Formation and composition of planets around very low mass stars

@article{Alibert2016FormationAC,
  title={Formation and composition of planets around very low mass stars},
  author={Yann Alibert and W. Benz},
  journal={Astronomy and Astrophysics},
  year={2016},
  volume={598}
}
  • Y. AlibertW. Benz
  • Published 11 October 2016
  • Physics, Geology
  • 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… 

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

Why do more massive stars host larger planets?

Aims. It has been suggested that planetary radii increase with stellar mass for planet sizes smaller than 6 R⊕ and host masses lower than 1 M⊙. In this study, we explore whether this inferred

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 may

Planet formation and disc mass dependence in a pebble-driven scenario for low-mass stars

Measured disc 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

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 habitable

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.

Density, not radius, separates rocky and water-rich small planets orbiting M dwarf stars

Exoplanets smaller than Neptune are common around red dwarf stars (M dwarfs), with those that transit their host star constituting the bulk of known temperate worlds amenable for atmospheric

A tale of planet formation: from dust to planets

  • Beibei LiuJ. Ji
  • Geology, Physics
    Research in Astronomy and Astrophysics
  • 2020
The characterization of exoplanets and their birth protoplanetary disks has enormously advanced in the last decade. Benefitting from that, our global understanding of the planet formation processes

Observational constraints on the likelihood of 26Al in planet-forming environments

  • M. Reiter
  • Physics, Geology
    Astronomy & Astrophysics
  • 2020
Recent work suggests that 26Al may determine the water budget in terrestrial exoplanets as its radioactive decay dehydrates planetesimals leading to rockier compositions. Here I consider the observed

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 rocky

References

SHOWING 1-10 OF 35 REFERENCES

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 planet

A Decreased Probability of Habitable Planet Formation around Low-Mass Stars

Smaller terrestrial planets (≲0.3 M⊕) are less likely to retain the substantial atmospheres and ongoing tectonic activity probably required to support life. A key element in determining whether

N-BODY SIMULATIONS OF PLANETARY ACCRETION AROUND M DWARF STARS

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 disk

FORMATION AND STRUCTURE OF LOW-DENSITY EXO-NEPTUNES

Kepler has found hundreds of Neptune-size (2–6 R⊕) 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 not been

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 have

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 that

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.

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.

Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations

We study the dependence of protoplanetary disk evolution on stellar mass using a large sample of young stellar objects in nearby young star-forming regions. We update the protoplanetary disk

Planets Formed in Habitable Zones of M Dwarf Stars Probably Are Deficient in Volatiles

Dynamical considerations, presented herein via analytic scalings and numerical experiments, imply that Earth-mass planets accreting in regions that become habitable zones of M dwarf stars form within