New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems

P. Bluhm, M. I. Jones, L. Vanzi, M. G. Soto, J. Vos, R. A. Wittenmyer, H. Drass, J. S. Jenkins, F. Olivares, R. E. Mennickent, M. Vučković, P. Rojo, C. H.F. Melo

Resultado de la investigación: Article

5 Citas (Scopus)

Resumen

We report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between ∼97-1600 days and eccentricities of between ∼0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities.

Idioma originalEnglish
Número de artículoA133
PublicaciónAstronomy and Astrophysics
Volumen593
DOI
EstadoPublished - 1 sep 2016
Publicado de forma externa

Huella dactilar

giant stars
eccentricity
metallicity
orbitals
binary stars
planet
stars
formation mechanism
orbital elements
circular orbits
extrasolar planets
distribution
metal
radial velocity
planets
trends
metals

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Bluhm, P., Jones, M. I., Vanzi, L., Soto, M. G., Vos, J., Wittenmyer, R. A., ... Melo, C. H. F. (2016). New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems. Astronomy and Astrophysics, 593, [A133]. https://doi.org/10.1051/0004-6361/201628459
Bluhm, P. ; Jones, M. I. ; Vanzi, L. ; Soto, M. G. ; Vos, J. ; Wittenmyer, R. A. ; Drass, H. ; Jenkins, J. S. ; Olivares, F. ; Mennickent, R. E. ; Vučković, M. ; Rojo, P. ; Melo, C. H.F. / New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems. En: Astronomy and Astrophysics. 2016 ; Vol. 593.
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abstract = "We report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between ∼97-1600 days and eccentricities of between ∼0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities.",
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Bluhm, P, Jones, MI, Vanzi, L, Soto, MG, Vos, J, Wittenmyer, RA, Drass, H, Jenkins, JS, Olivares, F, Mennickent, RE, Vučković, M, Rojo, P & Melo, CHF 2016, 'New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems', Astronomy and Astrophysics, vol. 593, A133. https://doi.org/10.1051/0004-6361/201628459

New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems. / Bluhm, P.; Jones, M. I.; Vanzi, L.; Soto, M. G.; Vos, J.; Wittenmyer, R. A.; Drass, H.; Jenkins, J. S.; Olivares, F.; Mennickent, R. E.; Vučković, M.; Rojo, P.; Melo, C. H.F.

En: Astronomy and Astrophysics, Vol. 593, A133, 01.09.2016.

Resultado de la investigación: Article

TY - JOUR

T1 - New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems

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AU - Jones, M. I.

AU - Vanzi, L.

AU - Soto, M. G.

AU - Vos, J.

AU - Wittenmyer, R. A.

AU - Drass, H.

AU - Jenkins, J. S.

AU - Olivares, F.

AU - Mennickent, R. E.

AU - Vučković, M.

AU - Rojo, P.

AU - Melo, C. H.F.

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N2 - We report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between ∼97-1600 days and eccentricities of between ∼0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities.

AB - We report the discovery of 24 spectroscopic binary companions to giant stars. We fully constrain the orbital solution for 6 of these systems. We cannot unambiguously derive the orbital elements for the remaining stars because the phase coverage is incomplete. Of these stars, 6 present radial velocity trends that are compatible with long-period brown dwarf companions. The orbital solutions of the 24 binary systems indicate that these giant binary systems have a wide range in orbital periods, eccentricities, and companion masses. For the binaries with restricted orbital solutions, we find a range of orbital periods of between ∼97-1600 days and eccentricities of between ∼0.1-0.4. In addition, we studied the metallicity distribution of single and binary giant stars. We computed the metallicity of a total of 395 evolved stars, 59 of wich are in binary systems. We find a flat distribution for these binary stars and therefore conclude that stellar binary systems, and potentially brown dwarfs, have a different formation mechanism than planets. This result is confirmed by recent works showing that extrasolar planets orbiting giants are more frequent around metal-rich stars. Finally, we investigate the eccentricity as a function of the orbital period. We analyzed a total of 130 spectroscopic binaries, including those presented here and systems from the literature. We find that most of the binary stars with periods 30 days have circular orbits, while at longer orbital periods we observe a wide spread in their eccentricities.

KW - Binaries: spectroscopic

KW - Techniques: radial velocities

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DO - 10.1051/0004-6361/201628459

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