Interstellar bubbles. II. Structure and evolution

Journal Article · Thu Dec 01 04:00:00 EST 1977 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/155692· OSTI ID:5300346

Weaver, R; McCray, R; Castor, J; Shapiro, P; Moore, R

We present the detailed structure of the interaction of a strong stellar wind with the interstellar medium. First we give an adiabatic similarity solution, which is applicable at early times. Second, we derive a similarity solution, including the effects of thermal conduction between the hot (Tapprox. =10/sup 6/ K) interior and the cold shell of swept-up interstellar matter. We then modify this solution to include the effects of radiative energy losses. We calculate the evolution of an interstellar bubble, 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. 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.

• Research Organization: Department of Physics and Astrophysics, University of Colorado
• OSTI ID: 5300346
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 218:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640105* -- Astrophysics & Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ADIABATIC PROCESSES
COOLING
COSMIC GASES
COSMIC RADIO SOURCES
ENERGY TRANSFER
FLUID MECHANICS
FLUIDS
GASES
H2 REGIONS
HEAT TRANSFER
HYDRODYNAMICS
INSTABILITY
INTERSTELLAR SPACE
IONIZATION
MECHANICS
RADIATIVE COOLING
RAYLEIGH-TAYLOR INSTABILITY
SPACE
STELLAR WINDS
THERMAL CONDUCTION