TY - JOUR
T1 - Planetary systems in a star cluster II
T2 - Intermediate-mass black holes and planetary systems
AU - Flammini Dotti, Francesco
AU - Kouwenhoven, M. B.N.
AU - Shu, Qi
AU - Hao, Wei
AU - Spurzem, Rainer
N1 - Publisher Copyright:
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2020/9/1
Y1 - 2020/9/1
N2 - Most stars form in dense stellar environments. It is speculated that some dense star clusters may host intermediate-mass black holes (IMBHs), which may have formed from runaway collisions between high-mass stars, or from the mergers of less massive black holes. Here, we numerically explore the evolution of populations of planets in star clusters with an IMBH. We study the dynamical evolution of single-planet systems and free-floating planets, over a period of 100 Myr, in star clusters without an IMBH, and in clusters with a central IMBH of mass 100 M ⊙ or 200 M⊙. In the central region (r ≲ 0.2 pc), the IMBH's tidal influence on planetary systems is typically 10 times stronger than the average neighbour star. For a star cluster with a 200 M⊙ IMBH, the region in which the IMBH's influence is stronger within the virial radius (∼1 pc). The IMBH quenches mass segregation, and the stars in the core tend to move towards intermediate regions. The ejection rate of both stars and planets is higher when an IMBH is present. The rate at which planets are expelled from their host star rate is higher for clusters with higher IMBH masses, for t < 0.5trh, while remains mostly constant while the star cluster fills its Roche lobe, similar to a star cluster without an IMBH. The disruption rate of planetary systems is higher in initially denser clusters, and for wider planetary orbits, but this rate is substantially enhanced by the presence of a central IMBH.
AB - Most stars form in dense stellar environments. It is speculated that some dense star clusters may host intermediate-mass black holes (IMBHs), which may have formed from runaway collisions between high-mass stars, or from the mergers of less massive black holes. Here, we numerically explore the evolution of populations of planets in star clusters with an IMBH. We study the dynamical evolution of single-planet systems and free-floating planets, over a period of 100 Myr, in star clusters without an IMBH, and in clusters with a central IMBH of mass 100 M ⊙ or 200 M⊙. In the central region (r ≲ 0.2 pc), the IMBH's tidal influence on planetary systems is typically 10 times stronger than the average neighbour star. For a star cluster with a 200 M⊙ IMBH, the region in which the IMBH's influence is stronger within the virial radius (∼1 pc). The IMBH quenches mass segregation, and the stars in the core tend to move towards intermediate regions. The ejection rate of both stars and planets is higher when an IMBH is present. The rate at which planets are expelled from their host star rate is higher for clusters with higher IMBH masses, for t < 0.5trh, while remains mostly constant while the star cluster fills its Roche lobe, similar to a star cluster without an IMBH. The disruption rate of planetary systems is higher in initially denser clusters, and for wider planetary orbits, but this rate is substantially enhanced by the presence of a central IMBH.
KW - planetary systems
KW - planets and satellites: Dynamical evolution and stability
KW - stars: Solar-type
KW - stars: Statistics
UR - http://www.scopus.com/inward/record.url?scp=85096981427&partnerID=8YFLogxK
U2 - 10.1093/mnras/staa2188
DO - 10.1093/mnras/staa2188
M3 - Article
AN - SCOPUS:85096981427
SN - 0035-8711
VL - 497
SP - 3623
EP - 3637
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -