# 2014A&A...566A..75O

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 Query : 2014A&A...566A..75O

2014A&A...566A..75O - Astronomy and Astrophysics, volume 566A, 75-75 (2014/6-1)

Radiation-pressure-driven dust waves inside bursting interstellar bubbles.

OCHSENDORF B.B., VERDOLINI S., COX N.L.J., BERNE O., KAPER L. and TIELENS A.G.G.M.

Abstract (from CDS):

Massive stars drive the evolution of the interstellar medium through their radiative and mechanical energy input. After their birth, they form bubbles'' of hot gas surrounded by a dense shell. Traditionally, the formation of bubbles is explained through the input of a powerful stellar wind, even though direct evidence supporting this scenario is lacking. Here we explore the possibility that interstellar bubbles seen by the Spitzer- and Herschel space telescopes, blown by stars with log(L/L)≲5.2, form and expand because of the thermal pressure that accompanies the ionization of the surrounding gas. We show that density gradients in the natal cloud or a puncture in the swept-up shell lead to an ionized gas flow through the bubble into the general interstellar medium, which is traced by a dust wave near the star, which demonstrates the importance of radiation pressure during this phase. Dust waves provide a natural explanation for the presence of dust inside HII bubbles, offer a novel method to study dust in HII regions and provide direct evidence that bubbles are relieving their pressure into the interstellar medium through a champagne flow, acting as a probe of the radiative interaction of a massive star with its surroundings. We explore a parameter space connecting the ambient density, the ionizing source luminosity, and the position of the dust wave, while using the well studied HII bubbles RCW 120 and RCW 82 as benchmarks of our model. Finally, we briefly examine the implications of our study for the environments of super star clusters formed in ultraluminous infrared galaxies, merging galaxies, and the early Universe, which occur in very luminous and dense environments and where radiation pressure is expected to dominate the dynamical evolution.

Journal keyword(s): ISM: bubbles - HII regions - infrared: ISM - hydrodynamics - ISM: kinematics and dynamics - dust, extinction

Full paper

 Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 IC 1848 OpC 02 51 25 +60 25.1   6.87 6.5     ~ 471 2
2 NAME 30 Dor Region reg 05 38.0 -69 06           ~ 210 0
3 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1884 1
4 IC 434 HII 05 41 -02.5           ~ 85 1
5 NAME Rosette Nebula HII 06 32 26.76 +04 47 37.1           ~ 472 1
6 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5636 6
7 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1634 0
8 RCW 82 HII 13 59.3 -61 27           ~ 30 0
9 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2847 4
10 SH 2-3 HII 17 12.4 -38 28           ~ 193 1
11 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1562 0
12 CORNISH G029.9559-00.0168 Y*O 18 46 04.18 -02 39 21.3           ~ 355 0
13 NAME Local Group GrG ~ ~           ~ 7772 0

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2022.10.02-02:42:57