C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:04:18

2011A&A...532A...9A - Astronomy and Astrophysics, volume 532A, 9-9 (2011/8-1)

The structure and kinematics of the ISM around HD 192281.


Abstract (from CDS):

This work aims at investigating the interaction of HD192281 (O5 Vn((f))p) with its local ISM. The purpose is to analyse the effects that a massive star has on the structure and kinematics of its surrounding gas. To carry out this study, we used high-resolution radio continuum and 21-cm HI line data from the Canadian Galactic Plane Survey (CGPS). This data base was complemented with radio continuum, infrared, and molecular data retrieved from available surveys. Given that HD192281 is very likely a runaway star, we attempt to establish whether the observed HI distribution can be interpreted in terms of a simple bow shock model. Analysis of the HI data shows the presence of an HI feature likely to be associated with HD192281. This feature remains detectable from ∼5 to -10km/s. At the most negative radial velocities, the shape of the HI feature is highly reminiscent of a bow shock structure seen projected onto the plane of the sky. This feature has counterparts at radio-continuum, infrared, and CO emissions. The analysis of the radio continuum data suggests a thermal spectrum for the gas related to this structure.

Abstract Copyright:

Journal keyword(s): stars: individual: HD192281 - stars: mass-loss - stars: winds, outflows - ISM: bubbles - ISM: structure

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 HD 14434 Em* 02 21 52.4122106464 +56 54 18.032877629 7.87 8.65 8.49 8.29 8.20 O5.5Vnn((f))p 169 0
2 IRAS 20097+4005 * 20 11 30.2753824400 +40 14 14.602631959           ~ 3 0
3 V* V2011 Cyg SB* 20 12 33.1205906584 +40 16 05.442931142 7.32 7.85 7.55     O4.5V(n)((f)) 195 0
4 Ass Cyg OB 8 As* 20 15 +40.9           ~ 63 0
5 NAME gam Cyg SNR SNR 20 20 17.100 +40 26 09.00           ~ 200 2

    Equat.    Gal    SGal    Ecl

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