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Verfasst von:Dullemond, Cornelis [VerfasserIn]   i
 Küffmeier, Michael [VerfasserIn]   i
 Garrido Goicovic, Felipe [VerfasserIn]   i
 Fukagawa, Munetoshi [VerfasserIn]   i
 Oehl, Veronika [VerfasserIn]   i
 Kramer, Manuel [VerfasserIn]   i
Titel:Cloudlet capture by transitional disk and FU Orionis stars
Verf.angabe:C.P. Dullemond, M. Küffmeier, F. Goicovic, M. Fukagawa, V. Oehl, and M. Kramer
E-Jahr:2019
Jahr:29 July 2019
Umfang:13 S.
Teil:volume:628
 year:2019
 pages:A20
 extent:13
Fussnoten:Gesehen am 21.02.2020 ; Received: 12 January 2018
Titel Quelle:Enthalten in: Astronomy and astrophysics
Ort Quelle:Les Ulis : EDP Sciences, 1969
Jahr Quelle:2019
Band/Heft Quelle:628(2019) Artikel-Nummer A20, 13 Seiten
ISSN Quelle:1432-0746
Abstract:After its formation, a young star spends some time traversing the molecular cloud complex in which it was born. It is therefore not unlikely that, well after the initial cloud collapse event which produced the star, it will encounter one or more low mass cloud fragments, which we call “cloudlets” to distinguish them from full-fledged molecular clouds. Some of this cloudlet material may accrete onto the star+disk system, while other material may fly by in a hyperbolic orbit. In contrast to the original cloud collapse event, this process will be a “cloudlet flyby” and/or “cloudlet capture” event: A Bondi-Hoyle-Lyttleton type accretion event, driven by the relative velocity between the star and the cloudlet. As we will show in this paper, if the cloudlet is small enough and has an impact parameter similar or less than (with <i>v<i/><sub><i>∞<i/><sub/> being the approach velocity), such a flyby and/or capture event would lead to arc-shaped or tail-shaped reflection nebulosity near the star. Those shapes of reflection nebulosity can be seen around several transitional disks and FU Orionis stars. Although the masses in the those arcs appears to be much less than the disk masses in these sources, we speculate that higher-mass cloudlet capture events may also happen occasionally. If so, they may lead to the tilting of the outer disk, because the newly infalling matter will have an angular momentum orientation entirely unrelated to that of the disk. This may be one possible explanation for the highly warped/tilted inner/outer disk geometries found in several transitional disks. We also speculate that such events, if massive enough, may lead to FU Orionis outbursts.
DOI:doi:10.1051/0004-6361/201832632
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext ; Verlag: https://doi.org/10.1051/0004-6361/201832632
 Volltext: https://www.aanda.org/articles/aa/abs/2019/08/aa32632-18/aa32632-18.html
 DOI: https://doi.org/10.1051/0004-6361/201832632
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1690632895
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