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GS64-01-97: Expanding Supershell in the Milky Way

Published online by Cambridge University Press:  25 May 2016

S. Ehlerová ,
B. Jungwiert  and
J. Palouš
S. Ehlerová
Affiliation:
Astronomical Institute, Charles University Švédská 8, 150 00 Prague 5, Czech Republic
B. Jungwiert
Affiliation:
Astronomical Institute, Charles University Švédská 8, 150 00 Prague 5, Czech Republic
J. Palouš
Affiliation:
Astronomical Institute, Academy of Sciences Boční II 1401, 141 31 Prague 4, Czech Republic

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The expansion of shocked interstellar medium around an OB association is an example of the astrophysical blastwave (Ostriker and McKee, 1988). The thin, cold, shell-like structure expanding supersonically accumulates the ambient medium. We assume that the shell has the zero thickness at radius of the shockwave rs and that it expands at velocity vs. The shell is divided into elements described with equations of motion: d/dt(Mv s ) = dS[(P–Po ) + novo (v s –vo )]–Mg(R,z), where M and dS are the mass and the surface of it, P, Po are the inside and outside pressures, no,vo are density and velocity of the ambient medium and g(R,z) is the gravitational acceleration in the Galaxy. R, z are the galactocentric cylindrical coordinates. The mass of an element increases as long as the expansion velocity component normal to the shell, v⊥ exceeds the velocity of sound in the ambient medium M = v ⊥ nodS. The 3D model using the above infinitesimally thin shell approximation was developed by Palouš (1990, 1992) and Silich (1992).

Type
Chapter 7: How are we to Understand the Small Scale Structure of the ISM?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 621 - 622
Copyright
Copyright © Kluwer 1996 

References

Burton, W. B., 1976, Ann. Rev. Astron. Astrophys. 14, 275 Google Scholar
Hartmann, D., Burton, B. W., 1994, private communication Google Scholar
Heiles, C. (1979) ApJ, 299, 533 CrossRefGoogle Scholar
Ostriker, J.P., McKee, Ch. F., 1988, Rev. Mod. Phys. 60, 1 Google Scholar
Palouš, J., 1990, IAU Symp. 144, Poster proceedings, ed. Bloemen, H., p. 101 Google Scholar
Palouš, J., 1992, in Evolution of Interstellar Matter and Dynamics of Galaxies, eds Palouš, J., Burton, W. B., and Lindblad, P. O., Cambridge University Press, p. 65 Google Scholar
Silich, S., 1992, Astrophys. Space Sci. 195, 317 Google Scholar
Wouterloot, J. G. A., Brand, J., Burton, W. B., & Kwee, K. K., 1990, Astron. Astrophys. 230, 21 Google Scholar