scholarly journals Asteroseismology of exoplanet host stars

2015 ◽  
Vol 11 (A29B) ◽  
pp. 620-627
Author(s):  
Daniel Huber
Keyword(s):  
Radial Velocity ◽  
Planetary Systems ◽  
Precise Determination ◽  
Spin Orbit ◽  
Velocity Measurements ◽  
Fundamental Properties ◽  
Future Space ◽  
Host Stars

AbstractAsteroseismology is among the most powerful observational tools to determine fundamental properties of stars. Space-based photometry has recently enabled the systematic detection of oscillations in exoplanet host stars, allowing a combination of asteroseismology with transit and radial-velocity measurements to characterize planetary systems. In this contribution I will review the key synergies between asteroseismology and exoplanet science such as the precise determination of radii and ages of exoplanet host stars, as well as applications of asteroseismology to measure spin-orbit inclinations in multiplanet systems and orbital eccentricities of small planets. Finally I will give a brief outlook on asteroseismic studies of exoplanet hosts with current and future space-based missions such as K2 and TESS.

scholarly journals Extra-solar Planets: Clues to Planetary Formation

2004 ◽  
Vol 219 ◽  
pp. 311-322 ◽  
Author(s):  
Nuno C. Santos ◽  
Michel Mayor ◽  
Dominique Naef ◽  
Francesco Pepe ◽  
Didier Queloz ◽  
...  
Keyword(s):  
Statistical Analysis ◽  
Radial Velocity ◽  
Crucial Role ◽  
Giant Planet ◽  
Planetary Systems ◽  
Current Status ◽  
Planetary Formation ◽  
Orbital Elements ◽  
Host Stars

Radial velocity surveys have revealed up to now about 115 extra-solar planets, among which a few multi-planetary systems. The discovered planets present a wide variety of orbital elements and masses, which are raising many problems and questions regarding the processes involved in their formation. The statistical analysis of the distributions of orbital elements, planetary masses, and relations between these, is however already giving some strong constraints on the formation of the planetary systems. Furthermore, the study of the planet host stars has revealed the crucial role of the stellar metallicity on the giant planet formation. In this paper we will review the current status of the research on this subject.

scholarly journals Precise determination of fundamental parameters of six exoplanet host stars and their planets

2014 ◽  
Vol 14 (11) ◽  
pp. 1447-1457 ◽  
Author(s):  
Kang Liu ◽  
Shao-Lan Bi ◽  
Tan-Da Li ◽  
Zhi-E Liu ◽  
Zhi-Jia Tian ◽  
...  
Keyword(s):  
Precise Determination ◽  
Fundamental Parameters ◽  
Host Stars

scholarly journals The HoSTS Project: A Homogeneous Study of Transiting Systems

2013 ◽  
Vol 8 (S299) ◽  
pp. 285-286
Author(s):  
Yilen Gómez Maqueo Chew ◽  
Francesca Faedi ◽  
Leslie Hebb ◽  
Don Pollacco ◽  
Keivan Stassun ◽  
...  
Keyword(s):  
Pilot Study ◽  
Physical Properties ◽  
Planetary Systems ◽  
Planetary Formation ◽  
Empirical Correlations ◽  
Large Sample ◽  
Fundamental Properties ◽  
Homogeneous Set ◽  
Formation And Evolution ◽  
Host Stars

AbstractThe Homogeneous Study of Transiting Systems (HoSTS) will derive a consistent and homogeneous set of both the stellar and planetary physical properties for a large sample of bright transiting planetary systems with confirmed planetary masses and measured radii. Our resulting catalogs of the fundamental properties of these bright planets and their host stars will enable us to explore empirical correlations that will lead to a better understanding of planetary formation and evolution. We present our pilot study of the planet-hosting star WASP-13, and the framework of our project which will allow for the identification of true relationships among the physical properties of the systems from any systematics.

scholarly journals Can we detect the stellar differential rotation of WASP-7 through the Rossiter–McLaughlin observations?

2020 ◽  
Vol 493 (4) ◽  
pp. 5928-5943
Author(s):  
L M Serrano ◽  
M Oshagh ◽  
H M Cegla ◽  
S C C Barros ◽  
N C Santos ◽  
...  
Keyword(s):  
White Noise ◽  
Radial Velocity ◽  
Differential Rotation ◽  
Precise Determination ◽  
Next Generation ◽  
Velocity Signal ◽  
Rotating Star ◽  
Derived Geometry ◽  
Hot Jupiter

ABSTRACT The Rossiter–McLaughlin (RM) effect is the radial velocity signal generated when an object transits a rotating star. Stars rotate differentially and this affects the shape and amplitude of this signal, on a level that can no longer be ignored with precise spectrographs. Highly misaligned planets provide a unique opportunity to probe stellar differential rotation via the RM effect, as they cross several stellar latitudes. In this sense, WASP-7, and its hot Jupiter with a projected misalignment of ∼90°, is one of the most promising targets. The aim of this work is to understand if the stellar differential rotation is measurable through the RM signal for systems with a geometry similar to WASP-7. In this sense, we use a modified version of soap3.0 to explore the main hurdles that prevented the precise determination of the differential rotation of WASP-7. We also investigate whether the adoption of the next generation spectrographs, like ESPRESSO, would solve these issues. Additionally, we assess how instrumental and stellar noise influence this effect and the derived geometry of the system. We found that, for WASP-7, the white noise represents an important hurdle in the detection of the stellar differential rotation, and that a precision of at least 2 m s−1 or better is essential.

scholarly journals Radial velocity measurements and orbit determination of eight single-lined spectroscopic binary systems

2017 ◽  
Vol 338 (6) ◽  
pp. 671-679 ◽  
Author(s):  
R. Bischoff ◽  
M. Mugrauer ◽  
T. Zehe ◽  
D. Wöckel ◽  
A. Pannicke ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Orbit Determination ◽  
Binary Systems ◽  
Velocity Measurements ◽  
Spectroscopic Binary

scholarly journals A white dwarf bound to the transiting planetary system WASP-98

2020 ◽  
Vol 497 (4) ◽  
pp. 4416-4422
Author(s):  
John Southworth ◽  
Pier-Emmanuel Tremblay ◽  
Boris T Gänsicke ◽  
Daniel Evans ◽  
Teo Močnik
Keyword(s):  
White Dwarf ◽  
White Dwarfs ◽  
Planetary System ◽  
Planetary Systems ◽  
Precise Determination ◽  
Spectral Lines ◽  
Low Metallicity ◽  
Gaia Dr2 ◽  
Rule Out

ABSTRACT WASP-98 is a planetary system containing a hot Jupiter transiting a late-G dwarf. A fainter star, 12 arcsec away, has previously been identified as a white dwarf, with a distance and proper motion consistent with a physical association with the planetary system. We present spectroscopy of the white dwarf, with the aim of determining its mass, radius, and temperature and hence the age of the system. However, the spectra show the featureless continuum and lack of spectral lines characteristic of the DC class of white dwarfs. We therefore fitted theoretical white dwarf spectra to the ugriz apparent magnitudes and Gaia DR2 parallax of this object in order to determine its physical properties and the age of the system. We find that the system is old, with a lower limit of 3.6 Gyr, but theoretical uncertainties preclude a precise determination of its age. Its kinematics are consistent with membership of the thick disc, but do not allow us to rule out the thin-disc alternative. The old age and low metallicity of the system suggest that it is subject to an age–metallicity relation, but analysis of the most metal-rich and metal-poor transiting planetary systems yields only insubstantial evidence of this. We conclude that the study of bound white dwarfs can yield independent ages to planetary systems, but such analysis may be better suited to DA and DB rather than DC white dwarfs.

scholarly journals HD 219666 b: a hot-Neptune from TESS Sector 1

2019 ◽  
Vol 623 ◽  
pp. A165 ◽  
Author(s):  
M. Esposito ◽  
D. J. Armstrong ◽  
D. Gandolfi ◽  
V. Adibekyan ◽  
M. Fridlund ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Thermal Structure ◽  
Formation Mechanisms ◽  
Mass Determination ◽  
Velocity Measurements ◽  
Fundamental Parameters ◽  
Refractory Elements ◽  
Rare Class ◽  
In Transit

We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD 219666 (M⋆ = 0.92 ± 0.03 M⊙, R⋆ = 1.03 ± 0.03 R⊙, τ⋆ = 10 ± 2 Gyr). With a mass of Mb = 16.6 ± 1.3 M⊕, a radius of Rb = 4.71 ± 0.17 R⊕, and an orbital period of Porb ≃ 6 days, HD 219666 b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD 219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with the High Accuracy Radial velocity Planet Searcher (HARPS) at ESO 3.6 m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (Teff = 5527 ± 65 K, log g⋆ = 4.40 ± 0.11 (cgs), [Fe/H]= 0.04 ± 0.04 dex, log R′HK = −5.07 ± 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmosphericmetal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects.

scholarly journals Precise characterisation of exoplanet-host stars parameters

2010 ◽  
Vol 6 (S276) ◽  
pp. 30-33
Author(s):  
Sylvie Vauclair
Keyword(s):  
Effective Temperature ◽  
Heavy Element ◽  
Precise Determination ◽  
Planetary Formation ◽  
Element Abundances ◽  
Stellar Oscillations ◽  
Host Stars ◽  
Excellent Tool

AbstractStudying the internal structure of exoplanet-host stars compared to that of similar stars without detected planets is particularly important for the understanding of planetary formation. In this framework, asteroseismic studies represent an excellent tool for a better characterization of stars and for a precise determination of the stellar parameters like mass, radius, gravity, effective temperature. The detection of stellar oscillations is obtained with the same instruments as used for the discovery of exoplanets, both from the ground and from space, although the time scales are very different. Here I discuss some details about the characterization of exoplanethost stars from seismology and the importance of the helium and heavy element abundances in this respect.

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