The transiting multi-planet system HD 3167

• Verfasst von: Gandolfi, Davide [VerfasserIn]
• Verfasst von: Brems, Stefan S. [VerfasserIn]
• Titel: The transiting multi-planet system HD 3167
• Titelzusatz: s 5.7 M[Earth] super-Earth and an 8.3 M[Earth] mini-Neptune
• Verf.angabe: Davide Gandolfi, Oscar Barragán, Artie P. Hatzes, Malcolm Fridlund, Luca Fossati, Paolo Donati, Marshall C. Johnson, Grzegorz Nowak, Jorge Prieto-Arranz, Simon Albrecht, Fei Dai, Hans Deeg, Michael Endl, Sascha Grziwa, Maria Hjorth, Judith Korth, David Nespral, Joonas Saario, Alexis M. S. Smith, Giuliano Antoniciello, Javier Alarcon, Megan Bedell, Pere Blay, Stefan S. Brems, Juan Cabrera, Szilard Csizmadia, Felice Cusano, William D. Cochran, Philipp Eigmüller, Anders Erikson, Jonay I. González Hernández, Eike W. Guenther, Teruyuki Hirano, Alejandro Suárez Mascareño, Norio Narita, Enric Palle, Hannu Parviainen, Martin Pätzold, Carina M. Persson, Heike Rauer, Ivo Saviane, Linda Schmidtobreick, Vincent Van Eylen, Joshua N. Winn and Olga V. Zakhozhay
• E-Jahr: 2017
• Jahr: 2017 August 31
• Umfang: 15 S.
• Fussnoten: Im Titel wird die Erde symbolisch mit Radkreuzzeichen dargestellt ; Gesehen am 09.10.2017
• Titel Quelle: Enthalten in: The astronomical journal
• Ort Quelle: London : Institute of Physics Publ., 1998
• Jahr Quelle: 2017
• Band/Heft Quelle: 154(2017,3) Artikel-Nummer 123, 15 Seiten
• ISSN Quelle: 1538-3881
• DOI: doi:10.3847/1538-3881/aa832a
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1564203611

Abstract

HD 3167 is a bright ( V = 8.9 mag) K0 V star observed by NASA’s K2 space mission during its Campaign 8. It has recently been found to host two small transiting planets, namely, HD 3167b, an ultra-short-period (0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 days). Here we present an intensive radial velocity (RV) follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6 m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69 ± 0.44 M ⊕ , a radius of 1.574 ± 0.054 R ⊕ , and a mean density of ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn1.gif] $8.00_-0.98^+1.10$ ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn2.gif] $\rmg\,\mathrmcm^-3$ , HD 3167b joins the small group of ultra-short-period planets known to have rocky terrestrial compositions. HD 3167c has a mass of ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn3.gif] $8.33_-1.85^+1.79$ M ⊕ and a radius of ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn4.gif] $2.740_-0.100^+0.106$ R ⊕ , yielding a mean density of ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn5.gif] $2.21_-0.53^+0.56$ ##IMG## [http://ej.iop.org/images/1538-3881/154/3/123/ajaa832aieqn6.gif] $\rmg\,\mathrmcm^-3$ , indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (∼350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the RV measurements but the currently available data set does not allow us to draw any firm conclusions on the origin of the observed variation.