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2
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33144488056
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M. C. Featou, K. U. Keller, H. A. Weaver, Eds. (Univ. of Arizona Press, Tucson, AZ)
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L. Dones, P. R. Weissman, H. F. Levison, M. J. Duncan, in Comets II, M. C. Featou, K. U. Keller, H. A. Weaver, Eds. (Univ. of Arizona Press, Tucson, AZ, 2004), p. 153.
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(2004)
Comets II
, pp. 153
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Dones, L.1
Weissman, P.R.2
Levison, H.F.3
Duncan, M.J.4
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3
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77954611739
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T. Paulech, M. Jakubí, L. Neslusan, P. A. Dybczynski, G. Leto, Astron. Astrophys. 509, A260000 (2010).
-
(2010)
Astron. Astrophys.
, vol.509
-
-
Paulech, T.1
Jakubík, M.2
Neslusan, L.3
Dybczynski, P.A.4
Leto, G.5
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4
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77954602116
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note
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This basic picture does not change if we invoke a model in which the planets migrate substantially (24-26).
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5
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77954619623
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The Sun was embedded in a star cluster for the first few million years of its existence. During this time, the gravitational potential of this cluster was the dominant perturber. After the Sun left the cluster, the Galaxy as a whole became the most important perturber
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The Sun was embedded in a star cluster for the first few million years of its existence. During this time, the gravitational potential of this cluster was the dominant perturber. After the Sun left the cluster, the Galaxy as a whole became the most important perturber.
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6
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77954593377
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note
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11.
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8
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0010961871
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S. Eggers, H. U. Keller, P. Kroupa, W. J. Markiewicz, Planet. Space Sci. 45, 1099 (1997).
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(1997)
Planet. Space Sci.
, vol.45
, pp. 1099
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Eggers, S.1
Keller, H.U.2
Kroupa, P.3
Markiewicz, W.J.4
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9
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33745300998
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F. C. Adams, E. M. Proszkow, M. Fatuzzo, P. C. Myers, Astrophys. J. 641, 504 (2006).
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(2006)
Astrophys. J.
, vol.641
, pp. 504
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Adams, F.C.1
Proszkow, E.M.2
Fatuzzo, M.3
Myers, P.C.4
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11
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77954591439
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As suggested by figure 2 of (9)
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As suggested by figure 2 of (9).
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12
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77954593376
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This was varied from run to run in order to optimize processing time
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This was varied from run to run in order to optimize processing time.
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13
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77954618534
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We have placed the same number of comets around each star, independent of its mass. We took this simple approach because too little is known about other planetary systems to make a more physically based assumption. See SOM text 3 for a discussion and for results where we have relaxed our assumption
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We have placed the same number of comets around each star, independent of its mass. We took this simple approach because too little is known about other planetary systems to make a more physically based assumption. See SOM text 3 for a discussion and for results where we have relaxed our assumption.
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14
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77954602660
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Here we define a singleton as a star that is not gravitationally bound to either another star or to the cluster as a whole. The Sun is a singleton
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Here we define a singleton as a star that is not gravitationally bound to either another star or to the cluster as a whole. The Sun is a singleton.
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15
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77954608785
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The Oort cloud has been evolving and losing objects over the lifetime of the solar system. Thus, although the Oort cloud extends to a > ̃105 AU, we only included comets with a < 50,000 AU in our analysis in order to avoid the need to account for this loss. We chose 50,000 AU because this is the largest semimajor axis for which survival for 4 billion years is likely (2)
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The Oort cloud has been evolving and losing objects over the lifetime of the solar system. Thus, although the Oort cloud extends to a > ̃105 AU, we only included comets with a < 50,000 AU in our analysis in order to avoid the need to account for this loss. We chose 50,000 AU because this is the largest semimajor axis for which survival for 4 billion years is likely (2)
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16
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77954590692
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As we were preparing this manuscript,we became aware of (29), who independently found that this mechanism can be responsible for the formation of wide binary star systems
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As we were preparing this manuscript, we became aware of (29), who independently found that this mechanism can be responsible for the formation of wide binary star systems.
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17
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77954576947
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An encounter between the Sun and another star has been invoked before (30,31) to explain the origin of Sedna, which has an unusual orbit with a semimajor axis of 526 AU and a perihelion distance well beyond the orbits of the planets at 76 AU. See (32) for a detailed early study of this type of encounter
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An encounter between the Sun and another star has been invoked before (30, 31) to explain the origin of Sedna, which has an unusual orbit with a semimajor axis of 526 AU and a perihelion distance well beyond the orbits of the planets at 76 AU. See (32) for a detailed early study of this type of encounter.
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18
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77954585837
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In the real system, there are two dynamical mechanisms for stripping comets away from their original parent stars. The first involves close encounters between the stars. This effect is included in our calculations. The second is caused by close encounters between the comets and the planets in orbit around the parent stars. For computational reasons, this effect was not directly included in these calculations. However, because most comets are stripped by the first process in our simulations, the lack of the second is not significant from the dynamical point of view
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In the real system, there are two dynamical mechanisms for stripping comets away from their original parent stars. The first involves close encounters between the stars. This effect is included in our calculations. The second is caused by close encounters between the comets and the planets in orbit around the parent stars. For computational reasons, this effect was not directly included in these calculations. However, because most comets are stripped by the first process in our simulations, the lack of the second is not significant from the dynamical point of view.
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20
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0039436513
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T. Rettig, J. M. Hahn, Eds. 107 of the Astronomical Society of the Pacific Conference Series (Astronomical Society of the Pacific, San Francisco)
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P. R. Weissman, in Completing the Inventory of the Solar System: A Symposium Held in Conjunction with the 106th Annual Meeting of the ASP, T. Rettig, J. M. Hahn, Eds., vol.107 of the Astronomical Society of the Pacific Conference Series (Astronomical Society of the Pacific, San Francisco, 1996), pp. 265-288.
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(1996)
Completing the Inventory of the Solar System: A Symposium Held in Conjunction with the 106th Annual Meeting of the ASP
, pp. 265-288
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Weissman, P.R.1
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21
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77954612584
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The uncertainty in this value is over an order of magnitude. Here, we are simply using the classic value from (20)
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The uncertainty in this value is over an order of magnitude. Here, we are simply using the classic value from (20).
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22
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77954578618
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16 g (20), which is very uncertain (21). Thus, it considers all possible sources for Oort cloud comets
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16 g (20), which is very uncertain (21). Thus, it considers all possible sources for Oort cloud comets.
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23
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77954603265
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It is interesting to speculate whether we would expect to see substantial compositional differences between comets due to our results. These stars formed in the same cluster as the Sun, and thus all the comets formed basically from the same cloud of material. Thus, it is not obvious what to expect.
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It is interesting to speculate whether we would expect to see substantial compositional differences between comets due to our results. These stars formed in the same cluster as the Sun, and thus all the comets formed basically from the same cloud of material. Thus, it is not obvious what to expect.
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26
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19544378163
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K. Tsiganis, R. Gomes, A. Morbidelli, H. F. Levison, Nature 435, 459 (2005).
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(2005)
Nature
, vol.435
, pp. 459
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Tsiganis, K.1
Gomes, R.2
Morbidelli, A.3
Levison, H.F.4
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33
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77954614201
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We thank A. Morbidelli and L. Dones for useful discussions. This work was supported by NASA's Astrobiology Institute through a grant to the Goddard Center for Astrobiology. H.F.L. is grateful to NASA for funding through its Operational Support Services and Outer Planets Research programs. M.J.D. is grateful for the hospitality and financial support of the Isaac Newton Institute at Cambridge University, where some of this work was performed. M.J.D. acknowledges the continuing financial support of the Natural Sciences and Engineering Research Council, Canada. R.B. thanks Germany's Helmholz Alliance for financial support
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We thank A. Morbidelli and L. Dones for useful discussions. This work was supported by NASA's Astrobiology Institute through a grant to the Goddard Center for Astrobiology. H.F.L. is grateful to NASA for funding through its Operational Support Services and Outer Planets Research programs. M.J.D. is grateful for the hospitality and financial support of the Isaac Newton Institute at Cambridge University, where some of this work was performed. M.J.D. acknowledges the continuing financial support of the Natural Sciences and Engineering Research Council, Canada. R.B. thanks Germany's Helmholz Alliance for financial support.
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