Shell-like H II regions

Details Shell-like H II regions Shell-like H II regions

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983afz....19..559l&link_type=abstract

(Astrofizika, vol. 19, July-Sept. 1983, p. 559-567) Astrophysics (ISSN 0571-7132), vol. 19, no. 3, Jan. 1984, p. 315-321. Transl

Astronomy and Astrophysics

Astrophysics

H Ii Regions, Interstellar Gas, Ionized Gases, Stellar Winds, Emission Spectra, Orion Nebula, Shells (Structural Forms)

Scientific paper

The structure of a H II region in the neighborhood of a star with wind is considered. In the initial stages, when the wind pressure is high, the ionized gas collects in a thin shell. After approximately 400,000 years the wind pressure on the shell has decreased so much that the shell structure of the H II region almost disappears. It is shown that the motions of ionized gas with high velocities (approximately 100 km/sec) observed in the Orion nebula and M 16 and M 17 could be due to stellar wind with power less than or approximately equal to 10 to the 36th erg/sec (the change in M being less than about 10 to the -6th solar mass/year).

Affiliated with

Also associated with

No associations

Rating

Shell-like H II regions does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Shell-like H II regions, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Shell-like H II regions will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1626585