Disk wind in the young binaries and the origin of the cyclic activity of young stars

V.P. Grinin, L.V. Tambovtseva, N.Ya. Sotnikova

Research output: Contribution to journalArticleResearchpeer-review

8 Citations (Scopus)

Abstract

We present the results of our numerical simulations of the cyclic brightness modulation in young binary systems with eccentric orbits and low-mass secondary components. We suggest that the binary components accrete matter from the remnants of the protostellar cloud, with the main accretor (according to current models) being the low-mass component. The brightness variations of the primary are attributable to the periodic extinction variations on the line of sight caused by the disk wind from the secondary and by the common envelope produced by this wind. The distribution of matter in the envelope was calculated in the ballistic approximation. When calculating the optical effects produced by the dust component of the disk wind, we adopted the dust-to-gas mass ratio of 1:100 characteristic of the interstellar medium and the optical parameters of the circumstellar dust typical of young stars. Our calculations show that the theoretical light curves for binaries with elliptical orbits exhibit a wider variety of sha
Original languageEnglish
Pages (from-to)694-706
JournalAstronomy Letters
Volume30
Issue number10
DOIs
StatePublished - 2004
Externally publishedYes

Keywords

  • stars—young binaries - accretion - disk wind - activity cycles - UXORs

Cite this

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title = "Disk wind in the young binaries and the origin of the cyclic activity of young stars",
abstract = "We present the results of our numerical simulations of the cyclic brightness modulation in young binary systems with eccentric orbits and low-mass secondary components. We suggest that the binary components accrete matter from the remnants of the protostellar cloud, with the main accretor (according to current models) being the low-mass component. The brightness variations of the primary are attributable to the periodic extinction variations on the line of sight caused by the disk wind from the secondary and by the common envelope produced by this wind. The distribution of matter in the envelope was calculated in the ballistic approximation. When calculating the optical effects produced by the dust component of the disk wind, we adopted the dust-to-gas mass ratio of 1:100 characteristic of the interstellar medium and the optical parameters of the circumstellar dust typical of young stars. Our calculations show that the theoretical light curves for binaries with elliptical orbits exhibit a wider variety of sha",
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Disk wind in the young binaries and the origin of the cyclic activity of young stars. / Grinin, V.P.; Tambovtseva, L.V.; Sotnikova, N.Ya.

In: Astronomy Letters, Vol. 30, No. 10, 2004, p. 694-706.

Research output: Contribution to journalArticleResearchpeer-review

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T1 - Disk wind in the young binaries and the origin of the cyclic activity of young stars

AU - Grinin, V.P.

AU - Tambovtseva, L.V.

AU - Sotnikova, N.Ya.

PY - 2004

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AB - We present the results of our numerical simulations of the cyclic brightness modulation in young binary systems with eccentric orbits and low-mass secondary components. We suggest that the binary components accrete matter from the remnants of the protostellar cloud, with the main accretor (according to current models) being the low-mass component. The brightness variations of the primary are attributable to the periodic extinction variations on the line of sight caused by the disk wind from the secondary and by the common envelope produced by this wind. The distribution of matter in the envelope was calculated in the ballistic approximation. When calculating the optical effects produced by the dust component of the disk wind, we adopted the dust-to-gas mass ratio of 1:100 characteristic of the interstellar medium and the optical parameters of the circumstellar dust typical of young stars. Our calculations show that the theoretical light curves for binaries with elliptical orbits exhibit a wider variety of sha

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JO - Astronomy Letters

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