Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog

Narang, Mayank; Manoj, P.; Furlan, E.; Mordasini, Christoph; Henning, Thomas; Mathew, Blesson; Banyal, Ravinder K.; Sivarani, T. (2018). Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog. The astronomical journal, 156(5), p. 221. American Astronomical Society 10.3847/1538-3881/aae391

Preview	Text 1809.08385.pdf - Draft Version Available under License Publisher holds Copyright. Download (1MB) | Preview
Preview	Text Narang_2018_AJ_156_221.pdf - Published Version Available under License Publisher holds Copyright. Download (5MB) | Preview

Correlations between the occurrence rate of exoplanets and their host star properties provide important clues about the planet formation processes. We studied the dependence of the observed properties of exoplanets (radius, mass, and orbital period) as a function of their host star metallicity. We analyzed the planetary radii and orbital periods of over 2800 Kepler candidates from the latest Kepler data release DR25 (Q1-Q17) with revised planetary radii based on Gaia~DR2 as a function of host star metallicity (from the Q1-Q17 (DR25) stellar and planet catalog). With a much larger sample and improved radius measurements, we are able to reconfirm previous results in the literature. We show that the average metallicity of the host star increases as the radius of the planet increases. We demonstrate this by first calculating the average host star metallicity for different radius bins and then supplementing these results by calculating the occurrence rate as a function of planetary radius and host star metallicity. We find a similar trend between host star metallicity and planet mass: the average host star metallicity increases with increasing planet mass. This trend, however, reverses for masses >4.0MJ: host star metallicity drops with increasing planetary mass. We further examined the correlation between the host star metallicity and the orbital period of the planet. We find that for planets with orbital periods less than 10 days, the average metallicity of the host star is higher than that for planets with periods greater than 10 days.

Interest & Impact

Downloads

360 since deposited on 13 Jun 2019
38 in the past 12 months

Citations

5 Citations in Web of Science ®
6 Citations in Scopus

Search

in Google Scholar™

Services

Actions (login required)

Edit item

Actions (login required)

Edit item