The Transiting Multi-planet System HD15337 : Two Nearly Equal-mass Planets Straddling the Radius Gap
(2019) In Astrophysical Journal Letters 876(2).- Abstract
We report the discovery of a super-Earth and a sub-Neptune transiting the star HD 15337 (TOI-402, TIC 120896927), a bright (V = 9) K1 dwarf observed by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 3 and 4. We combine the TESS photometry with archival High Accuracy Radial velocity Planet Searcher spectra to confirm the planetary nature of the transit signals and derive the masses of the two transiting planets. With an orbital period of 4.8 days, a mass of and a radius of 1.64 ± 0.06 R ⊕, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of , and a radius of 2.39 ± 0.12 R... (More)
We report the discovery of a super-Earth and a sub-Neptune transiting the star HD 15337 (TOI-402, TIC 120896927), a bright (V = 9) K1 dwarf observed by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 3 and 4. We combine the TESS photometry with archival High Accuracy Radial velocity Planet Searcher spectra to confirm the planetary nature of the transit signals and derive the masses of the two transiting planets. With an orbital period of 4.8 days, a mass of and a radius of 1.64 ± 0.06 R ⊕, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of , and a radius of 2.39 ± 0.12 R ⊕, suggesting that the planet might be surrounded by a thick atmospheric envelope. The two planets have similar masses and lie on opposite sides of the radius gap, and are thus an excellent testbed for planet formation and evolution theories. Assuming that HD 15337 c hosts a hydrogen-dominated envelope, we employ a recently developed planet atmospheric evolution algorithm in a Bayesian framework to estimate the history of the high-energy (extreme ultraviolet and X-ray) emission of the host star. We find that at an age of 150 Myr, the star possessed on average between 3.7 and 127 times the high-energy luminosity of the current Sun.
(Less)
- author
- publishing date
- 2019-05-10
- type
- Contribution to journal
- publication status
- published
- in
- Astrophysical Journal Letters
- volume
- 876
- issue
- 2
- article number
- L24
- publisher
- IOP Publishing
- external identifiers
-
- scopus:85067310082
- ISSN
- 2041-8205
- DOI
- 10.3847/2041-8213/ab17d9
- language
- English
- LU publication?
- no
- additional info
- Publisher Copyright: © 2019. The American Astronomical Society. All rights reserved..
- id
- fc8ea625-8c08-4cd4-9df4-933918e1689c
- date added to LUP
- 2023-02-02 10:24:53
- date last changed
- 2023-02-20 14:20:26
@article{fc8ea625-8c08-4cd4-9df4-933918e1689c,
abstract = {{<p>We report the discovery of a super-Earth and a sub-Neptune transiting the star HD 15337 (TOI-402, TIC 120896927), a bright (V = 9) K1 dwarf observed by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 3 and 4. We combine the TESS photometry with archival High Accuracy Radial velocity Planet Searcher spectra to confirm the planetary nature of the transit signals and derive the masses of the two transiting planets. With an orbital period of 4.8 days, a mass of and a radius of 1.64 ± 0.06 R <sub>⊕</sub>, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of , and a radius of 2.39 ± 0.12 R <sub>⊕</sub>, suggesting that the planet might be surrounded by a thick atmospheric envelope. The two planets have similar masses and lie on opposite sides of the radius gap, and are thus an excellent testbed for planet formation and evolution theories. Assuming that HD 15337 c hosts a hydrogen-dominated envelope, we employ a recently developed planet atmospheric evolution algorithm in a Bayesian framework to estimate the history of the high-energy (extreme ultraviolet and X-ray) emission of the host star. We find that at an age of 150 Myr, the star possessed on average between 3.7 and 127 times the high-energy luminosity of the current Sun.</p>}},
author = {{Gandolfi, Davide and Fossati, Luca and Livingston, John H. and Stassun, Keivan G. and Grziwa, Sascha and Barragán, Oscar and Fridlund, Malcolm and Kubyshkina, Daria and Persson, Carina M. and Dai, Fei and Lam, Kristine W.F. and Albrecht, Simon and Batalha, Natalie and Beck, Paul G. and Justesen, Anders Bo and Cabrera, Juan and Cartwright, Scott and Cochran, William D. and Csizmadia, Szilard and Davies, Misty D. and Deeg, Hans J. and Eigmüller, Phili and Endl, Michael and Erikson, Anders and Esposito, Massimiliano and Garciá, Rafael A. and Goeke, Robert and González-Cuesta, Luciá and Guenther, Eike W. and Hatzes, Artie P. and Hidalgo, Diego and Hirano, Teruyuki and Hjorth, Maria and Kabath, Petr and Knudstrup, Emil and Korth, Judith and Li, Jie and Luque, Rafael and Mathur, Savita and Rodríguez, Pilar Montañes and Narita, Norio and Nespral, David and Niraula, Prajwal and Nowak, Grzegorz and Palle, Enric and Pätzold, Martin and Prieto-Arranz, Jorge and Rauer, Heike and Redfield, Seth and Ribas, Ignasi and Skarka, Marek and Smith, Alexis M.S. and Rowden, Pamela and Torres, Guillermo and Van Eylen, Vincent and Vezie, Michael L.}},
issn = {{2041-8205}},
language = {{eng}},
month = {{05}},
number = {{2}},
publisher = {{IOP Publishing}},
series = {{Astrophysical Journal Letters}},
title = {{The Transiting Multi-planet System HD15337 : Two Nearly Equal-mass Planets Straddling the Radius Gap}},
url = {{http://dx.doi.org/10.3847/2041-8213/ab17d9}},
doi = {{10.3847/2041-8213/ab17d9}},
volume = {{876}},
year = {{2019}},
}