Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/823
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dc.contributor.authorNamboodiri, P. M. S-
dc.contributor.authorSastry, K. S-
dc.contributor.authorNarasimhan, K. S. V. S-
dc.date.accessioned2006-03-29T11:38:46Z-
dc.date.available2006-03-29T11:38:46Z-
dc.date.issued2006-02-
dc.identifier.citationAstrophysics and Space Science, Vol. 301, No. 1-4, pp. 3 - 9en
dc.identifier.issn0004-640X-
dc.identifier.urihttp://hdl.handle.net/2248/823-
dc.descriptionRestricted Access-
dc.descriptionThe original publication is available at springerlink.com-
dc.description.abstractNumerical simulations are performed to study the tidal effects of non-merging rapid head-on collision between a disk galaxy and a spherical galaxy. The disk consists of three components – a disk, a bulge and a halo – and the spherical galaxy is a Plummer model. The galaxies have the same dimensions with different mass ratios viz., 2, 1 and 0.5. They move in a rectilinear orbit with a relative velocity of 1000 km s−1. None of the simulations leads to the merger of the galaxies by tidal capture. The results of our simulations indicate that although tidal effects are sensitive to both the mass ratio and the inclination of the disk to the orbital plane, it is the mass ratio which is more important in producing tidal damage to the less massive galaxy. The spherical galaxy undergoes considerable tidal effects if the mass of the disk is same or larger. On the other hand the collisions in which the mass of the spherical galaxy is more, result in the formation of a ring structure after the closest approach and the structure disappears by the end of the simulationsen
dc.format.extent369158 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.subjectGalaxies:Interactionsen
dc.subjectMethods:Numericalen
dc.titleHead-on collision of disk-sphere galaxiesen
dc.typeArticleen
Appears in Collections:IIAP Publications

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