2021A&A...656A..72B


Query : 2021A&A...656A..72B

2021A&A...656A..72B - Astronomy and Astrophysics, volume 656A, 72-72 (2021/12-1)

The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars.

BURN R., SCHLECKER M., MORDASINI C., EMSENHUBER A., ALIBERT Y., HENNING T., KLAHR H. and BENZ W.

Abstract (from CDS):


Context. Previous theoretical works on planet formation around low-mass stars have often been limited to large planets and individual systems. As current surveys routinely detect planets down to terrestrial size in these systems, models have shifted toward a more holistic approach that reflects their diverse architectures.
Aims. Here, we investigate planet formation around low-mass stars and identify differences in the statistical distribution of modeled planets. We compare the synthetic planet populations to observed exoplanets and we discuss the identified trends.
Methods. We used the Generation III Bern global model of planet formation and evolution to calculate synthetic populations, while varying the central star from Solar-like stars to ultra-late M dwarfs. This model includes planetary migration, N-body interactions between embryos, accretion of planetesimals and gas, and the long-term contraction and loss of the gaseous atmospheres.
Results. We find that temperate, Earth-sized planets are most frequent around early M dwarfs (0.3 M-0.5 M) and that they are more rare for Solar-type stars and late M dwarfs. The planetary mass distribution does not linearly scale with the disk mass. The reason behind this is attributed to the emergence of giant planets for M* ≥ 0.5 M, which leads to the ejection of smaller planets. Given a linear scaling of the disk mass with stellar mass, the formation of Earth-like planets is limited by the available amount of solids for ultra-late M dwarfs. For M* ≥ 0.3 M, however, there is sufficient mass in the majority of systems, leading to a similar amount of Exo-Earths going from M to G dwarfs. In contrast, the number of super-Earths and larger planets increases monotonically with stellar mass. We further identify a regime of disk parameters that reproduces observed M-dwarf systems such as TRAPPIST-1. However, giant planets around late M dwarfs, such as GJ 3512b, only form when type I migration is substantially reduced.
Conclusions. We are able to quantify the stellar mass dependence of multi-planet systems using global simulations of planet formation and evolution. The results fare well in comparison to current observational data and predict trends that can be tested with future observations.

Abstract Copyright: © R. Burn et al. 2021

Journal keyword(s): planetary systems - protoplanetary disks - planets and satellites: formation - planets and satellites: composition - planets and satellites: dynamical evolution and stability - stars: low-mass

Simbad objects: 23

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Number of rows : 23
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 NAME G 268-38c Pl 00 44 59.3314993038 -15 16 17.543124886           ~ 50 0
2 NAME G 268-38b Pl 00 44 59.3314993038 -15 16 17.543124886           ~ 145 0
3 NAME 2MASS J02192210-3925225b Pl 02 19 22.1105002404 -39 25 22.520274475           ~ 10 0
4 [BCG93] 1 TT* 04 14 17.6095515480 +28 06 09.654704388 18.04         M4.5 94 0
5 Wolf 1539 PM* 04 52 05.7321216445 +06 28 35.588676189 14.791 13.568 12.018 10.854 9.334 M2V 148 1
6 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2207 1
7 NGC 2264 OpC 06 40 52 +09 52.6           ~ 1730 0
8 NGC 2362 OpC 07 18 41 -24 57.2           ~ 396 0
9 NGC 2547 OpC 08 09 52.360 -49 10 35.01           ~ 377 0
10 K2-146 LM* 08 40 06.4242250368 +19 05 34.430759088   17.87 16.25 15.97   M3.0V 30 0
11 L 675-81 PM* 08 40 59.2057867166 -23 27 22.592748045   13.2 11.975 11.637 9.37 M3.5V 131 1
12 G 234-45 PM* 08 41 20.1286588424 +59 29 50.444062516   16.98   14.1   dM5.5 66 0
13 NAME G 234-45b Pl 08 41 20.1289475639 +59 29 50.444849212           ~ 18 0
14 NAME L 320-124b Pl 10 14 51.7783473599 -47 09 24.189733387           ~ 141 0
15 NAME Proxima Centauri b Pl 14 29 42.9451234609 -62 40 46.170818907           ~ 320 0
16 BD-07 4003 BY* 15 19 26.8269387505 -07 43 20.189497466 13.403 11.76 10.560 9.461 8.911 M3V 601 2
17 NAME Upper Sco Association As* 16 12 -23.4           ~ 1252 1
18 NAME G 139-21b Pl 17 15 18.9337265994 +04 57 50.064695682           ~ 653 1
19 NGC 6530 OpC 18 04 31 -24 21.5           ~ 400 0
20 BD-05 5715 PM* 22 09 40.3443137051 -04 38 26.650757960 13.006 11.868 10.366 9.279 7.877 M3.5V 261 1
21 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
22 TRAPPIST-1b Pl 23 06 29.3684052886 -05 02 29.031690445           ~ 197 0
23 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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2023.01.30-22:43:41

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