Statistics – Computation
Scientific paper
Mar 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.219..305n&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 219, March 15, 1986, p. 305-331.
Statistics
Computation
130
Celestial Mechanics, Computational Astrophysics, Galaxies, Interstellar Gas, Star Formation, Star Formation Rate, Angular Momentum, Clouds, Collisions, Orbital Mechanics, Peculiar Galaxies, Supernovae, X Ray Astronomy
Scientific paper
Numerical simulations are performed for close encounters between a parent galaxy with a disc system and a perturbing galaxy. Cloud particles are used in constructing the disc of the parent galaxy in order to investigate the behavior of the interstellar gas clouds and the influence of the encounter on the star formation rate. Star formation is assumed to take place when a pair of cloud particles collide. In the most violent encounter investigated, the prominent bridge and tail are formed by the passage of the perturbing galaxy. As these structures develop, the star formation rate begins to rise because the cloud-cloud collisions become more frequent. The star formation rate reaches the maximum value of about 8 times as large as the preencounter value at about 300 million yr after the perigalactic passage of the perturber. This enhancement of the star formation activity explains fairly well the large scatter of the colors of the morphologically peculiar galaxies as well as their X-ray luminosities. Another important result is that the system of the gas clouds often makes a ring-like structure in the late stage of the encounter as a result of the cloud-cloud collisions.
Ishibashi Shoji
Noguchi Masayuki
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