Interstellar molecular clouds

Details Interstellar molecular clouds Interstellar molecular clouds

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sci...232..185b&link_type=abstract

Science (ISSN 0036-8075), vol. 232, April 11, 1986, p. 185-193.

Astronomy and Astrophysics

Astronomy

4

Interstellar Gas, Milky Way Galaxy, Molecular Clouds, Stellar Evolution, Astronomical Maps, Carbon Monoxide, Galactic Structure, Orion Nebula, Space Plasmas

Scientific paper

The physical properties of the molecular phase of the interstellar medium are studied with regard to star formation and the structure of the Galaxy. Most observations of molecular clouds are made with single-dish, high-surface precision radio telescopes, with the best resolution attainable at 0.2 to 1 arcmin; the smallest structures that can be resolved are of order 10 to the 17th cm in diameter. It is now believed that: (1) most of the mass of the Galaxy is in the form of giant molecular clouds; (2) the largest clouds and those responsible for most massive star formation are concentrated in spiral arms; (3) the molecular clouds are the sites of perpetual star formation, and are significant in the chemical evolution of the Galaxy; (4) giant molecular clouds determine the evolution of the kinematic properties of galactic disk stars; (5) the total gas content is diminishing with time; and (6) most clouds have supersonic internal motions and do not form stars on a free-fall time scale. It is concluded that though progress has been made, more advanced instruments are needed to inspect the processes operating within stellar nurseries and to study the distribution of the molecular clouds in more distant galaxies. Instruments presently under construction which are designed to meet these ends are presented.

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