Other
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...438..950c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 438, no. 2, p. 950-956
Other
9
Interstellar Matter, Molecular Clouds, Nebulae, Shock Waves, Stellar Mass Ejection, Stellar Winds, Wolf-Rayet Stars, Astronomical Models, Carbon Monoxide
Scientific paper
We discuss two possible cases to explain the parabolic arc in the nebula NGC 2359 as a bow shock structure. In case A, the progenitor of the WN star HD 56925 may have evolved along the sequence: O goes to RSG goes to WN, while moving supersonically with respect to the Interstellar Medium (ISM). About 7 x 104 yr ago, the progenitor switched to the WN stage and began to blow a fast wind which drove a new bubble into the slow RSG wind, but some interstellar clumps might have been left within the bubble. At present, the spherical shock is intersecting with the bow shock in the east, forcing its way through the latter. It is shown that the radiation energy of the outer structure (i.e., bow shock shell) comes from the UV photons that escape from the inner bubble. In case B the bow shock may be powered by another star and collide with the eastern molecular clouds. They are all located in the foreground of the spherical shell and HD 56925.
Chen Yang
Qu Qin-Yue
Wang Zhen-Ru
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