期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 478, 期 4, 页码 4866-4880出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1390
关键词
asteroseismology; planets and satellites: composition; planets and satellites: formation; planets and satellites: fundamental parameters
资金
- ESO-3.6m telescope at La Silla Observatory [0100.C-0808]
- NASA Exoplanet Exploration Program
- NASA Ames Research Center
- European Union's Horizon 2020 research and innovation programme [730890]
- Programma Giovani Ricercatori - Rita Levi Montalcini - Rientro dei Cervelli - Italian Ministry of Education, Universities and Research (MIUR)
- Ramon y Cajal fellowship [RYC-2015-17697]
- Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant [4181-00487B]
- DFG priority program [SPP 1992, HA 3279/12-1, PA 525/18-1, PA5 25/19-1, PA525/20-1, RA 714/14-1]
- MINECO [ESP2015-65712-C5-4-R, AYA2016-76378-P]
- Ministry of Economy and Competitiveness
- FEDER funds [IACA13-3E-2493]
- Swedish National Space Board
- CNES PLATO grant
- MINECO-programme 'Juan de la Cierva Incorporacion' [IJCI-2015-26034]
- ERC through SPIRE grant [647383]
- ISSI through the ENCELADE 2.0 team
- VILLUM FONDEN [10118]
- ESA-PRODEX programme
- Danish National Research Foundation [DNRF106]
- European Research Council (ERC) [647383] Funding Source: European Research Council (ERC)
We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding themass and radius to be 1.12(-0.01)(+0.04) and 1.657(-0.004)(+0.020)R(circle dot), respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4(-1.3)(+0.4)Gyr, and the non-detection of mixed modes. The star hosts a 'warm Saturn' (P = 11.8 d, R-p = 6.86 +/- 0.14 R-circle plus). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 +/- 3.3 M-circle plus. The data also show that the planet's orbit is eccentric (e approximate to 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter-McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity.
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