학술논문
Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets
Document Type
article
Author
Christiansen, Jessie L; Vanderburg, Andrew; Burt, Jennifer; Fulton, BJ; Batygin, Konstantin; Benneke, Björn; Brewer, John M; Charbonneau, David; Ciardi, David R; Cameron, Andrew Collier; Coughlin, Jeffrey L; Crossfield, Ian JM; Dressing, Courtney; Greene, Thomas P; Howard, Andrew W; Latham, David W; Molinari, Emilio; Mortier, Annelies; Mullally, Fergal; Pepe, Francesco; Rice, Ken; Sinukoff, Evan; Sozzetti, Alessandro; Thompson, Susan E; Udry, Stéphane; Vogt, Steven S; Barman, Travis S; Batalha, Natasha E; Bouchy, François; Buchhave, Lars A; Butler, R Paul; Cosentino, Rosario; Dupuy, Trent J; Ehrenreich, David; Fiorenzano, Aldo; Hansen, Brad MS; Henning, Thomas; Hirsch, Lea; Holden, Bradford P; Isaacson, Howard T; Johnson, John A; Knutson, Heather A; Kosiarek, Molly; López-Morales, Mercedes; Lovis, Christophe; Malavolta, Luca; Mayor, Michel; Micela, Giuseppina; Motalebi, Fatemeh; Petigura, Erik; Phillips, David F; Piotto, Giampaolo; Rogers, Leslie A; Sasselov, Dimitar; Schlieder, Joshua E; Ségransan, Damien; Watson, Christopher A; Weiss, Lauren M
Source
The Astronomical Journal. 154(3)
Subject
Language
Abstract
HD 3167 is a bright (V = 8.9), nearby K0 star observed by the NASA K2 mission (EPIC 220383386), hosting two small, short-period transiting planets. Here we present the results of a multi-site, multi-instrument radial-velocity campaign to characterize the HD 3167 system. The masses of the transiting planets are 5.02 ±0.38 M+for HD 3167 b, a hot super-Earth with a likely rocky composition (ρb = 5.60 +2.15-1.43= g cm-3), and 9.80 +1.30-1.24 M+for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement (pc = 1.97 0.94-0.59 g cm-3). We explore the possibility of atmospheric composition analysis and determine that planet c is amenable to transmission spectroscopy measurements, and planet b is a potential thermal emission target. We detect a third, non-transiting planet, HD 3167 d, with a period of 8.509 ±0.045 d (between planets b and c) and a minimum mass of 6.90 ±0.71 M⊕. We are able to constrain the mutual inclination of planet d with planets b and c: we rule out mutual inclinations below 1.°3 because we do not observe transits of planet d. From 1.°3 to 40°, there are viewing geometries invoking special nodal configurations, which result in planet d not transiting some fraction of the time. From 40° to 60°, Kozai-Lidov oscillations increase the system's instability, but it can remain stable for up to 100 Myr. Above 60°, the system is unstable. HD 3167 promises to be a fruitful system for further study and a preview of the many exciting systems expected from the upcoming NASA TESS mission.