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Title: | Three’s Company: An Additional Non-transiting Super-Earth in the Bright HD 3167 System, and Masses for All Three Planets | Authors: | Christiansen, Jessie L. Vanderburg, Andrew Burt, Jennifer Fulton, B. J. Batygin, Konstantin Benneke, Björn Brewer, John M. Charbonneau, David Ciardi, David R. Collier Cameron, Andrew Coughlin, Jeffrey L. Crossfield, Ian J. M. Dressing, Courtney Greene, Thomas P. Howard, Andrew W. Latham, David W. MOLINARI, Emilio Carlo 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 M. S. 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. |
Issue Date: | 2017 | Journal: | THE ASTRONOMICAL JOURNAL | Number: | 154 | Issue: | 3 | First Page: | 122 | 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}<SUB>\oplus </SUB> for HD 3167 b, a hot super-Earth with a likely rocky composition ({ρ }<SUB>b</SUB> = {5.60}<SUB>-1.43</SUB><SUP>+2.15</SUP> g cm<SUP>-3</SUP>), and {9.80}<SUB>-1.24</SUB><SUP>+1.30</SUP> {M}<SUB>\oplus </SUB> for HD 3167 c, a warm sub-Neptune with a likely substantial volatile complement ({ρ }<SUB>c</SUB> = {1.97}<SUB>-0.59</SUB><SUP>+0.94</SUP> g cm<SUP>-3</SUP>). 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}<SUB>\oplus </SUB>. 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. | URI: | http://hdl.handle.net/20.500.12386/26890 | URL: | https://iopscience.iop.org/article/10.3847/1538-3881/aa832d | ISSN: | 0004-6256 | DOI: | 10.3847/1538-3881/aa832d | Bibcode ADS: | 2017AJ....154..122C | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Christiansen_2017_AJ_154_122.pdf | pdf editoriale | 3.11 MB | Adobe PDF | View/Open |
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