The physics of the galactic halo gas

Details The physics of the galactic halo gas The physics of the galactic halo gas

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ap%26ss.152..223k&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 152, no. 2, Feb. 1989, p. 223-238.

Astronomy and Astrophysics

Astrophysics

3

Galactic Structure, H Ii Regions, Milky Way Galaxy, Absorption Spectra, Astronomical Models, High Temperature Gases, Ionized Gases, Star Formation

Scientific paper

The available data speak in favor of space and time inhomogeneity of gaseous corona of our Galaxy. The observed C IV and Si IV ions are formed mainly by fast photons and localized in H II-clouds of the galactic halo. On the other hand, the NV ions are thermally ionized and localized in the gas corresponding to a transformation of hot intercloud coronal gas in the H II-clouds. The H II-clouds exhibit downward the gas flow. The galactic fountain can eject the interstellar matter up to height of 1 kpc. Such ejections may be also displayed in C IV, Si IV, and partially NV, and partially NV absorptions. But large gaseous corona extending up to 3-5 kpc proves to be mass-unbalanced. It is possible that the existence of corona is evidence for violent star formation in the galactic disk in the recent past.

Affiliated with

Also associated with

No associations

Rating

The physics of the galactic halo gas 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 The physics of the galactic halo gas, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The physics of the galactic halo gas will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1884237