2018A&A...615A..63O


Query : 2018A&A...615A..63O

2018A&A...615A..63O - Astronomy and Astrophysics, volume 615A, 63-63 (2018/7-1)

Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds.

OGIHARA M., KOKUBO E., SUZUKI T.K. and MORBIDELLI A.

Abstract (from CDS):


Context. Planets with masses larger than about 0.1 M undergo rapid inward migration (type I migration) in a standard protoplanetary disk. Recent magnetohydrodynamical simulations revealed the presence of magnetically driven disk winds, which would alter the disk profile and the type I migration in the close-in region.
Aims. We investigate orbital evolution of planetary embryos in disks that viscously evolve under the effects of disk winds. The aim is to discuss effects of altered disk profiles on type I migration. In addition, we aim to examine whether observed distributions of close-in super-Earths can be reproduced by simulations that include effects of disk winds.
Methods. We perform N-body simulations of super-Earth formation from planetary embryos, in which a recent model for disk evolution is used. We explore a wide range of parameters and draw general trends. We also carry out N-body simulations of close-in super-Earth formation from embryos in such disks under various conditions.
Results. We find that the type I migration is significantly suppressed in many cases. Even in cases in which inward migration occurs, the migration timescale is lengthened to 1Myr, which mitigates the type I migration problem. This is because the gas surface density is decreased and has a flatter profile in the close-in region due to disk winds. We find that when the type I migration is significantly suppressed, planets undergo late orbital instability during the gas depletion, leading to a non-resonant configuration. We also find that observed distributions of close-in super-Earths (e.g., period ratio, mass ratio) can be reproduced. In addition, we show that in some results of simulations, systems with a chain of resonant planets, like the TRAPPIST-1 system, form.

Abstract Copyright: © ESO 2018

Journal keyword(s): planets and satellites: formation - protoplanetary disks - planet-disk interactions - methods: numerical

Simbad objects: 4

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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 - 2022
#notes
1 Kepler-60 Ro* 19 15 50.6983640712 +42 15 54.050260968           ~ 90 1
2 Kepler-80 Ro* 19 44 27.0200680656 +39 58 43.594100688           M0V 112 1
3 Kepler-223 Ro* 19 53 16.4202435936 +47 16 46.308434088     15 15.78   ~ 124 1
4 TRAPPIST-1 LM* 23 06 29.3684948589 -05 02 29.037301866     18.798 16.466 14.024 M7.5e 757 0

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2022.09.30-19:30:26

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