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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.

в: Astronomy Letters, Том 30, № 10, 2004, стр. 694-706.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Grinin, VP, Tambovtseva, LV & Sotnikova, NY 2004, 'Disk wind in the young binaries and the origin of the cyclic activity of young stars', Astronomy Letters, Том. 30, № 10, стр. 694-706. https://doi.org/10.1134/1.1808056

APA

Grinin, V. P., Tambovtseva, L. V., & Sotnikova, N. Y. (2004). Disk wind in the young binaries and the origin of the cyclic activity of young stars. Astronomy Letters, 30(10), 694-706. https://doi.org/10.1134/1.1808056

Vancouver

Grinin VP, Tambovtseva LV, Sotnikova NY. Disk wind in the young binaries and the origin of the cyclic activity of young stars. Astronomy Letters. 2004;30(10):694-706. https://doi.org/10.1134/1.1808056

Author

Grinin, V.P. ; Tambovtseva, L.V. ; Sotnikova, N.Ya. / Disk wind in the young binaries and the origin of the cyclic activity of young stars. в: Astronomy Letters. 2004 ; Том 30, № 10. стр. 694-706.

BibTeX

@article{caa62fdeabb143c8a3e709c8b51cfc38,
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",
keywords = "stars—young binaries - accretion - disk wind - activity cycles - UXORs",
author = "V.P. Grinin and L.V. Tambovtseva and N.Ya. Sotnikova",
year = "2004",
doi = "10.1134/1.1808056",
language = "English",
volume = "30",
pages = "694--706",
journal = "Astronomy Letters",
issn = "1063-7737",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "10",

}

RIS

TY - JOUR

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

Y1 - 2004

N2 - 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

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

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

U2 - 10.1134/1.1808056

DO - 10.1134/1.1808056

M3 - Article

VL - 30

SP - 694

EP - 706

JO - Astronomy Letters

JF - Astronomy Letters

SN - 1063-7737

IS - 10

ER -

ID: 5023953