Migrating planets

Science

Volumn 279, Issue 5347, 1998, Pages 69-72

  Murray, N ^a   Hansen, B ^a   Holman, M ^a   Tremaine, S ^a,b  

^a UNIVERSITY OF TORONTO   (Canada)

^b CANADIAN INSTITUTE FOR ADVANCED RESEARCH   (Canada)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; EVOLUTION; GRAVITY; MIGRATION; PHYSICS; PRIORITY JOURNAL; THEORY;

EID: 0032472240     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.279.5347.69     Document Type: Article

References (45)

1. J. J. Lissauer, Annu. Rev. Astron. Astrophys. 31, 129 (1993).
2. R. P. Butler, G. W. Marcy, E. Williams, H. Hauser, P. Shirts, Astrophys. J. 474, L115 (1997).
3. M. Mayor and D. Queloz, Nature 378, 355 (1995).
4. R. W. Noyes et al., Astrophys. J. 483, L111 (1997); see also erratum, ibid. 487, L195 (1997).
5. D. W. Latham, R. P. Stefanik, T. Mazeh, M. Mayor, G. Burki, Nature 339, 38 (1989).
6. G. W. Marcy and R. P. Butler, Astrophys. J. 464, L147 (1996).
7. W. D. Cochran, A. P. Hatzes, R. P. Butler, G. W. Marcy, ibid. 483, 457 (1997).
8. R. P. Butler and G. W. Marcy, ibid. 464, L153 (1996). See also the extrasolar planets catalog at http://www. obspm.fr:80/departement/darc/planets/catalog. html.
9. D. Gray, Nature 385, 795 (1996); G. Marcy et al., Astrophys. J. 481, 926 (1997).
10. D. Gray, Nature 385, 795 (1996); G. Marcy et al., Astrophys. J. 481, 926 (1997).
11. D. N. C. Lin, P. Bodenheimer, D. C. Richardson, Nature 380, 606 (1996).
12. P. Goldreich and S. Tremaine, Astrophys. J. 241, 425 (1980).
13. F. A. Rasio and E. B. Ford, Science 274, 954 (1996).
14. S. J. Weidenschilling and F. Marzari, Nature 384, 619 (1996).
15. M. Holman and N. Murray, Astron. J. 112, 1278 (1996); N. Murray and M. Holman, ibid. 114, 1246 (1997); The presence of a massive planetesimal disk can change both the location and the amount of overlap relative to a Keplerian potential. The change in location will not affect the dynamics, and our calculations show that the change in the amount of overlap is generally small.
16. M. Holman and N. Murray, Astron. J. 112, 1278 (1996); N. Murray and M. Holman, ibid. 114, 1246 (1997); The presence of a massive planetesimal disk can change both the location and the amount of overlap relative to a Keplerian potential. The change in location will not affect the dynamics, and our calculations show that the change in the amount of overlap is generally small.
17. 1 but this expression must be used with caution when the resonances are strong, because the dynamics are more complicated [see (14)].
18. Somewhat longer times apply in other low-order, mean-motion resonances. Similar results apply if the planet orbits inside the planetesimal.
19. p) than the random walk in E or L.
20. H. F. Levison and M. Duncan, Icarus 108, 18 (1994). The lifetimes of Centaurs are similar [see L. Dones, H. F. Levison, M. Duncan, in Completing the Inventory of the Solar System, T. W. Rettig and J. M. Hahn, Eds. (Astronomical Society of the Pacific, San Francisco, CA, 1996), p. 233].
21. H. F. Levison and M. Duncan, Icarus 108, 18 (1994). The lifetimes of Centaurs are similar [see L. Dones, H. F. Levison, M. Duncan, in Completing the Inventory of the Solar System, T. W. Rettig and J. M. Hahn, Eds. (Astronomical Society of the Pacific, San Francisco, CA, 1996), p. 233].
22. Equation 2 holds for planets the mass and size of Jupiter with orbital periods larger than about 50 days.
23. B. V. Chirikov, Chaotic Dynamics in Hamiltonian Systems with Divided Phase Space (Springer, Berlin, 1983); C. F. F. Karney, Physica D 8, 360 (1983); N. Murray, ibid. 52, 220 (1991).
24. B. V. Chirikov, Chaotic Dynamics in Hamiltonian Systems with Divided Phase Space (Springer, Berlin, 1983); C. F. F. Karney, Physica D 8, 360 (1983); N. Murray, ibid. 52, 220 (1991).
25. B. V. Chirikov, Chaotic Dynamics in Hamiltonian Systems with Divided Phase Space (Springer, Berlin, 1983); C. F. F. Karney, Physica D 8, 360 (1983); N. Murray, ibid. 52, 220 (1991).
26. H. F. Levison and M. Duncan, Icarus 127, 13 (1997); M. J. Duncan and H. F. Levison, Science 276, 1670 (1997).
27. H. F. Levison and M. Duncan, Icarus 127, 13 (1997); M. J. Duncan and H. F. Levison, Science 276, 1670 (1997).
28. By similar arguments, orbit-crossing planetesimals that collide with the star add energy to the planet; however, consumption by the star is much less common than ejection for planets at semimajor axes larger than a few stellar radii.
29. J. A. Fernández and W.-H. Ip, Icarus 58, 109 (1984).
30. J.-C. Liou and R. Malhotra, Science 275, 375 (1997).
31. -2/3 = 0.7 if the inner 7:4 resonance is the only relevant one.
32. E. J. Öpik, Interplanetary Encounters (Elsevier Scientific, Amsterdam, 1976).
33. A. Toomre, Astrophys. J. 139, 1217 (1964); V. S. Safronov, Ann. Astrophys. 23, 979 (1960); J. Binney and S. Tremaine, Galactic Dynamics (Princeton Univ. Press, Princeton, NJ, 1987).
34. A. Toomre, Astrophys. J. 139, 1217 (1964); V. S. Safronov, Ann. Astrophys. 23, 979 (1960); J. Binney and S. Tremaine, Galactic Dynamics (Princeton Univ. Press, Princeton, NJ, 1987).
35. A. Toomre, Astrophys. J. 139, 1217 (1964); V. S. Safronov, Ann. Astrophys. 23, 979 (1960); J. Binney and S. Tremaine, Galactic Dynamics (Princeton Univ. Press, Princeton, NJ, 1987).
36. M. Holman, J. Touma, S. Tremaine, Nature 386, 254 (1997); K. A. Innanen, J. Q. Zheng, S. Mikkola, M. J. Valtonen Astron. J. 113, 1915 (1997); T. Mazeh, Y. Krymolowski, G. Rosenfeld, Astrophys. J. 477, L103 (1997).
37. M. Holman, J. Touma, S. Tremaine, Nature 386, 254 (1997); K. A. Innanen, J. Q. Zheng, S. Mikkola, M. J. Valtonen Astron. J. 113, 1915 (1997); T. Mazeh, Y. Krymolowski, G. Rosenfeld, Astrophys. J. 477, L103 (1997).
38. M. Holman, J. Touma, S. Tremaine, Nature 386, 254 (1997); K. A. Innanen, J. Q. Zheng, S. Mikkola, M. J. Valtonen Astron. J. 113, 1915 (1997); T. Mazeh, Y. Krymolowski, G. Rosenfeld, Astrophys. J. 477, L103 (1997).
39. S. V. W. Beckwith, A. I. Sargent, R. S. Chini, R. Güsten, Astron. J. 99, 924 (1990).
40. A possible concern with the interpretation of these observations is that the gas surface density may imply gravitational instability if the disk extends out to 100 AU. See the references in (27).
41. R. P. Butler, G. W. Marcy, E. Williams, H. Hauser, P. Shirts, Astrophys. J. 474, L115 (1997); S. L. Baliunas, G. W. Henry, R. A. Donahue, F. C. Fekel, W. H. Soon, ibid., p. L119; G. Gonzalez, Mon. Not. R. Astron. Soc. 285, 403 (1997); G. Laughlin and F. C. Adams, http://xxx.lanl.gov/abs/astro-ph/9710110. "Planet swallowing" as a source of abundance anomalies in stellar atmospheres was first discussed by J. B. Alexander [Observatory 87, 238 (1967)].
42. R. P. Butler, G. W. Marcy, E. Williams, H. Hauser, P. Shirts, Astrophys. J. 474, L115 (1997); S. L. Baliunas, G. W. Henry, R. A. Donahue, F. C. Fekel, W. H. Soon, ibid., p. L119; G. Gonzalez, Mon. Not. R. Astron. Soc. 285, 403 (1997); G. Laughlin and F. C. Adams, http://xxx.lanl.gov/abs/astro-ph/9710110. "Planet swallowing" as a source of abundance anomalies in stellar atmospheres was first discussed by J. B. Alexander [Observatory 87, 238 (1967)].
43. R. P. Butler, G. W. Marcy, E. Williams, H. Hauser, P. Shirts, Astrophys. J. 474, L115 (1997); S. L. Baliunas, G. W. Henry, R. A. Donahue, F. C. Fekel, W. H. Soon, ibid., p. L119; G. Gonzalez, Mon. Not. R. Astron. Soc. 285, 403 (1997); G. Laughlin and F. C. Adams, http://xxx.lanl.gov/abs/astro-ph/9710110. "Planet swallowing" as a source of abundance anomalies in stellar atmospheres was first discussed by J. B. Alexander [Observatory 87, 238 (1967)].
44. R. P. Butler, G. W. Marcy, E. Williams, H. Hauser, P. Shirts, Astrophys. J. 474, L115 (1997); S. L. Baliunas, G. W. Henry, R. A. Donahue, F. C. Fekel, W. H. Soon, ibid., p. L119; G. Gonzalez, Mon. Not. R. Astron. Soc. 285, 403 (1997); G. Laughlin and F. C. Adams, http://xxx.lanl.gov/abs/astro-ph/9710110. "Planet swallowing" as a source of abundance anomalies in stellar atmospheres was first discussed by J. B. Alexander [Observatory 87, 238 (1967)].
45. We acknowledge useful conversations with R. Malhotra and B. Paczyński. This research was supported by the Natural Sciences and Engineering Research Council of Canada and the Canadian Institute for Advanced Research.