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Interstellar bubbles. II - Structure and evolution
Abstract
The detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented. First, an adiabatic similarity solution is given which is applicable at early times. Second, a similarity solution is derived which includes the effects of thermal conduction between the hot (about 1 million K) interior and the cold shell of swept-up interstellar matter. This solution is then modified to include the effects of radiative energy losses. The evolution of an interstellar bubble is calculated, including the radiative losses. The quantitative results for the outer-shell radius and velocity and the column density of highly ionized species such as O VI are within a factor 2 of the approximate results of Castor, McCray, and Weaver (1975). The effect of stellar motion on the structure of a bubble, the hydrodynamic stability of the outer shell, and the observable properties of the hot region and the outer shell are discussed.
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In the citing paper
“Clearly, the outflow becomes slower quickly in the presence of a CGM over a time scale of ∼ Myr.”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Weaver et al. 1977
In the citing paper
“The dynamical time-scale of the actual expansion would depend on the speed of the shock driven by this hot gas and can be much lower (Castor et al. 1975; Weaver et al. 1977).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Weaver et al. 1977
In the citing paper
“The higher value of σ compared to a blast wave case is due to a higher fraction of thermal energy stored in wind-driven bubbles (Weaver et al. 1977).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Weaver et al. 1977
In the citing paper
“Shocks driven by a constant energy source (namely, winds) are also self-similar and can be represented by the equation 10 with the modification Eb = L t , where L is the power of the energy source (Castor et al. 1975; Weaver et al. 1977).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Weaver et al. 1977
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THE CONNECTING MOLECULAR RIDGE IN THE GALACTIC CENTER
Hsieh, P.-Y., Ho, P. T. P., & Hwang, C.-Y. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/811/2/142 · Cited by 8
“One of the possible origin of the energy input is from multiple supernova explosions, which is able to release the energy into the ISM with efficiency up to 20% (Weaver et al. 1977; McCray & Kafatos 1987).”
Background
Metadata
- Authors
- Weaver, R., McCray, R., Castor, J., Shapiro, P., & Moore, R.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1977-12
- Volume
- 218
- Pages
- 377
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2089390834
- Cited by
- 1,736
- References
- 0
- Citations by year
- 2026: 49 · 2025: 74 · 2024: 77 · 2023: 70 · 2022: 81 · 2021: 73 · 2020: 67 · 2019: 58 · 2018: 69 · 2017: 52 · 2016: 68 · 2015: 47 · 2014: 76 · 2013: 70 · 2012: 64
- FWCI
- 11.64
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- The Astrophysical Journal (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
- Keywords
- interstellar bubbles, stellar winds, interstellar medium, heat conduction, radiative losses, hot interstellar gas, stellar kinematics, hydrodynamic stability
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