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Moving shadows on the dusty disks of young stars. / Tambovtseva, L. V.; Grinin, V. P.; Weigelt, G.

в: Astronomy and Astrophysics, Том 448, № 2, 03.2006, стр. 633-639.

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

Harvard

Tambovtseva, LV, Grinin, VP & Weigelt, G 2006, 'Moving shadows on the dusty disks of young stars', Astronomy and Astrophysics, Том. 448, № 2, стр. 633-639. https://doi.org/10.1051/0004-6361:20053884

APA

Tambovtseva, L. V., Grinin, V. P., & Weigelt, G. (2006). Moving shadows on the dusty disks of young stars. Astronomy and Astrophysics, 448(2), 633-639. https://doi.org/10.1051/0004-6361:20053884

Vancouver

Tambovtseva LV, Grinin VP, Weigelt G. Moving shadows on the dusty disks of young stars. Astronomy and Astrophysics. 2006 Март;448(2):633-639. https://doi.org/10.1051/0004-6361:20053884

Author

Tambovtseva, L. V. ; Grinin, V. P. ; Weigelt, G. / Moving shadows on the dusty disks of young stars. в: Astronomy and Astrophysics. 2006 ; Том 448, № 2. стр. 633-639.

BibTeX

@article{c841385ee9dd404eb098668150a236b7,
title = "Moving shadows on the dusty disks of young stars",
abstract = "We investigate the formation of moving shadows on the circumbinary (CB) disk of young binary systems. Moving shadows can be created by a dusty disk wind of the secondary component. The densest parts of the dusty disk wind and the associated common envelope can be optically thick and may block the stellar radiation inside a certain solid angle, resulting in the appearance of a moving shadow zone. Its shape and size depends on the mass loss rate, the disk wind velocity, and optical properties of the dust. Our calculations show that the shadow zone is observable if the mass loss rate Ṁw is greater than 10-9 M⊙ per year. This shadow resembles a clock hand. If the orbit is an elliptical, the properties of this clock hand will change during the orbital motion of the secondary.",
keywords = "Accretion, accretion disks, Binaries: close, Circumstellar matter, Stars: formation, Stars: pre-main sequence",
author = "Tambovtseva, {L. V.} and Grinin, {V. P.} and G. Weigelt",
year = "2006",
month = mar,
doi = "10.1051/0004-6361:20053884",
language = "English",
volume = "448",
pages = "633--639",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "2",

}

RIS

TY - JOUR

T1 - Moving shadows on the dusty disks of young stars

AU - Tambovtseva, L. V.

AU - Grinin, V. P.

AU - Weigelt, G.

PY - 2006/3

Y1 - 2006/3

N2 - We investigate the formation of moving shadows on the circumbinary (CB) disk of young binary systems. Moving shadows can be created by a dusty disk wind of the secondary component. The densest parts of the dusty disk wind and the associated common envelope can be optically thick and may block the stellar radiation inside a certain solid angle, resulting in the appearance of a moving shadow zone. Its shape and size depends on the mass loss rate, the disk wind velocity, and optical properties of the dust. Our calculations show that the shadow zone is observable if the mass loss rate Ṁw is greater than 10-9 M⊙ per year. This shadow resembles a clock hand. If the orbit is an elliptical, the properties of this clock hand will change during the orbital motion of the secondary.

AB - We investigate the formation of moving shadows on the circumbinary (CB) disk of young binary systems. Moving shadows can be created by a dusty disk wind of the secondary component. The densest parts of the dusty disk wind and the associated common envelope can be optically thick and may block the stellar radiation inside a certain solid angle, resulting in the appearance of a moving shadow zone. Its shape and size depends on the mass loss rate, the disk wind velocity, and optical properties of the dust. Our calculations show that the shadow zone is observable if the mass loss rate Ṁw is greater than 10-9 M⊙ per year. This shadow resembles a clock hand. If the orbit is an elliptical, the properties of this clock hand will change during the orbital motion of the secondary.

KW - Accretion, accretion disks

KW - Binaries: close

KW - Circumstellar matter

KW - Stars: formation

KW - Stars: pre-main sequence

UR - http://www.scopus.com/inward/record.url?scp=33644937065&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20053884

DO - 10.1051/0004-6361:20053884

M3 - Article

AN - SCOPUS:33644937065

VL - 448

SP - 633

EP - 639

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

IS - 2

ER -

ID: 87426004