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HD 213885b: A transiting 1-day-period super-Earth with an Earth-like composition around a bright ($V=7.9$) star unveiled by TESS | | Néstor Espinoza
; Rafael Brahm
; Thomas Henning
; Andrés Jordán
; Caroline Dorn
; Felipe Rojas
; Paula Sarkis
; Diana Kossakowski
; Matías Díaz
; James S. Jenkins
; Claudia Aguilera-Gomez
; Jon M. Jenkins
; Joseph D. Twicken
; Karen A. Collins
; Jack Lissauer
; David J. Armstrong
; Vardan Adibekyan
; David Barrado
; Susana C. C. Barros
; Matthew Battley
; Daniel Bayliss
; François Bouchy
; Edward Bryant
; Benjamin F. Cooke
; Olivier D. S. Demangeon
; Xavier Dumusque
; Pedro Figueira
; Helen Giles
; Jorge Lillo-Box
; Christophe Lovis
; Louise D. Nielsen
; Francesco Pepe
; Don Pollaco
; Nuno C. Santos
; Sergio G. Sousa
; Stéphane Udry
; Peter J. Wheatley
; Oliver Turner
; Maxime Marmier
; Damien Ségransan
; George Ricker
; David Latham
; Sara Seager
; Joshua N. Winn
; John F. Kielkopf
; Rhodes Hart
; Geof Wingham
; Eric L. N. Jensen
; Krzysztof G. Hełminiak
; A. Tokovinin
; C. Briceño
; Carl Ziegler
; Nicholas M. Law
; Andrew W. Mann
; Tansu Daylan
; John P. Doty
; Natalia Guerrero
; Patricia Boyd
; Ian Crossfield
; Robert L. Morris
; Christopher E. Henze
; Aaron Dean Chacon
; | | Date: |
18 Mar 2019 | | Abstract: | We report the discovery of the 1.008-day, ultra-short period (USP)
super-Earth HD 213885b (TOI-141b) orbiting the bright ($V=7.9$) star HD 213885
(TOI-141, TIC 403224672), detected using photometry from the recently launched
extit{TESS} mission. Using FEROS, HARPS and CORALIE radial-velocities, we
measure a precise mass of $8.83^{+0.66}_{-0.65}$ $M_oplus$ for this
$1.745^{+0.051}_{-0.052}$ $R_oplus$ exoplanet, which provides enough
information to constrain its bulk composition, which is similar to Earth’s
composition but enriched in iron. The radius, mass and stellar irradiation of
HD 213885b are almost indistinguishable from that of 55 Cancri e, making this
exoplanet its first "twin" in terms of its physical properties --- HD 213885b,
however, appears to be denser ($9.15^{+1.1}_{-1.0}$ gr cm$^{-3}$) than 55
Cancri e. Our precise radial-velocities reveal an additional $4.78$-day signal
which we interpret as arising from a second, non-transiting planet in the
system, HD 213885c (TOI-141c), which has a minimum mass of
$19.95^{+1.38}_{-1.36}$ $M_oplus$ and thus is consistent with being a
Neptune-mass exoplanet. The HD 213885 system is very interesting from the
perspective of future atmospheric characterization, being the second brightest
star to host an ultra-short period transiting super-Earth (with the brightest
star being, in fact, 55 Cancri). Prospects for characterization with present
and future observatories are discussed. | | Source: | arXiv, 1903.7694 | | Services: | Forum | Review | PDF | Favorites | |
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