Artículo de revista
TESS Reveals a short-period sub-neptune sibling (HD 86226c) to a known long-period giant planet
Fecha
2020Registro en:
The Astronomical Journal, 160:96 (17pp), 2020 August
10.3847/1538-3881/ab9f95
Autor
Teske, Johanna
Díaz, Matías R.
Luque, Rafael
Močnik, Teo
Seidel, Julia V.
Fernández Otegi, Jon
Feng, Fabo
Jenkins, James S.
Pallè, Enric
Ségransan, Demien
Udry, Stéphane
Collins, Karen A.
Eastman, Jason D.
Ricker, George R.
Vanderspek, Roland
Latham, David W.
Seager, Sara
Winn, Joshua N.
Jenkins, Jon M.
Anderson, David R.
Barclay, Thomas
Bouchy, François
Burt, Jennifer A.
Paul Butler, R.
Caldwell, Douglas A.
Collins, Kevin I.
Crane, Jeffrey D.
Dorn, Caroline
Flowers, Erin
Haldemann, Jonás
Helled, Ravit
Hellier, Coel
Jensen, Eric L. N.
Kane, Stephen R.
Law, Nicholas
Lissauer, Jack J.
Mann, Andrew W.
Marmier, Maxime
Nielsen, Louise Dyregaard
Rose, Mark E.
Shectman, Stephen A.
Shporer, Avi
Torres, Guillermo
Wang, Sharon
Wolfgang, Angie
Wong, Ian
Ziegler, Carl
Institución
Resumen
The Transiting Exoplanet Survey Satellite mission was designed to find transiting planets around bright, nearby
stars. Here, we present the detection and mass measurement of a small, short-period (≈4 days) transiting planet
around the bright (V=7.9), solar-type star HD 86226 (TOI-652, TIC 22221375), previously known to host a
long-period (∼1600 days) giant planet. HD 86226c (TOI-652.01) has a radius of 2.16±0.08R⊕ and a mass of
-
7.25+1.12
1.19 M⊕, based on archival and new radial velocity data. We also update the parameters of the longer-period,
not-known-to-transit planet, and find it to be less eccentric and less massive than previously reported. The density
of the transiting planet is 3.97 gcm−3, which is low enough to suggest that the planet has at least a small volatile
envelope, but the mass fractions of rock, iron, and water are not well-constrained. Given the host star brightness,
planet period, and location of the planet near both the “radius gap” and the “hot Neptune desert,” HD 86226c is an
interesting candidate for transmission spectroscopy to further refine its composition.