Farmer, R.; Kolb, U. and Norton, A. J.
(2013).
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| DOI (Digital Object Identifier) Link: | https://doi.org/10.1093/mnras/stt795 |
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| Google Scholar: | Look up in Google Scholar |
Abstract
Using population synthesis tools we create a synthetic Kepler Input Catalogue (KIC) and subject it to the Kepler Stellar Classification Program (SCP) method for deter- mining stellar parameters such as the effective temperature Teff and surface gravity g. We achieve a satisfactory match between the synthetic KIC and the real KIC in the log g vs log Teff diagram,while there is a significant difference between the actual physical stellar parameters and those derived by the SCP of the stars in the synthetic sample. We find a median difference ∆Teff = +500 K and ~ ∆ log g = −0.2 dex for main-sequence stars, and ~ ∆Teff = +50 K and ∆ log g = −0.5 dex for giants, although there is a large variation across parameter space. For a MS star the median difference in g would equate to a ~ 3% increase in stellar radius and a consequent 3% overestimate of the radius for any transiting exoplanet. We find no significant difference between ∆Teff and ∆ log g for single stars and the primary star in a binary system. We also re-created the Kepler target selection method and found that the binary fraction is unchanged by the target selection. Binaries are selected in similar proportions to single star systems; the fraction of MS dwarfs in the sample increases from about 75% to 80%, and the giant star fraction decreases from 25% to 20%.
| Item Type: | Journal Item |
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| Copyright Holders: | 2013 RAS |
| ISSN: | 1365-2966 |
| Keywords: | binaries - general; Galaxy - stellar content; planetary systems; stars - evolution; stars - statistics; surveys |
| Academic Unit/School: | Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences Faculty of Science, Technology, Engineering and Mathematics (STEM) |
| Item ID: | 37049 |
| Depositing User: | Ulrich Kolb |
| Date Deposited: | 03 Apr 2013 10:55 |
| Last Modified: | 04 Dec 2019 19:25 |
| URI: | http://oro.open.ac.uk/id/eprint/37049 |
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