They are small worlds after all: revised properties of Kepler M dwarf stars and their planets

By E. Gaidos, A. Mann, A. Kraus, Michael J. Ireland. 2015

132 citations recorded by the source corpus.

This research was supported by NASA grants NNX10AQ36G and NNX11AC33G to EG. EG was also supported by an International Visitor grant from the Swiss National Science Foundation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c4a7cbc396a6ecdec004a77cce9c43d90cd8d0a6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Charbonneau
2. E. Gaidos
3. J. Johnson
4. A. Mann
5. D. Huber
6. Andrew W. Howard
7. Timothy Morton
8. A. Kraus

Citations in the corpus

• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, methodology): “…given in the KSPC for two sets of stars: stars in the California- Kepler Survey (CKS), for which we adopted spectroscopic parameters from Petigura et al. (2017), and stars with Teff < 4000 K with Teff provenances from the KIC, for which we adopted revised Teff values from Gaidos et al. (2016).”
• The CARMENES search for exoplanets around M dwarfs (2018, background): “M stars account for three quarters of all stars known within 10 pc of our Solar System (Henry et al. 2016) and show an occurrence rate in average of more than two planets per host star (Dressing & Charbonneau 2015; Gaidos et al. 2016).”
• Characterization of the K2-18 multi-planetary system with HARPS: A habitable zone super-Earth and discovery of a second, warm super-Earth on a non-coplanar orbit (2017, background): “M dwarfs are also known to frequently host multiple small planets (typically 2.5 planets per star with 0.5 ≤ rp/R⊕ ≤ 4 and within 200 days; Dressing & Charbonneau 2015; Gaidos et al. 2016) thus enabling direct comparative planetology to be conducted on known multi-planet systems.”
• How to Constrain Your M Dwarf. II. The Mass–Luminosity–Metallicity Relation from 0.075 to 0.70 Solar Masses (2018, background): “…significantly more common around M dwarfs than their Sun-like counterparts (Dressing & Charbonneau 2013; Petigura et al. 2013; Mulders et al. 2015; Gaidos et al. 2016) On larger scales, the properties of both the Milky Way and more distant galaxies are inexorably linked to parameters of their…”
• Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes (2016, background): “…of the host stars, often resulting in quite different conclusions as to the radius distribution of the Kepler target stars and thus their transiting planetary companions (see, e.g., Mann et al. 2012; Pinsonneault et al. 2012; Dressing & Charbonneau 2013; Huber et al. 2014; Gaidos et al. 2016).”
• Revised Stellar Properties of Kepler Targets for the Q1-17 (DR25) Transit Detection Run (2016, methodology): “For example, Gaidos et al. (2016) obtained spectra for more than 3,000 dwarfs providing more accurate Teff and logg.”
• SOAR TESS Survey. I. Sculpting of TESS Planetary Systems by Stellar Companions (2019, background): “In general, the identity of the host star for an S-type planet in a close binary is ambiguous (Horch et al. 2014), although there is evidence that typically, the primary is more likely to be the planet host (Gaidos et al. 2016).”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “…for such an effect, based upon the hypothesis that planetesimal chemistry (and indeed, the presence or absence of planets) reflects the composition of oxygen-rich dust inherited from the molecular cloud (Barshay & Lewis, 1976; Bond et al., 2010; Moriarty et al., 2014; Gaidos et al., 2016a).”
• ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “…a few Myr of age, only ∼25% of disks have sufficient reservoirs of dust to form giant planet cores (Mdust & 10 M⊕), in line with the rarity of giant planets seen in the exoplanet population (e.g., Cassan et al. 2012; Fressin et al. 2013; Montet et al. 2014; Bowler et al. 2015; Gaidos et al. 2016).”
• ZODIACAL EXOPLANETS IN TIME (ZEIT). III. A SHORT-PERIOD PLANET ORBITING A PRE-MAIN-SEQUENCE STAR IN THE UPPER SCORPIUS OB ASSOCIATION (2016, methodology): “Most planets around M dwarfs found by Kepler are 1-2.5R⊕ (Morton & Swift 2014; Mulders et al. 2015; Dressing & Charbonneau 2015; Gaidos et al. 2016b), while K2-33b is roughly twice this size at 5.04+0.34−0.37 R⊕.”
• An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “If gas is being depleted in disks (e.g., due to winds) then this may help to explain the lack of gas giants and prevalence of super-Earths seen in the exoplanet population (e.g., Fressin et al. 2013; Gaidos et al. 2016).”