Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..483d&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 2, p. 483-488.
Astronomy and Astrophysics
Astrophysics
11
Gas Dynamics, H I Regions, Radio Emission, Spiral Galaxies, Star Formation, Angular Momentum, H Lines, Massive Stars
Scientific paper
Surprising radio properties of the Sc galaxy NGC 1792 revealed by VLA H I line observations are reported. Its H I gas mass is 1.2 x 10 exp 9 solar masses, i.e., about 2 per cent of the total dynamical mass. The H I gas of NGC 1792 is confined to the optically visible disk. The radio continuum, which peaks at the center of NGC 1792, is more extended along the minor axis than H I. Via a combination of these results with those at other wavelengths, it is found that the observations of NGC 1792 can be consistently interpreted either by ram pressure stripping of the outer parts of NGC 1792, or by gas accretion towards the turnover points of galactic rotation, probably caused by a transfer of angular momentum during the closest encounter with NGC 1808. Independent of the process depleting the outer parts of NGC 1792 of H I gas, gas condensation and turbulence appear to have initiated star formation further inward in the disk. It is suggested that massive star formation activity in giant H II regions in the disk might have led to the creation of a thick disk or halo of relativistic electrons similar, for example, to that in NGC 891.
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