TY - JOUR
T1 - Constraining the initial planetary population in the gravitational instability model
AU - Humphries, J.
AU - Vazan, A.
AU - Bonavita, M.
AU - Helled, R.
AU - Nayakshin, S.
N1 - Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
PY - 2019/10/1
Y1 - 2019/10/1
N2 - Direct imaging (DI) surveys suggest that gas giants beyond 20 au are rare around FGK stars. However, it is not clear what this means for the formation frequency of gravitational instability (GI) protoplanets due to uncertainties in gap opening and migration efficiency. Here we combine state-of-the-art calculations of homogeneous planet contraction with a population synthesis code. We find DI constraints to be satisfied if protoplanet formation by GI occurs in tens of per cent of systems if protoplanets 'supermigrate' to small separations. In contrast, GI may occur in only a few per cent of systems if protoplanets remain stranded at wide orbits because their migration is 'quenched' by efficient gap opening. We then use the frequency of massive giants in radial velocity surveys inside 5 au to break this degeneracy - observations recently showed that this population does not correlate with the host star metallicity and is therefore suspected to have formed via GI followed by inward migration. We find that only the supermigration scenario can sufficiently explain this population while simultaneously satisfying the DI constraints and producing the right mass spectrum of planets inside 5 au. If massive gas giants inside 5 au formed via GI, then our models imply that migration must be efficient and that the formation of GI protoplanets occurs in at least tens of per cent of systems.
AB - Direct imaging (DI) surveys suggest that gas giants beyond 20 au are rare around FGK stars. However, it is not clear what this means for the formation frequency of gravitational instability (GI) protoplanets due to uncertainties in gap opening and migration efficiency. Here we combine state-of-the-art calculations of homogeneous planet contraction with a population synthesis code. We find DI constraints to be satisfied if protoplanet formation by GI occurs in tens of per cent of systems if protoplanets 'supermigrate' to small separations. In contrast, GI may occur in only a few per cent of systems if protoplanets remain stranded at wide orbits because their migration is 'quenched' by efficient gap opening. We then use the frequency of massive giants in radial velocity surveys inside 5 au to break this degeneracy - observations recently showed that this population does not correlate with the host star metallicity and is therefore suspected to have formed via GI followed by inward migration. We find that only the supermigration scenario can sufficiently explain this population while simultaneously satisfying the DI constraints and producing the right mass spectrum of planets inside 5 au. If massive gas giants inside 5 au formed via GI, then our models imply that migration must be efficient and that the formation of GI protoplanets occurs in at least tens of per cent of systems.
KW - Accretion
KW - Accretion discs
KW - Brown dwarfs
KW - Planet-disc interactions
KW - Planets and satellites: composition
KW - Planets and satellites: formation
KW - Protoplanetary discs
UR - http://www.scopus.com/inward/record.url?scp=85083157953&partnerID=8YFLogxK
U2 - 10.1093/mnras/stz2006
DO - 10.1093/mnras/stz2006
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AN - SCOPUS:85083157953
SN - 0035-8711
VL - 488
SP - 4873
EP - 4889
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -