期刊
ASTRONOMICAL JOURNAL
卷 152, 期 6, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/0004-6256/152/6/204
关键词
planets and satellites: formation; planets and satellites: individual (Kepler-21b); stars:individual (HD 179070); techniques: photometric; techniques: radial velocities; techniques: spectroscopic
资金
- Prodex Program of the Swiss Space Office (SSO)
- Harvard University Origins of Life Initiative (HUOLI)
- Scottish Universities Physics Alliance (SUPA)
- University of Geneva
- Smithsonian Astrophysical Observatory (SAO)
- Italian National Astrophysical Institute (INAF)
- University of St. Andrews
- Queens University Belfast
- University of Edinburgh
- John Templeton Foundation
- National Aeronautics and Space Administration [NNX15AC9OG]
- European Union Seventh Framework Programme (FP7) [313014]
- NASA through the Sagan Fellowship Program
- Fundacao para a Ciencias e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013]
- POPH/FSE (EC) by FEDER funding through the program Programa Operacional de Factores de Competitividade COMPETE
- Simons Foundation (SCOL) [337090]
- NSF Graduate Research Fellowship [DGE 1144152]
- Society in Science-Branco Weiss Fellowship
- [IF/01037/2013CP1191/CT0001]
- STFC [ST/M001296/1, PP/D000890/1, ST/L00139X/1, ST/G001006/1, ST/I000666/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D000890/1, ST/G001006/1, 1105238, ST/I000666/1, ST/L00139X/1, ST/M001296/1] Funding Source: researchfish
HD 179070, aka Kepler-21, is a V = 8.25 F6IV star and the brightest exoplanet host discovered by Kepler. An early detailed analysis by Howell et al. of the first 13 months (Q0-Q5) of Kepler light curves revealed transits of a planetary companion, Kepler-21b, with a radius of about 1.60 +/- 0.04 R(circle plus)and an orbital period of about 2.7857 days. However, they could not determine the mass of the planet from the initial radial velocity (RV) observations with Keck-HIRES, and were only able to impose a 2 sigma upper limit of 10 M-circle plus. Here, we present results from the analysis of 82 new RV observations of this system obtained with HARPS-N, together with the existing 14 HIRES data points. We detect the Doppler signal of Kepler-21b with a RV semiamplitude K = 2.00 +/- 0.65 m s(-1), which corresponds to a planetary mass of 5.1 +/- 1.7 M-circle plus. We also measure an improved radius for the planet of 1.639 +0.019/-0.015 R-circle plus, in agreement with the radius reported by Howell et al. We conclude that Kepler-21b, with a density of 6.4 +/- 2.1 g cm(-3), belongs to the population of small, less than or similar to 6 Me planets with iron and magnesium silicate interiors, which have lost the majority of their envelope volatiles via stellar winds or gravitational escape. The RV analysis presented in this paper serves as an example of the type of analysis that will be necessary to confirm the masses of TESS small planet candidates.
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