2020A&A...641A..25N


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.05CET01:23:09

2020A&A...641A..25N - Astronomy and Astrophysics, volume 641A, 25-25 (2020/9-1)

TESS asteroseismology of the known planet host star λ2 Fornacis.

NIELSEN M.B., BALL W.H., STANDING M.R., TRIAUD A.H.M.J., BUZASI D., CARBONEAU L., STASSUN K.G., KANE S.R., CHAPLIN W.J., BELLINGER E.P., MOSSER B., ROXBURGH I.W., CELIK ORHAN Z., YILDIZ M., ORTEL S., VRARD M., MAZUMDAR A., RANADIVE P., DEAL M., DAVIES G.R., CAMPANTE T.L., GARCIA R.A., MATHUR S., GONZALEZ-CUESTA L. and SERENELLI A.

Abstract (from CDS):


Context. The Transiting Exoplanet Survey Satellite (TESS) is observing bright known planet-host stars across almost the entire sky. These stars have been subject to extensive ground-based observations, providing a large number of radial velocity measurements.
Aims. The objective of this work is to use the new TESS photometric observations to characterize the star λ2 Fornacis, and following this to update the parameters of the orbiting planet λ2 For b.
Methods. We measured the frequencies of the p-mode oscillations in λ2 For, and in combination with non-seismic parameters estimated the stellar fundamental properties using stellar models. Using the revised stellar properties and a time series of archival radial velocities from the UCLES, HIRES and HARPS instruments spanning almost 20 years, we refit the orbit of λ2 For b and searched the residual radial velocities for remaining variability.
Results. We find that λ2 For has a mass of 1.16±0.03M and a radius of 1.63±0.04R, with an age of 6.3±0.9Gyr. This and the updated radial velocity measurements suggest a mass of λ2 For b of 16.8–1.3+1.2M, which is ∼5M less than literature estimates. We also detect an additional periodicity at 33 days in the radial velocity measurements, which is likely due to the rotation of the host star .
Conclusions. While previous literature estimates of the properties of λ2 For are ambiguous, the asteroseismic measurements place the star firmly at the early stage of its subgiant evolutionary phase. Typically only short time series of photometric data are available from TESS, but by using asteroseismology it is still possible to provide tight constraints on the properties of bright stars that until now have only been observed from the ground. This prompts a reexamination of archival radial velocity data that have been accumulated in the past few decades in order to update the characteristics of the planet hosting systems observed by TESS for which asteroseismology is possible.

Abstract Copyright: © ESO 2020

Journal keyword(s): asteroseismology - stars: individual: HD 16417 - planetary systems - techniques: radial velocities - techniques: photometric

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * lam02 For PM* 02 36 58.6079324808 -34 34 40.713450652 6.67 6.45 5.79     G1V 180 1
2 HD 16417b Pl 02 36 58.6079324808 -34 34 40.713450652           ~ 20 1

    Equat.    Gal    SGal    Ecl

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2020.12.05-01:23:09

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