ATTENTION: The software behind KU ScholarWorks is being upgraded to a new version. Starting July 15th, users will not be able to log in to the system, add items, nor make any changes until the new version is in place at the end of July. Searching for articles and opening files will continue to work while the system is being updated.
If you have any questions, please contact Marianne Reed at mreed@ku.edu .
A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS
dc.contributor.author | Huber, Daniel | |
dc.contributor.author | Crossfield, Ian | |
dc.date.accessioned | 2020-12-23T19:47:01Z | |
dc.date.available | 2020-12-23T19:47:01Z | |
dc.date.issued | 2019-05-30 | |
dc.identifier.citation | Daniel Huber et al 2019 AJ 157 245 | en_US |
dc.identifier.uri | http://hdl.handle.net/1808/31003 | |
dc.description.abstract | We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (Rsstarf = 2.943 ± 0.064 R⊙), mass (Msstarf = 1.212 ± 0.074 M⊙), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ~14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm−3). The properties of HD 221416 b show that the host-star metallicity–planet mass correlation found in sub-Saturns (4–8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ~15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology. | en_US |
dc.publisher | IOP Publishing | en_US |
dc.rights | © 2019. The American Astronomical Society. All rights reserved. | en_US |
dc.subject | Asteroseismology | en_US |
dc.subject | Techniques: photometric | en_US |
dc.subject | Planets and satellites: individual | en_US |
dc.subject | (HD 221416 b) | en_US |
dc.subject | Stars: fundamental parameters | en_US |
dc.subject | Planets and satellites: fundamental parameters | en_US |
dc.title | A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS | en_US |
dc.type | Article | en_US |
kusw.kuauthor | Crossfield, Ian | |
kusw.kudepartment | Physics and Astronomy | en_US |
dc.identifier.doi | 10.3847/1538-3881/ab1488 | en_US |
dc.identifier.orcid | https://orcid.org/0000-0001-8832-4488 | en_US |
kusw.oaversion | Scholarly/refereed, publisher version | en_US |
kusw.oapolicy | This item meets KU Open Access policy criteria. | en_US |
dc.rights.accessrights | openAccess | en_US |