On the Formation of Boxy and Disky Elliptical Galaxies

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dc.creatorBurkert, A.
dc.creatorNaab, Th.
dc.date1999-12-23
dc.date.accessioned2026-07-07T02:35:10Z
dc.date.available2026-07-07T02:35:10Z
dc.descriptionN-body simulations of major spiral-spiral mergers with different mass ratios q <= 4:1 are presented. All mergers lead to spheroidal stellar systems with de Vaucouleurs-like surface density profiles, resembling elliptical galaxies. The internal dynamical structure of the remnants does however depend critically on the adopted mass ratio. Equal-mass mergers with q <= 2:1 form radially anisotropic, slowly rotating systems with preferentially boxy isophotes. Unequal-mass mergers with q > 2:1 result in the formation of rotationally supported ellipticals with disky isophotes and small minor axis rotation. Projection effects lead in general to a large scatter in the kinematical and isophotal properties. If the observed dichotomy between boxy and disky ellipticals is a result of different mass ratios of the merger components massive ellipticals must have formed preferentially from equal-mass mergers in contrast to low-mass ellipticals which had to form from unequal-mass mergers.
dc.description4 pages, 1 postscript figure, uses newpasp.sty, to appear in ASP Conf. Proc. "Galaxy Dynamics"
dc.identifierhttps://arxiv.org/abs/astro-ph/9912489
dc.identifierhttp://arxiv.org/abs/astro-ph/9912489
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/15516
dc.subjectAstrophysics
dc.titleOn the Formation of Boxy and Disky Elliptical Galaxies
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