2021A&A...656A.115H


Query : 2021A&A...656A.115H

2021A&A...656A.115H - Astronomy and Astrophysics, volume 656A, 115-115 (2021/12-1)

Kepler-223 resonance holds information about turbulence during the gas-disk phase.

HUHN L.-A., PICHIERRI G., BITSCH B. and BATYGIN K.

Abstract (from CDS):


Context. Planet formation remains an open field of research, and many fundamental physical processes regarding planetary formation in protoplanetary disks are still imperfectly understood. It remains to be investigated how different conditions in these protoplanetary disks affect the emergence of different types of observed systems. An elusive phenomenon is the turbulence in these disks. Observations are available of planetary systems and of some protoplanetary disks, which can serve as a starting point for these investigations. The detected systems reveal different architectures of planets. One particularly interesting case to consider is the Kepler-223 system, which contains a rare configuration of four planets in a resonance chain. This implies a certain migration history.
Aims. We aim to use the orbital configuration of the Kepler-223 planets to constrain the parameters of the protoplanetary disk that allow the formation of a chain of mean-motion resonances that resembles the resonances of Kepler-223. We primarily investigate the disk viscosity and surface density.
Methods. We used the swift_symbaN-body integrator with additional dissipative forces to mimic planet-disk interactions.
Results. We constrained the surface densities and viscosities that allow the formation of a resonant chain like that of Kepler-223. We find that surface densities of up to a few minimum mass solar nebula surface densities and disk viscosity parameters α of a few x 10–3 up to x 10–2 are most successful at reproducing the architecture of this particular planetary system. We describe the connection of these two quantities with each other, considering the success of reproducing the chain. We find that higher disk surface densities in turn require lower viscosities to build the chain.
Conclusions. Our results show that well-characterized observed planetary systems hold information about their formation conditions in the protoplanetary disks and that it is possible to extract this information, namely the initial disk surface density and viscosity. This helps to constrain planet formation.

Abstract Copyright: © L.-A. Hühn et al. 2021

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

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 Kepler-223 Ro* 19 53 16.4202435936 +47 16 46.308434088     15 15.78   ~ 129 1
2 Kepler-223b Pl 19 53 16.4203115605 +47 16 46.308061008           ~ 26 0
3 Kepler-223c Pl 19 53 16.4203115605 +47 16 46.308061008           ~ 27 0
4 Kepler-223d Pl 19 53 16.4203115605 +47 16 46.308061008           ~ 36 0
5 Kepler-223e Pl 19 53 16.4203115605 +47 16 46.308061008           ~ 30 0
6 BD-15 6290 BY* 22 53 16.7325836486 -14 15 49.304052185 12.928 11.749 10.192 9.013 7.462 M3.5V 955 1
7 TRAPPIST-1 LM* 23 06 29.3684948589 -05 02 29.037301866     18.798 16.466 14.024 M7.5e 811 0

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2023.01.30-23:26:51

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