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The interstellar medium local to HD 10125 (O9.7II)

Published online by Cambridge University Press:  26 May 2016

Silvina Cichowolski
Affiliation:
Instituto Argentino de Radioastronomía, C.C. 5, 1894 Villa Elisa, Buenos Aires, Argentina
E. Marcelo Arnal
Affiliation:
Instituto Argentino de Radioastronomía, C.C. 5, 1894 Villa Elisa, Buenos Aires, Argentina Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional La Plata, 1900 La Plata, Argentina
Cristina E. Cappa
Affiliation:
Instituto Argentino de Radioastronomía, C.C. 5, 1894 Villa Elisa, Buenos Aires, Argentina Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional La Plata, 1900 La Plata, Argentina
Sergey Pineault
Affiliation:
Département de Physique, Université Laval, Ste-Foy, Québec G1K 7P4, Canada Observatoire du Mont Mégantic, Notre-Dame-des-Bois, Canada
Nicole St-Louis
Affiliation:
Observatoire du Mont Mégantic, Notre-Dame-des-Bois, Canada Département de Physique, Université de Montréal, CP 6128, Succursale Centre Ville, Montréal, Québec H3C 3J7, Canada

Extract

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The structure and dynamics of the interstellar medium (ISM) are strongly affected by the action of massive stars. They deposit in the ISM a huge number of ionizing photons and transfer to it vast amounts of mechanical energy via their powerful stellar winds. As a consequence, massive stars create what is known as an interstellar bubble, i.e., a minimum in the gas distribution characterized by a low volume density and a high temperature, surrounded by an expanding envelope (Weaver et al. 1977). The star should be seen projected onto, or close to, the centre of the H i minimum.

Type
Part 4. Feedback from Massive Stars
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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Weaver, R.P., McCray, R., Castor, J.I., Shapiro, P.R., Moore, R.L. 1977, ApJ 218, 377.Google Scholar