A Distinct Population of Small Planets: Sub-Earths

  title={A Distinct Population of Small Planets: Sub-Earths},
  author={Yansong 岩松 Qian 钱 and Yan-Qing 燕庆 Wu 武},
  journal={The Astronomical Journal},
The sizes of small planets are known to be bimodal, with a gap separating planets that have lost their primordial atmospheres (super-Earths) and the ones that retain them (mini-Neptunes). Here, we report evidence for another distinct population at smaller sizes. By focusing on planets orbiting around GK dwarfs inward of 16 days and correcting for observational completeness, we find that the number of super-Earths peaks around 1.4 Earth radii and disappears shortly below this size. Instead, a… 
1 Citations

Super-Earths and Sub-Neptunes Are Insensitive to Stellar Metallicity

Kepler planets (including super-Earths and sub-Neptunes, from 1–4 Earth radii) are likely formed before the gaseous protoplanetary disks have dissipated, as are the Jovian planets. If the metal



Formation of Ultra-short-period Planets by Obliquity-driven Tidal Runaway

Small, rocky planets have been found orbiting in extreme proximity to their host stars, sometimes down to only ∼2 stellar radii. These ultra-short-period planets (USPs) likely did not form in their

Ultra-short-period Planets in K2. III. Neighbors are Common with 13 New Multiplanet Systems and 10 Newly Validated Planets in Campaigns 0–8 and 10

Using the EVEREST photometry pipeline, we have identified 74 candidate ultra-short-period planets (USPs; orbital period P < 1 day) in the first half of the K2 data (Campaigns 0–8 and 10). Of these,

Kepler-62f: Kepler's first small planet in the habitable zone, but is it real?

A Joint Mass–Radius–Period Distribution of Exoplanets

The radius–period distribution of exoplanets has been characterized by the Kepler survey, and the empirical mass–radius relation by the subset of Kepler planets with mass measurements. We combine the

Mass and Mass Scalings of Super-Earths

  • Yanqin Wu
  • Physics, Geology
    The Astrophysical Journal
  • 2019
The majority of the transiting planets discovered by the Kepler mission (called super-Earths here, includes the so-called “sub-Neptunes”) orbit close to their stars. As such, photoevaporation of

The Gaia–Kepler Stellar Properties Catalog. II. Planet Radius Demographics as a Function of Stellar Mass and Age

Studies of exoplanet demographics require large samples and precise constraints on exoplanet host stars. Using the homogeneous Kepler stellar properties derived using the Gaia Data Release 2 by

The Gaia–Kepler Stellar Properties Catalog. I. Homogeneous Fundamental Properties for 186,301 Kepler Stars

An accurate and precise Kepler Stellar Properties Catalog is essential for the interpretation of the Kepler exoplanet survey results. Previous Kepler Stellar Properties Catalogs have focused on

Occurrence Rates of Planets Orbiting FGK Stars: Combining Kepler DR25, Gaia DR2, and Bayesian Inference

We characterize the occurrence rate of planets, ranging in size from 0.5 to 16 R⊕, orbiting FGK stars with orbital periods from 0.5 to 500 days. Our analysis is based on results from the “DR25”

Measuring Transit Signal Recovery in the Kepler Pipeline. IV. Completeness of the DR25 Planet Candidate Catalog

In this work we empirically measure the detection efficiency of the Kepler pipeline used to create the final Kepler threshold crossing event and planet candidate catalogs, a necessary ingredient for