Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-27T02:34:32.516Z Has data issue: false hasContentIssue false
  • English
  • Français

Interstellar gas around WO stars in the Galaxy and the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

Tatiana A. Lozinskaya
Tatiana A. Lozinskaya*
Affiliation:
Sternberg State Astronomical Institute, Moscow, USSR

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The four oxygen-sequence WR stars, Sand 1 in the Small Magellanic Cloud (SMC), Sand 2 in the Large Magellanic Cloud (LMC), and WR 102 and WR 142 in the Galaxy represent the latest stage of the evolution of massive stars (Sanduleak 1971, Barlow and Hummer 1982, Moffat et al. 1985). We have shown WR 102 to be a stripped CO core of a supermassive star (Dopita et al. 1990), probably seen only several thousand years before a SN explosion. The four stars are characterized by extremely energetic stellar winds –Vw from 4500 to 7400 km/s (Barlow and Hummer 1982, Dopita et al. 1990, Torres et al. 1986). Examination of the environments of WO stars leads to the conclusion that the four objects appear to be associated with optical and/or IR shell-like structures, although the short WO-superwind does not prevail in the shell's formation.

Type
The Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 438 - 439
Copyright
Copyright © Kluwer 1991 

References

Barlow, M.J. and Hummer, D.G. (1982), IAU Symp. 99 Wolf-Rayet Stars: Observations, Physics, Evolution , de Loore, C.W.H., Willis, A.J. (eds). p. 387.Google Scholar
Davies, R.D., Elliott, K.H. and Meaburn, J. (1976), Mem. R. Astron. Soc. 81, 89.Google Scholar
Dopita, M.A., Lozinskaya, T.A., McGregor, P.J. and Rawlings, S.J. (1990), Ap. J. 351, 563.Google Scholar
Dopita, M. and Lozinskaya, T.A. (1990), Ap. J. in press.Google Scholar
Graham, J.R. (1985), Observatory. 105, 7.Google Scholar
Kontizas, E., Morgan, D.H., Kontizas, M. and Dapergolas, A. (1988), A. Ap. 201, 208.Google Scholar
Loiseau, N., Klein, U., Greibe, A., Wielebinski, R. and Haynes, R.F. (1987), A. Ap. 178, 62.Google Scholar
Lozinskaya, T.A. (1990), IAU Symp. 143. in press.Google Scholar
Lozinskaya, T.A. and Repin, S.V. (1990), Sov. Astron. J. in press.Google Scholar
Meaburn, J. (1980), M.N.R.A.S. 192, 365.Google Scholar
Moffat, A.F.J., Breysacher, J. and Seggewiss, W. (1985), Ap. J. 292, 511.Google Scholar
McGee, R.X. and Newton, L.M. (1981/2), Proc. Astron. Soc. Austral. 4, 189 & 308.CrossRefGoogle Scholar
Pitault, A. (1981), A. Ap. 97, L5.Google Scholar
Sanduleak, N. (1971), Astrophys. J. 164, L71.Google Scholar
Torres, A.V., Conti, P.S. and Massey, P. (1986), Ap. J. 300, 379.Google Scholar
Turner, D.G. and Forbes, D. (1982), Publ. Astron. Soc. Pac. 94, 789.Google Scholar
Westerlund, B.E. (1964), M.N.R.A.S. 127, 429.Google Scholar