PROBABILISTIC FORECASTING OF THE MASSES AND RADII OF OTHER WORLDS

@article{Chen2016PROBABILISTICFO,
  title={PROBABILISTIC FORECASTING OF THE MASSES AND RADII OF OTHER WORLDS},
  author={Jingjing Chen and David M. Kipping},
  journal={The Astrophysical Journal},
  year={2016},
  volume={834},
  pages={17}
}
Mass and radius are two of the most fundamental properties of an astronomical object. Increasingly, new planet discoveries are being announced with a measurement of one of these terms, but not both. This has led to a growing need to forecast the missing quantity using the other, especially when predicting the detectability of certain follow-up observations. We present am unbiased forecasting model built upon a probabilistic mass-radius relation conditioned on a sample of 316 well-constrained… 

Figures from this paper

Forecasting the detectability of known radial velocity planets with the upcoming CHEOPS mission
The Characterizing Exoplanets Satellite (CHEOPS) mission is planned for launch next year with a major objective being to search for transits of known RV planets, particularly those orbiting bright
An Empirical Mass–Radius Relation for Cool Giant Planets
Probabilistic relationships between the mass and radius of planets are useful for a variety of purposes, including estimating the yields of planet discovery efforts and the radii of discovered
Two empirical regimes of the planetary mass-radius relation
Today, with the large number of detected exoplanets and improved measurements, we can reach the next step of planetary characterization. Classifying different populations of planets is not only
Unbiased inference of the masses of transiting planets from radial velocity followup
Data from the TESS mission will be used to discover hundreds of small planets amenable to radial velocity (RV) followup. Often, RV observations are obtained until a particular fractional precision on
Predicting exoplanet mass from radius and incident flux: a Bayesian mixture model
The relationship between mass and radius (M-R relation) is the key for inferring the planetary compositions and thus valuable for the studies of formation and migration models. However, the M-R
Estimating Planetary Mass with Deep Learning
While thousands of exoplanets have been confirmed, the known properties about individual discoveries remain sparse and depend on detection technique. To utilize more than a small section of the
Beyond the exoplanet mass-radius relation
Context. Mass and radius are two fundamental properties for characterising exoplanets, but only for a relatively small fraction of exoplanets are they both available. Mass is often derived from
Mass–Radius Relationship for M Dwarf Exoplanets: Comparing Nonparametric and Parametric Methods
M dwarfs, though the most abundant star in the galaxy, form only a small subset of stellar hosts with exoplanets with measured radii and masses. In this paper we analyze the Mass-Radius (M-R)
Searching the Entirety of Kepler Data. II. Occurrence Rate Estimates for FGK Stars
We present exoplanet occurrence rates estimated with approximate Bayesian computation for planets with radii between 0.5 and 16 $R_{\bigoplus}$ and orbital periods between 0.78 and 400 days, orbiting
The Mass Budgets and Spatial Scales of Exoplanet Systems and Protoplanetary Disks
Planets are born from disks of gas and dust, and observations of protoplanetary disks are used to constrain the initial conditions of planet formation. However, dust mass measurements of Class II
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 203 REFERENCES
Probabilistic Mass-Radius Relationship for Sub-Neptune-Sized Planets
The Kepler Mission has discovered thousands of planets with radii $<4\ R_\oplus$, paving the way for the first statistical studies of the dynamics, formation, and evolution of these sub-Neptunes and
An accurate mass and radius measurement for an ultracool white dwarf
Studies of cool white dwarfs in the solar neighbourhood have placed a limit on the age of the Galactic disc of 8–9 billion years. However, determining their cooling ages requires the knowledge of
Exoplanet population inference and the abundance of Earth analogs from noisy, incomplete catalogs
No true extrasolar Earth analog is known. Hundreds of planets have been found around Sun-like stars that are either Earth-sized but on shorter periods, or else on year-long orbits but somewhat
Masses, Radii, and Orbits of Small Kepler Planets: The Transition From Gaseous to Rocky Planets
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise
The size distribution of inhabited planets
Earth-like planets are expected to provide the greatest opportunity for the detection of life beyond the Solar system. However, our planet cannot be considered a fair sample, especially if
Accurate masses and radii of normal stars: modern results and applications
This article presents and discusses a critical compilation of accurate, fundamental determinations of stellar masses and radii. We have identified 95 detached binary systems containing 190 stars (94
MOST 1.6 EARTH-RADIUS PLANETS ARE NOT ROCKY
The Kepler mission, combined with ground-based radial velocity (RV) follow-up and dynamical analyses of transit timing variations, has revolutionized the observational constraints on
A simple, quantitative method to infer the minimum atmospheric height of small exoplanets
Amongst the many hundreds of transiting planet candidates discovered by the Kepler Mission, one finds a large number of candidates with sizes between that of the Earth and Neptune. The composition of
UNDERSTANDING THE MASS-RADIUS RELATION FOR SUB-NEPTUNES: RADIUS AS A PROXY FOR COMPOSITION
Transiting planet surveys like Kepler have provided a wealth of information on the distribution of planetary radii, particularly for the new populations of super-Earth- and sub-Neptune-sized planets.
The Mass-Radius(-Rotation?) Relation for Low-Mass Stars
The fundamental properties of low-mass stars are not as well understood as those of their more massive counterparts. The best method for constraining these properties, especially masses and radii, is
...
1
2
3
4
5
...