2019A&A...628A..20D


Query : 2019A&A...628A..20D

2019A&A...628A..20D - Astronomy and Astrophysics, volume 628A, 20-20 (2019/8-1)

Cloudlet capture by transitional disk and FU Orionis stars.

DULLEMOND C.P., KUFFMEIER M., GOICOVIC F., FUKAGAWA M., OEHL V. and KRAMER M.

Abstract (from CDS):

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 GM*/v2 (with v 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.

Abstract Copyright: © ESO 2019

Journal keyword(s): protoplanetary disks - stars: formation - ISM: clouds

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1371 0
2 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 704 1
3 V* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 690 0
4 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 1068 2
5 V* SU Aur Or* 04 55 59.3866872552 +30 34 01.499608092   10.33 9.30 9.17   G2IIIne 591 0
6 V* FU Ori Or* 05 45 22.3647842544 +09 04 12.291320064   10.72 9.60     F0Iab 816 1
7 V* Z CMa Ae* 07 03 43.1599411656 -11 33 06.209065836 10.51 9.99 8.80     B5/8eq+F5/7 579 3
8 V* V646 Pup Or* 07 50 35.5923145848 -33 06 23.905800180   13.96 12.65 12.04   ~ 70 0
9 HD 97048 Ae* 11 08 03.3109731720 -77 39 17.490777444 9.03 8.76 9.00   8.64 A0Vep 543 0
10 HD 100453 Ae* 11 33 05.5766482920 -54 19 28.547100696   8.09 7.79     F1Vn 285 1
11 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 807 1
12 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 643 1
13 HD 325367 Or* 16 03 05.4915085848 -40 18 25.426727676   11.40 8.50     M0 357 0
14 YLW 15 Y*O 16 27 26.906 -24 40 50.81           ~ 269 1

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