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed