On the structure of intermediate- and high-velocity clouds

Details On the structure of intermediate- and high-velocity clouds On the structure of intermediate- and high-velocity clouds

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.203.1233d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 203, June 1983, p. 1233-1238.

Astronomy and Astrophysics

Astronomy

67

Early Stars, Interstellar Gas, Molecular Clouds, Neutral Gases, Stellar Evolution, Magnetic Fields, Stellar Radiation, Stellar Winds, Supernovae, Ultraviolet Radiation

Scientific paper

About 103 early-type stars may be formed in the halo every 107-108 yr by the collision of cloudlets within intermediate- and high-velocity clouds at high galactic latitude. Star formation occurs in cloudlets with column densities greater than a few times 1019 cm-2. Energy generated by these stars can accelerate the cloudlets and account for the observed velocity dispersion of 30 km s-1. These high-velocity clouds are not virially stable but could be confined by a magnetic field of at least 5×10-7 G in the hot coronal gas. Since the cloudlets' random kinetic energy could be renewed by successive bursts of star formation, the clouds, in principle, could be extremely long-lived.

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