The Habitability of Planets Orbiting M-dwarf Stars

  title={The Habitability of Planets Orbiting M-dwarf Stars},
  author={Aomawa L. Shields and Sarah Ballard and John Asher Johnson},
  journal={arXiv: Earth and Planetary Astrophysics},
Habitability and Water Loss Limits on Eccentric Planets Orbiting Main-sequence Stars
A planet's climate can be strongly affected by its orbital eccentricity and obliquity. Here we use a 1-dimensional energy balance model modified to include a simple runaway greenhouse (RGH)
The Contribution of M-dwarf Flares to the Thermal Escape of Potentially Habitable Planet Atmospheres
The habitability of planets around M dwarfs (≲0.5 M ⊙) can be affected by the X-rays + extreme UV (XUV) emission of these stars, with flares occasionally increasing the XUV flux by more than 2 orders
Atmospheric escape from the TRAPPIST-1 planets and implications for habitability
The atmospheric escape rates numerically and analytically for the planets of the TRAPPIST-1 system are determined and it is shown that the outer planets are potentially likely to retain their atmospheres over billion-year timescales.
On the detectability of transiting planets orbiting white dwarfs using LSST
White dwarfs are one of the few types of stellar object for which we have yet to confirm the existence of companion planets. Recent evidence for metal contaminated atmospheres, circumstellar debris
The Surface UV Environment on Planets Orbiting M Dwarfs: Implications for Prebiotic Chemistry and the Need for Experimental Follow-up
Potentially-habitable planets orbiting M-dwarfs are of intense astrobiological interest because they are the only rocky worlds accessible to biosignature search over the next 10+ years due to a
Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST
Nine transiting Earth-sized planets have recently been discovered around nearby late M dwarfs, including the TRAPPIST-1 planets and two planets discovered by the MEarth survey, GJ 1132b and LHS
Absence of a thick atmosphere on the terrestrial exoplanet LHS 3844b
Results support theoretical predictions that hot terrestrial planets orbiting small stars may not retain substantial atmospheres, and are well fitted by a bare-rock model with a low Bond albedo.
Galactic habitable zone around M and FGK stars with chemical evolution models that include dust
The Galactic habitable zone is defined as the region with highly enough metallicity to form planetary systems in which Earth-like planets could be born and might be capable of sustaining life
Predicted Number, Multiplicity, and Orbital Dynamics of TESS M-dwarf Exoplanets
  • S. Ballard
  • Physics, Geology
    The Astronomical Journal
  • 2019
We present a study of the M dwarf exoplanetary systems forthcoming from NASA's TESS mission. While the mission's footprint is too complex to be characterized by a single detection completeness, we
Effective temperature – radius relationship of M dwarfs
M-dwarf stars provide very favourable conditions for finding habitable worlds beyond our solar system. The estimation of the fundamental parameters of the transiting exoplanets relies on the accuracy


The Impact of Stellar Rotation on the Detectability of Habitable Planets Around M Dwarfs
Stellar activity and rotation frustrate the detection of exoplanets through the radial velocity technique. This effect is particularly of concern for M dwarfs, which can remain magnetically active
A reappraisal of the habitability of planets around M dwarf stars.
It is concluded that M dwarf stars may indeed be viable hosts for planets on which the origin and evolution of life can occur and it makes sense to include M dwarfs in programs that seek to find habitable worlds and evidence of life.
Tides and the evolution of planetary habitability.
The tidal evolution of hypothetical terrestrial planets around low-mass stars is calculated and it is shown that tides can evolve planets past the inner edge of the habitable zone, sometimes in less than 1 billion years.
Tides, planetary companions, and habitability: habitability in the habitable zone of low-mass stars
Earth-scale planets in the classical habitable zone (HZ) are more likely to be habitable if they possess active geophysics. Without a constant internal energy source, planets cool as they age,
Habitability of terrestrial-mass planets in the HZ of M Dwarfs – I. H/He-dominated atmospheres
The ubiquity of M dwarfs, combined with the relative ease of detecting terrestrial-mass planets around them, has made them prime targets for finding and characterising planets in the "Habitable Zone"
The inner edge of the habitable zone for synchronously rotating planets around low-mass stars using general circulation models
Terrestrial planets at the inner edge of the habitable zone of late-K and M-dwarf stars are expected to be in synchronous rotation, as a consequence of strong tidal interactions with their host
Effects of M dwarf magnetic fields on potentially habitable planets
We investigate the e ect of the magnetic fields of M dwarf (dM) stars on potentially habitable Earth-like planets. These fields can reduce the size of planetary magnetospheres to such an extent that
An Earth-Sized Planet in the Habitable Zone of a Cool Star
The detection of Kepler-186f, a 1.11 ± 0.14 Earth-radius planet that is the outermost of five planets, all roughly Earth-sized, that transit a 0.47 ±0.05 solar-radius star, implying that if Kepler- 186f has an Earth-like atmosphere and water at its surface, then some of this water is likely to be in liquid form.
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.