C.D.S. - SIMBAD4 rel 1.7 - 2019.10.23CEST03:20:32

2018MNRAS.479.1651M - Mon. Not. R. Astron. Soc., 479, 1651-1671 (2018/September-2)

Scattering of exocomets by a planet chain: exozodi levels and the delivery of cometary material to inner planets.


Abstract (from CDS):

Exocomets scattered by planets have been invoked to explain observations in multiple contexts, including the frequently found near- and mid-infrared excess around nearby stars arising from exozodiacal dust. Here we investigate how the process of inward scattering of comets originating in an outer belt is affected by the architecture of a planetary system, to determine whether this could lead to observable exozodi levels or deliver volatiles to inner planets. Using N-body simulations, we model systems with different planet mass and orbital spacing distributions in the 1-50 au region. We find that tightly packed (Δap < 20R_H, m_) low-mass planets are the most efficient at delivering material to exozodi regions ( 5-7 per cent of scattered exocomets end up within 0.5 au at some point), although the exozodi levels do not vary by more than a factor of ∼7 for the architectures studied here. We suggest that emission from scattered dusty material in between the planets could provide a potential test for this delivery mechanism. We show that the surface density of scattered material can vary by two orders of magnitude (being highest for systems of low-mass planets with medium spacing), while the exozodi delivery rate stays roughly constant, and that future instruments such as JWST could detect it. In fact for η Corvi, the current Herschel upper limit rules out the scattering scenario by a chain of <=30 M planets. Finally, we show that exocomets could be efficient at delivering cometary material to inner planets ( 0.1-1 per cent of scattered comets are accreted per inner planet). Overall, the best systems at delivering comets to inner planets are the ones that have low-mass outer planets and medium spacing (∼20R_H, m_).

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): methods: numerical - planets and satellites: dynamical evolution and stability - planets and satellites: general - zodiacal dust - circumstellar matter - planetary systems

Simbad objects: 3

goto Full paper

goto View the reference in ADS

Number of rows : 3

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
1 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 452 2
2 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.69 4.31     F2V 270 0
3 * alf Lyr dS* 18 36 56.33635 +38 47 01.2802 0.03 0.03 0.03 0.07 0.10 A0Va 2472 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018MNRAS.479.1651M and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact