Orbital Characterization of GJ1108A System, and Comparison of Dynamical Mass with Model-derived Mass for Resolved Binaries

T. Mizuki, M. Kuzuhara, K. Mede, J. E. Schlieder, M. Janson, T. D. Brandt, T. Hirano, N. Narita, J. Wisniewski, T. Yamada, B. Biller, M. Bonnefoy, J. C. Carson, M. W. McElwain, T. Matsuo, E. L. Turner, S. Mayama, E. Akiyama, T. Uyama, T. Nakagawa & 38 others T. Kudo, N. Kusakabe, J. Hashimoto, L. Abe, W. Brander, S. Egner, M. Feldt, M. Goto, C. A. Grady, Olivier Guyon, Y. Hayano, M. Hayashi, S. S. Hayashi, T. Henning, K. W. Hodapp, M. Ishii, M. Iye, R. Kandori, G. R. Knapp, J. Kwon, S. Miyama, J. Morino, A. Moro-Martin, T. Nishimura, T. Pyo, E. Serabyn, T. Suenaga, H. Suto, R. Suzuki, Y. H. Takahashi, M. Takami, N. Takato, H. Terada, C. Thalmann, M. Watanabe, H. Takami, T. Usuda, M. Tamura

Research output: Contribution to journalArticle

Abstract

We report an orbital characterization of GJ1108Aab that is a low-mass binary system in the pre-main-sequence phase. Via the combination of astrometry using adaptive optics and radial velocity measurements, an eccentric orbital solution of e = 0.63 is obtained, which might be induced by the Kozai-Lidov mechanism with a widely separated GJ1108B system. Combined with several observed properties, we confirm that the system is indeed young. Columba is the most probable moving group, to which the GJ1108A system belongs, although its membership to the group has not been established. If the age of Columba is assumed for GJ1108A, the dynamical masses of both GJ1108Aa and GJ1108Ab (M dynamical,GJ1108Aa = 0.72 ± 0.04 M o and M dynamical,GJ1108Ab = 0.30 ± 0.03 M o) are more massive than what an evolutionary model predicts based on the age and luminosities. We consider that the discrepancy in mass comparison can be attributed to an age uncertainty; the system is likely older than stars in Columba, and effects that are not implemented in classical models such as accretion history and magnetic activity are not preferred to explain the mass discrepancy. We also discuss the performance of the evolutionary model by compiling similar low-mass objects in the evolutionary state based on the literature. Consequently, it is suggested that the current model on average reproduces the mass of resolved low-mass binaries without any significant offsets.

Original languageEnglish (US)
Article number152
JournalAstrophysical Journal
Volume865
Issue number2
DOIs
StatePublished - Oct 1 2018
Externally publishedYes

Fingerprint

orbitals
astrometry
eccentrics
comparison
adaptive optics
velocity measurement
radial velocity
accretion
luminosity
histories
stars
history

Keywords

  • binaries: spectroscopic
  • binaries: visual
  • stars: imaging
  • stars: individual (GJ1108A)
  • stars: low-mass

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Mizuki, T., Kuzuhara, M., Mede, K., Schlieder, J. E., Janson, M., Brandt, T. D., ... Tamura, M. (2018). Orbital Characterization of GJ1108A System, and Comparison of Dynamical Mass with Model-derived Mass for Resolved Binaries. Astrophysical Journal, 865(2), [152]. https://doi.org/10.3847/1538-4357/aada82

Orbital Characterization of GJ1108A System, and Comparison of Dynamical Mass with Model-derived Mass for Resolved Binaries. / Mizuki, T.; Kuzuhara, M.; Mede, K.; Schlieder, J. E.; Janson, M.; Brandt, T. D.; Hirano, T.; Narita, N.; Wisniewski, J.; Yamada, T.; Biller, B.; Bonnefoy, M.; Carson, J. C.; McElwain, M. W.; Matsuo, T.; Turner, E. L.; Mayama, S.; Akiyama, E.; Uyama, T.; Nakagawa, T.; Kudo, T.; Kusakabe, N.; Hashimoto, J.; Abe, L.; Brander, W.; Egner, S.; Feldt, M.; Goto, M.; Grady, C. A.; Guyon, Olivier; Hayano, Y.; Hayashi, M.; Hayashi, S. S.; Henning, T.; Hodapp, K. W.; Ishii, M.; Iye, M.; Kandori, R.; Knapp, G. R.; Kwon, J.; Miyama, S.; Morino, J.; Moro-Martin, A.; Nishimura, T.; Pyo, T.; Serabyn, E.; Suenaga, T.; Suto, H.; Suzuki, R.; Takahashi, Y. H.; Takami, M.; Takato, N.; Terada, H.; Thalmann, C.; Watanabe, M.; Takami, H.; Usuda, T.; Tamura, M.

In: Astrophysical Journal, Vol. 865, No. 2, 152, 01.10.2018.

Research output: Contribution to journalArticle

Mizuki, T, Kuzuhara, M, Mede, K, Schlieder, JE, Janson, M, Brandt, TD, Hirano, T, Narita, N, Wisniewski, J, Yamada, T, Biller, B, Bonnefoy, M, Carson, JC, McElwain, MW, Matsuo, T, Turner, EL, Mayama, S, Akiyama, E, Uyama, T, Nakagawa, T, Kudo, T, Kusakabe, N, Hashimoto, J, Abe, L, Brander, W, Egner, S, Feldt, M, Goto, M, Grady, CA, Guyon, O, Hayano, Y, Hayashi, M, Hayashi, SS, Henning, T, Hodapp, KW, Ishii, M, Iye, M, Kandori, R, Knapp, GR, Kwon, J, Miyama, S, Morino, J, Moro-Martin, A, Nishimura, T, Pyo, T, Serabyn, E, Suenaga, T, Suto, H, Suzuki, R, Takahashi, YH, Takami, M, Takato, N, Terada, H, Thalmann, C, Watanabe, M, Takami, H, Usuda, T & Tamura, M 2018, 'Orbital Characterization of GJ1108A System, and Comparison of Dynamical Mass with Model-derived Mass for Resolved Binaries', Astrophysical Journal, vol. 865, no. 2, 152. https://doi.org/10.3847/1538-4357/aada82
Mizuki, T. ; Kuzuhara, M. ; Mede, K. ; Schlieder, J. E. ; Janson, M. ; Brandt, T. D. ; Hirano, T. ; Narita, N. ; Wisniewski, J. ; Yamada, T. ; Biller, B. ; Bonnefoy, M. ; Carson, J. C. ; McElwain, M. W. ; Matsuo, T. ; Turner, E. L. ; Mayama, S. ; Akiyama, E. ; Uyama, T. ; Nakagawa, T. ; Kudo, T. ; Kusakabe, N. ; Hashimoto, J. ; Abe, L. ; Brander, W. ; Egner, S. ; Feldt, M. ; Goto, M. ; Grady, C. A. ; Guyon, Olivier ; Hayano, Y. ; Hayashi, M. ; Hayashi, S. S. ; Henning, T. ; Hodapp, K. W. ; Ishii, M. ; Iye, M. ; Kandori, R. ; Knapp, G. R. ; Kwon, J. ; Miyama, S. ; Morino, J. ; Moro-Martin, A. ; Nishimura, T. ; Pyo, T. ; Serabyn, E. ; Suenaga, T. ; Suto, H. ; Suzuki, R. ; Takahashi, Y. H. ; Takami, M. ; Takato, N. ; Terada, H. ; Thalmann, C. ; Watanabe, M. ; Takami, H. ; Usuda, T. ; Tamura, M. / Orbital Characterization of GJ1108A System, and Comparison of Dynamical Mass with Model-derived Mass for Resolved Binaries. In: Astrophysical Journal. 2018 ; Vol. 865, No. 2.
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abstract = "We report an orbital characterization of GJ1108Aab that is a low-mass binary system in the pre-main-sequence phase. Via the combination of astrometry using adaptive optics and radial velocity measurements, an eccentric orbital solution of e = 0.63 is obtained, which might be induced by the Kozai-Lidov mechanism with a widely separated GJ1108B system. Combined with several observed properties, we confirm that the system is indeed young. Columba is the most probable moving group, to which the GJ1108A system belongs, although its membership to the group has not been established. If the age of Columba is assumed for GJ1108A, the dynamical masses of both GJ1108Aa and GJ1108Ab (M dynamical,GJ1108Aa = 0.72 ± 0.04 M o and M dynamical,GJ1108Ab = 0.30 ± 0.03 M o) are more massive than what an evolutionary model predicts based on the age and luminosities. We consider that the discrepancy in mass comparison can be attributed to an age uncertainty; the system is likely older than stars in Columba, and effects that are not implemented in classical models such as accretion history and magnetic activity are not preferred to explain the mass discrepancy. We also discuss the performance of the evolutionary model by compiling similar low-mass objects in the evolutionary state based on the literature. Consequently, it is suggested that the current model on average reproduces the mass of resolved low-mass binaries without any significant offsets.",
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AU - Mizuki, T.

AU - Kuzuhara, M.

AU - Mede, K.

AU - Schlieder, J. E.

AU - Janson, M.

AU - Brandt, T. D.

AU - Hirano, T.

AU - Narita, N.

AU - Wisniewski, J.

AU - Yamada, T.

AU - Biller, B.

AU - Bonnefoy, M.

AU - Carson, J. C.

AU - McElwain, M. W.

AU - Matsuo, T.

AU - Turner, E. L.

AU - Mayama, S.

AU - Akiyama, E.

AU - Uyama, T.

AU - Nakagawa, T.

AU - Kudo, T.

AU - Kusakabe, N.

AU - Hashimoto, J.

AU - Abe, L.

AU - Brander, W.

AU - Egner, S.

AU - Feldt, M.

AU - Goto, M.

AU - Grady, C. A.

AU - Guyon, Olivier

AU - Hayano, Y.

AU - Hayashi, M.

AU - Hayashi, S. S.

AU - Henning, T.

AU - Hodapp, K. W.

AU - Ishii, M.

AU - Iye, M.

AU - Kandori, R.

AU - Knapp, G. R.

AU - Kwon, J.

AU - Miyama, S.

AU - Morino, J.

AU - Moro-Martin, A.

AU - Nishimura, T.

AU - Pyo, T.

AU - Serabyn, E.

AU - Suenaga, T.

AU - Suto, H.

AU - Suzuki, R.

AU - Takahashi, Y. H.

AU - Takami, M.

AU - Takato, N.

AU - Terada, H.

AU - Thalmann, C.

AU - Watanabe, M.

AU - Takami, H.

AU - Usuda, T.

AU - Tamura, M.

PY - 2018/10/1

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N2 - We report an orbital characterization of GJ1108Aab that is a low-mass binary system in the pre-main-sequence phase. Via the combination of astrometry using adaptive optics and radial velocity measurements, an eccentric orbital solution of e = 0.63 is obtained, which might be induced by the Kozai-Lidov mechanism with a widely separated GJ1108B system. Combined with several observed properties, we confirm that the system is indeed young. Columba is the most probable moving group, to which the GJ1108A system belongs, although its membership to the group has not been established. If the age of Columba is assumed for GJ1108A, the dynamical masses of both GJ1108Aa and GJ1108Ab (M dynamical,GJ1108Aa = 0.72 ± 0.04 M o and M dynamical,GJ1108Ab = 0.30 ± 0.03 M o) are more massive than what an evolutionary model predicts based on the age and luminosities. We consider that the discrepancy in mass comparison can be attributed to an age uncertainty; the system is likely older than stars in Columba, and effects that are not implemented in classical models such as accretion history and magnetic activity are not preferred to explain the mass discrepancy. We also discuss the performance of the evolutionary model by compiling similar low-mass objects in the evolutionary state based on the literature. Consequently, it is suggested that the current model on average reproduces the mass of resolved low-mass binaries without any significant offsets.

AB - We report an orbital characterization of GJ1108Aab that is a low-mass binary system in the pre-main-sequence phase. Via the combination of astrometry using adaptive optics and radial velocity measurements, an eccentric orbital solution of e = 0.63 is obtained, which might be induced by the Kozai-Lidov mechanism with a widely separated GJ1108B system. Combined with several observed properties, we confirm that the system is indeed young. Columba is the most probable moving group, to which the GJ1108A system belongs, although its membership to the group has not been established. If the age of Columba is assumed for GJ1108A, the dynamical masses of both GJ1108Aa and GJ1108Ab (M dynamical,GJ1108Aa = 0.72 ± 0.04 M o and M dynamical,GJ1108Ab = 0.30 ± 0.03 M o) are more massive than what an evolutionary model predicts based on the age and luminosities. We consider that the discrepancy in mass comparison can be attributed to an age uncertainty; the system is likely older than stars in Columba, and effects that are not implemented in classical models such as accretion history and magnetic activity are not preferred to explain the mass discrepancy. We also discuss the performance of the evolutionary model by compiling similar low-mass objects in the evolutionary state based on the literature. Consequently, it is suggested that the current model on average reproduces the mass of resolved low-mass binaries without any significant offsets.

KW - binaries: spectroscopic

KW - binaries: visual

KW - stars: imaging

KW - stars: individual (GJ1108A)

KW - stars: low-mass

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