期刊
ASTRONOMICAL JOURNAL
卷 163, 期 3, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-3881/ac3a06
关键词
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资金
- National Science Foundation [NSF AST-1616636]
- NASA Headquarters under the NASA Earth and Space Science Fellowship Program [80NSSC18K1114]
- NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1801940]
- State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU)
- European Regional Development Fund (FEDER) [AYA2017-88254-P]
- NASA through the NASA Hubble Fellowship - Space Telescope Science Institute [51424]
- NASA [NAS5-26555]
- Alfred P. Sloan Foundation
- U.S. Department of Energy Office of Science
- Center for High Performance Computing at the University of Utah
- Brazilian Participation Group
- Carnegie Institution for Science, Carnegie Mellon University
- Center for Astrophysics \ Harvard Smithsonian
- Chilean Participation Group
- French Participation Group
- Instituto de Astrofisica de Canarias
- Johns Hopkins University
- Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo
- Korean Participation Group
- Lawrence Berkeley National Laboratory
- Leibniz Institut fur Astrophysik Potsdam (AIP)
- Max-Planck-Institut fur Astronomie (MPIA Heidelberg)
- Max-Planck-Institut fur Astrophysik (MPA Garching)
- Max-Planck-Institut fur Extraterrestrische Physik (MPE)
- National Astronomical Observatories of China
- New Mexico State University
- New York University
- University of Notre Dame
- Observatario Nacional/MCTI
- United Kingdom Participation Group
- Universidad Nacional Autonoma de Mexico
- University of Arizona
- University of Colorado Boulder
- University of Oxford
- University of Portsmouth
- University of Utah
- University of Virginia
- University of Washington
- University of Wisconsin
- Vanderbilt University
- Yale University
- National Aeronautics and Space Administration
Chemical abundances of planet-hosting stars provide insight into the composition of planet-forming environments. In this study, we measured the correlation between planet occurrence and chemical abundances for ten different elements. The results show that an enhancement in element abundances corresponds to an increase in planet occurrence, but the trends are weak. We also caution against interpreting trends between planet occurrence and stellar age due to degeneracies caused by Galactic chemical evolution, and make predictions for planet occurrence rates in nearby open clusters to facilitate demographics studies of young planetary systems.
The chemical abundances of planet-hosting stars offer a glimpse into the composition of planet-forming environments. To further understand this connection, we make the first ever measurement of the correlation between planet occurrence and chemical abundances for ten different elements (C, Mg, Al, Si, S, K, Ca, Mn, Fe, and Ni). Leveraging data from the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and Gaia to derive precise stellar parameters (sigma(R star) approximate to 2.3%, sigma(M star) approximate to 4.5%) for a sample of 1018 Kepler Objects of Interest, we construct a sample of well-vetted Kepler planets with precisely measured radii (sigma(Rp) approximate to 3.4%). After controlling for biases in the Kepler detection pipeline and the selection function of the APOGEE survey, we characterize the relationship between planet occurrence and chemical abundance as the number density of nuclei of each element in a star's photosphere raised to a power, beta. varies by planet type, but is consistent within our uncertainties across all ten elements. For hot planets (P = 1-10 days), an enhancement in any element of 0.1 dex corresponds to an increased occurrence of approximate to 20% for super-Earths (R-p = 1-1.9 R-circle plus) and approximate to 60% for sub-Neptunes (R-p = 1.9-4 R-circle plus). Trends are weaker for warm (P = 10-100 days) planets of all sizes and for all elements, with the potential exception of sub-Saturns (R-p = 4-8 R.). Finally, we conclude this work with a caution to interpreting trends between planet occurrence and stellar age due to degeneracies caused by Galactic chemical evolution and make predictions for planet occurrence rates in nearby open clusters to facilitate demographics studies of young planetary systems.
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