IAU Symposium Abstract S186-051T
Fundamental plane and merger scenario
Astronomical Institute, Tohoku University, Sendai, 980-77, Japan
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We perform a set of numerical simulations of galaxy mergers between
disk galaxies considerably abundant in interstellar gas
in order to explore physical meaning of the fundamental plane
of elliptical galaxies.
We consider that origin of global scaling relation in the FP
is closely related to
nonhomology both in spacial structure
and in kinematics
of elliptical galaxies formed by galaxy merging.
investigate dynamical and kinematical properties of
merger remnants and
found that rapidity of gas
consumption by star formation during galaxy merging can
density profile and relative importance of global rotation
of the remnants.
This result indicates that both structural nonhomology
and kinematical one
observed in elliptical galaxies result from
the difference in the rapidity of star formation between
the precursor mergers.
It is also found that the ratio of total dynamical mass to
luminous mass in the remnants, which is also regarded as an another
important determinant for the origin of the FP,
depends on the rapidity of gas consumption
by star formation in galaxy mergers.
These numerical results demonstrate that
the origin of the FP can be
essentially ascribed to the difference in
the star formation history between forming elliptical galaxies.