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Query : 2009MNRAS.393.1219P |
2009MNRAS.393.1219P - Mon. Not. R. Astron. Soc., 393, 1219-1234 (2009/March-2)
Dynamical simulations of the planetary system HD69830.
PAYNE M.J., FORD E.B., WYATT M.C. and BOOTH M.
Abstract (from CDS):
We find that (i) it is not possible to explain the observed planetary eccentricities (∼0.1) purely as the result of planetary perturbations during migration unless the planetary systems nearly face-on. However, the presence of gas damping in the system only serves to exacerbate the problem again. (ii) The rate of accretion of planetesimals on to planets in our N-body simulations is significantly different to that assumed in the semi-analytic models, with our inner planet accreting at a rate an order of magnitude greater than the outer ones, suggesting that one cannot successfully treat planetesimal accretion in the simplified manner of Alibert et al. (iii) We find that the eccentricity damping of planetesimals does not act as an insurmountable obstacle to the existence of an excited eccentric disc: all simulations result in a significant fraction (∼15 per cent) of the total planetesimal disc mass, corresponding to ∼25M⊕, remaining bound in the region ∼1-9au, even after all three planets have migrated through the region. (iv) This swarm of planetesimals has orbital distributions that are size sorted by gas drag, with the largest planetesimals (∼1000km), which may contain a large proportion of the system mass, preferentially occupying the highest eccentricity (and thus longest lived) orbits. Although such planetesimals would be expected to collide and produce a disc of warm dust, further work will be required to understand whether these eccentricity distributions are high enough to explain the level of dust emission observed despite mass loss via steady state collisional evolution.
Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS
Journal keyword(s): planetary systems - planetary systems: formation
Simbad objects: 4
Number of rows : 4 |
N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2024 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | HD 69830d | Pl | 08 18 23.9469682407 | -12 37 55.817187530 | ~ | 52 | 1 | |||||
2 | HD 69830b | Pl | 08 18 23.9469682407 | -12 37 55.817187530 | ~ | 69 | 1 | |||||
3 | HD 69830 | PM* | 08 18 23.9469682407 | -12 37 55.817187530 | 6.74 | 5.95 | G8:V | 526 | 1 | |||
4 | HD 69830c | Pl | 08 18 23.9469682407 | -12 37 55.817187530 | ~ | 58 | 1 |
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