Formation and composition of planets around very low mass stars

  title={Formation and composition of planets around very low mass stars},
  author={Yann Alibert and W. Benz},
  journal={Astronomy and Astrophysics},
Context. The recent detection of planets around very low mass stars raises the question of the formation, composition, and potential habitability of these objects. Aims. We use planetary system formation models to infer the properties, in particular their radius distribution and water content, of planets that may form around stars ten times less massive than the Sun. Methods. Our planetary system formation and composition models take into account the structure and evolution of the… Expand

Figures from this paper

Rapid formation of super-Earths around low-mass stars
NASA’s TESS mission is expected to discover hundreds of M dwarf planets. However, few studies focus on how planets form around low-mass stars. We aim to better characterize the formation process of MExpand
Why do more massive stars host larger planets?
Aims. It has been suggested that planetary radii increase with the stellar mass, for planets below 6 R⊕ and host below 1 M . In this study, we explore whether this inferred relation between planetaryExpand
Host Star Dependence of Small Planet Mass–Radius Distributions
The planet formation environment around M dwarf stars is different than around G dwarf stars. The longer hot protostellar phase, activity levels and lower protoplanetary disk mass of M dwarfs all mayExpand
Planet formation and disc mass dependence in a pebble-driven scenario for low-mass stars
Measured disk masses seem to be too low to form the observed population of planetary systems. In this context, we develop a population synthesis code in the pebble accretion scenario, to analyse theExpand
Planetary formation and water delivery in the habitable zone around solar-type stars in different dynamical environments
Context. Observational and theoretical studies suggest that there are many and various planetary systems in the Universe. Aims. We study the formation and water delivery of planets in the habitableExpand
The rate of planet–star coalescences due to tides and stellar evolution
Orbits of close-in planets can shrink significantly due to dissipation of tidal energy in a host star. This process can result in star–planet coalescence within the Galactic lifetime. In someExpand
Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1
The observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST-1, and the six inner planets form a near-resonant chain, such that their orbital periods are near-ratios of small integers. Expand
A water budget dichotomy of rocky protoplanets from 26Al-heating
In contrast to the water-poor planets of the inner Solar System, stochasticity during planetary formation1,2 and order-of-magnitude deviations in exoplanet volatile contents3 suggest that rockyExpand
Pebbles versus planetesimals: the case of Trappist-1
We present a study into the formation of planetary systems around low mass stars similar to Trappist-1, through the accretion of either planetesimals or pebbles. The aim is to determine if theExpand
RedDots: a temperate 1.5 Earth-mass planet candidate in a compact multiterrestrial planet system around GJ 1061
Abstract Small low-mass stars are favourable targets for the detection of rocky habitable planets. In particular, planetary systems in the solar neighbourhood are interesting and suitable for preciseExpand


Extrasolar planet population synthesis. III. Formation of planets around stars of different masses
Aims. We extend the models presented by Mordasini and collaborators to the formation of planets orbiting stars of different masses. We discuss the properties of the resulting synthetic planetExpand
A Decreased Probability of Habitable Planet Formation around Low-Mass Stars
Smaller terrestrial planets (P0.3 M⊕) are less likely to retain the substantial atmospheres and ongoing tectonic activity probably required to support life. A key element in determining whetherExpand
Effect of the stellar spin history on the tidal evolution of close-in planets
We investigate how the evolution of the stellar spin rate affects, and is affected by, planets in close orbits, via star-planet tidal interactions. To do this, we used a standard equilibrium tidalExpand
We have investigated planetary accretion from planetesimals in terrestrial planet regions inside the ice line around M dwarf stars through N-body simulations including tidal interactions with diskExpand
Theoretical models of planetary system formation: mass vs. semi-major axis
Context. Planet formation models have been developed during the past years to try to reproduce what has been observed of both the solar system and the extrasolar planets. Some of these models haveExpand
Planet formation models: the interplay with the planetesimal disc
Context. According to the sequential accretion model (or core-nucleated accretion model), giant planet formation is based first on the formation of a solid core which, when massive enough, canExpand
Models of giant planet formation with migration and disc evolution
We present a new model of giant planet formation that extends the core-accretion model of Pollack et al. (1996, Icarus, 124, 62) to include migration, disc evolution and gap formation. We show thatExpand
Constraining the volatile fraction of planets from transit observations
The determination of the abundance of volatiles in extrasolar planets is very important as it can provide constraints on transport in protoplanetary disks and on the formation location of planets.Expand
Temperate Earth-sized planets transiting a nearby ultracool dwarf star
Observations of three short-period Earth-sized planets transiting an ultracool dwarf star only 12 parsecs away suggest that 11 orbits remain possible for the third planet, the most likely resulting in irradiation significantly less than that received by Earth. Expand
Kepler has found hundreds of Neptune-size (2-6 R{sub +}) planet candidates within 0.5 AU of their stars. The nature of the vast majority of these planets is not known because their masses have notExpand