Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...218..377w&link_type=abstract
Astrophysical Journal, Part 1, vol. 218, Dec. 1, 1977, p. 377-395.
Astronomy and Astrophysics
Astrophysics
1120
Interstellar Gas, Plasma Interactions, Stellar Winds, Adiabatic Flow, Bubbles, Conductive Heat Transfer, Early Stars, Energy Dissipation, Hydrodynamics, Ion Density (Concentration), Radiative Transfer, Stellar Motions
Scientific paper
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.
Castor John
McCray Richard
Moore Randy
Shapiro Paul
Weaver Richard
No associations
LandOfFree
Interstellar bubbles. II - Structure and evolution does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Interstellar bubbles. II - Structure and evolution, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Interstellar bubbles. II - Structure and evolution will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1417628