Asteroseismology of exoplanets hosts stars: Tests of internal metallicity

Michael Bazot, S. Vauclair

Research output: Contribution to journalArticle

Abstract

Exoplanet host stars present a clear metallicity excess compared to stars without detected planets, with an average overabundance of 0.2 dex. This excess may be primordial, in which case the stars should be overmetallic down to their center, or it may be due to accretion in the early phases of planetary formation, in which case the stars would be overmetallic only in their outer layers. In the present paper, we show the differences in the internal structure of stars, according to the chosen scenario. Namely two stars with the same observable parameters (luminosity, effective temperature, outer chemical composition) are completely different in their interiors according to their past histories, which we reconstitute through the computations of their evolutionary tracks. It may happen that stars with an initial overmetallicity have a convective core while the stars which suffered accretion do not. We claim that asteroseismic studies of these exoplanet host stars can give clues about their internal structures and metallicities, which may help in understanding planetary formation.

Original languageEnglish (US)
Pages (from-to)965-973
Number of pages9
JournalAstronomy and Astrophysics
Volume427
Issue number3
DOIs
StatePublished - Dec 1 2004

Fingerprint

asteroseismology
extrasolar planets
metallicity
accretion
stars
planet
chemical composition
temperature
test
planets
luminosity
histories
parameter

Keywords

  • Abundances - Stars
  • Formation - Stars
  • Oscillations
  • Planetary systems
  • Stars

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Asteroseismology of exoplanets hosts stars : Tests of internal metallicity. / Bazot, Michael; Vauclair, S.

In: Astronomy and Astrophysics, Vol. 427, No. 3, 01.12.2004, p. 965-973.

Research output: Contribution to journalArticle

@article{d6ffa2b4f2114acba9520222dfaee726,
title = "Asteroseismology of exoplanets hosts stars: Tests of internal metallicity",
abstract = "Exoplanet host stars present a clear metallicity excess compared to stars without detected planets, with an average overabundance of 0.2 dex. This excess may be primordial, in which case the stars should be overmetallic down to their center, or it may be due to accretion in the early phases of planetary formation, in which case the stars would be overmetallic only in their outer layers. In the present paper, we show the differences in the internal structure of stars, according to the chosen scenario. Namely two stars with the same observable parameters (luminosity, effective temperature, outer chemical composition) are completely different in their interiors according to their past histories, which we reconstitute through the computations of their evolutionary tracks. It may happen that stars with an initial overmetallicity have a convective core while the stars which suffered accretion do not. We claim that asteroseismic studies of these exoplanet host stars can give clues about their internal structures and metallicities, which may help in understanding planetary formation.",
keywords = "Abundances - Stars, Formation - Stars, Oscillations, Planetary systems, Stars",
author = "Michael Bazot and S. Vauclair",
year = "2004",
month = "12",
day = "1",
doi = "10.1051/0004-6361:20041528",
language = "English (US)",
volume = "427",
pages = "965--973",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "3",

}

TY - JOUR

T1 - Asteroseismology of exoplanets hosts stars

T2 - Tests of internal metallicity

AU - Bazot, Michael

AU - Vauclair, S.

PY - 2004/12/1

Y1 - 2004/12/1

N2 - Exoplanet host stars present a clear metallicity excess compared to stars without detected planets, with an average overabundance of 0.2 dex. This excess may be primordial, in which case the stars should be overmetallic down to their center, or it may be due to accretion in the early phases of planetary formation, in which case the stars would be overmetallic only in their outer layers. In the present paper, we show the differences in the internal structure of stars, according to the chosen scenario. Namely two stars with the same observable parameters (luminosity, effective temperature, outer chemical composition) are completely different in their interiors according to their past histories, which we reconstitute through the computations of their evolutionary tracks. It may happen that stars with an initial overmetallicity have a convective core while the stars which suffered accretion do not. We claim that asteroseismic studies of these exoplanet host stars can give clues about their internal structures and metallicities, which may help in understanding planetary formation.

AB - Exoplanet host stars present a clear metallicity excess compared to stars without detected planets, with an average overabundance of 0.2 dex. This excess may be primordial, in which case the stars should be overmetallic down to their center, or it may be due to accretion in the early phases of planetary formation, in which case the stars would be overmetallic only in their outer layers. In the present paper, we show the differences in the internal structure of stars, according to the chosen scenario. Namely two stars with the same observable parameters (luminosity, effective temperature, outer chemical composition) are completely different in their interiors according to their past histories, which we reconstitute through the computations of their evolutionary tracks. It may happen that stars with an initial overmetallicity have a convective core while the stars which suffered accretion do not. We claim that asteroseismic studies of these exoplanet host stars can give clues about their internal structures and metallicities, which may help in understanding planetary formation.

KW - Abundances - Stars

KW - Formation - Stars

KW - Oscillations

KW - Planetary systems

KW - Stars

UR - http://www.scopus.com/inward/record.url?scp=10044295137&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=10044295137&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20041528

DO - 10.1051/0004-6361:20041528

M3 - Article

AN - SCOPUS:10044295137

VL - 427

SP - 965

EP - 973

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 3

ER -