Interstellar bubbles

Castor, J.; Weaver, Robert P.; McCray, Richard

doi:10.1086/181908

Cited by 663 publications

(645 citation statements)

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“…In what follows, we will examine in more detail this possibility and the models used to describe this formation and evolution. The shell formation and evolution as a result of the interaction of strong winds of a massive star with its ambient medium has been studied a long time ago by several authors (Dyson & de Vries 1972;Castor et al 1975;Steigman et al 1975;Weaver et al 1977, amongst others). The more favored (and complete) description of this interaction is the "standard model" (Weaver et al 1977) which considers that a star at rest releases a constant wind power, L W , that interacts with the ambient medium (assumed to be homogeneous).…”

Section: Discussionmentioning

confidence: 99%

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Valdez-Gutiérrez

Rosado

Георгиев

et al. 2001

A&A

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Abstract. We present Hα and [S ii] observations for the Local Group irregular galaxy IC 1613 using the PUMA scanning Fabry-Perot interferometer. Our goal is to analyze the kinematics of the ionized gas in the complex sample of superbubbles located in the whole extension of our field (10 ), which includes most of the optical emission of this galaxy, and to study the inter-relationship between young stellar associations and nebulae based on a previous study that we have made on the stellar associations of the central region of this galaxy. The ionized gas in this galaxy is distributed in classical H ii regions and in a series of superbubbles (also called giant shells) covering a large fraction of the optical extent of the galaxy. We present a catalog of kinematical properties of both the H ii regions of this galaxy and the superbubbles. We have also compared the kinematics of the ionized gas in H ii regions to search for possible dynamic differences between neutral and ionized gas.

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Section: Discussionmentioning

confidence: 99%

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Valdez-Gutiérrez

Rosado

Георгиев

et al. 2001

A&A

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“…Only the difference in the overall geometry (axi-symmetric in the former or spherically symmetric in the latter) enables us to find the bow shock. But, when taking the surrounding ISM having a density gradient, the structure of a stellar bubble described by Castor et al (1975) is altered. The resulting stellar bubble becomes ellipsoidal and the part at the high-density end will be brighter or the only visible part.…”

Section: Methodsmentioning

confidence: 99%

“…1, is in its longest snowplow stage divided into four parts centred upon the OB-star (Castor et al 1975): the innermost area (A) is an unshocked and freely expanding stellar wind, followed by a larger area (B) of shocked stellar wind. These hot regions, as if they were a snowplow (hence the name of this stage), have pushed together a thinner area (C) of shocked ISM.…”

Section: Scenariomentioning

confidence: 99%

“…This stellar wind with velocities of v ∞ ≈ 1000−3000 km s −1 transfers a great amount of mechanical energy to the surrounding ISM, comparable to a supernova explosion. As a result, OB-stars create a stellar bubble (Castor et al 1975) which structures the Interstellar Medium (ISM). This spherical bubble is altered when the OB-star is in motion, as wind and ISM interact directly.…”

Section: Introductionmentioning

confidence: 99%

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To see or not to see a bow shock

Brown¹,

Bomans²

2005

A&A

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Abstract. OB-stars have the highest luminosities and strongest stellar winds of all stars, which enables them to interact strongly with their surrounding ISM, thus creating bow shocks. These offer us an ideal opportunity to learn more about the ISM. They were first detected and analysed around runaway OB-stars using the IRAS allsky survey by van Buren et al. (1995, AJ, 110, 2614. Using the geometry of such bow shocks information concerning the ISM density and its fluctuations can be gained from such infrared observations. As to help to improve the bow shock models, additional observations at other wavelengths, e.g. Hα, are most welcome. However due to their low velocity these bow shocks have a size of ∼1 • , and could only be observed as a whole with great difficulties. In the light of the new Hα allsky surveys (SHASSA/VTSS) this is no problem any more. We developed different methods to detect bow shocks, e.g. the improved determination of their symmetry axis with radial distance profiles. Using two Hα-allsky surveys (SHASSA/VTSS), we searched for bow shocks and compared the different methods. From our sample we conclude, that the correlation between the direction of both proper motion and the symmetry axis determined with radial distance profile is the most promising detection method. We found eight bow shocks around HD 17505, HD 24430, HD 48099, HD 57061, HD 92206, HD 135240, HD 149757, and HD 158186 from 37 candidates taken from van Buren et al. (1995, AJ, 110, 2614. Additionally to the traditional determination of ISM parameters using the standoff distance of the bow shock, another approach was chosen, using the thickness of the bowshock layer. Both methods lead to the same results, yielding densities (∼1 cm −3 ) and the maximal temperatures (∼10 4 K), that fit well to the up-to-date picture of the Warm Ionised Medium.

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“…Our VLBA water maser and VLA continuum radio observations allow us to set a value for the shell radius and velocity with R 0 ≈ 500 AU, and V 0 ≈ 40 km s −1 respectively. To model the dynamics of the wind-driven shell, we have used equations given in Castor et al (1975) and Shull (1980). A detailed report of our calculations is given in Moscadelli et al 2007 (in preparation).…”

Section: Evidence For Expansionmentioning

confidence: 99%

Massive star-formation in G24.78+0.08 studied by means of maser VLBI and thermal interferometric observations

Moscadelli¹,

Goddi

Cesaroni³

et al. 2007

Proc. IAU

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Abstract. This work presents the results of VLBI observations of 6.7 GHz methanol and 22.2 GHz water masers towards the mm core A in the massive star-forming region G24.78+0.08. Comparing the maser with previous millimeter interferometric and recent continuum VLA observations, the physical properties and the gas kinematics of the G24 A core on linear scales from ∼100 AU to ∼0.1 pc are determined.

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Interstellar bubbles

Cited by 663 publications

References 0 publications

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

To see or not to see a bow shock

Massive star-formation in G24.78+0.08 studied by means of maser VLBI and thermal interferometric observations

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