Mathematics
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993egte.conf..328r&link_type=abstract
In NASA. Ames Research Center, The Evolution of Galaxies and Their Environment p 328-329 (SEE N93-26706 10-90)
Mathematics
Boundary Conditions, Gravitational Fields, Hydrodynamics, Interstellar Matter, Mathematical Models, Stellar Mass, Stellar Winds, Finite Difference Theory, Rotation, Supernovae, Vapor Phases, Wind Velocity
Scientific paper
We have been developing detailed hydrodynamic models of the global interstellar medium in the hope of understanding the mass and volume occupied by various phases, as well as their structure and kinematics. In our model, the gas is modeled by one fluid while representative Pop 1 stars are modeled by a second fluid. The two fluids are coupled in that the gas forms into stars at a rate given by a Schmidt law while stellar mass loss returns matter into the gas phase (on a time scale of 100 Myr). Also, the stars heat the gas through stellar winds and the gas cools through optically thin radiation. The time behavior of these two fluids is studied in two spatial dimensions with the Eulerian finite difference numerical hydrodynamic code Zen. The two spatial dimensions are along the plane of a disk (x, total length of 2 kpc) and perpendicular to the disk (z, total height of +/- 15 kpc) and a galactic gravitational field in the z direction, typical of that at the solar circle, is imposed upon the simulation; self-gravity and rotation are absent. For the boundary conditions, outflow is permitted at the top and bottom of the grid (z = +/- 15 kpc) while periodic boundary conditions are imposed upon left and right sides of the grid. As initial conditions, we assumed a gaseous distribution like that seen for the H1 by earlier researchers, although the results are insensitive to the initial conditions. We have run simulations in which the heating due to stars, parameterized as a stellar wind velocity, a, is varied from low (a = 150 km/s), to intermediate (a = 300 km/s), to high (a = 600 km/s). Since the intermediate case is roughly equivalent to the Galactic energy injection rate from supernovae, this summary will concentrate on results from this simulation.
Bregman Joel N.
Norman Michael L.
Rosen Alexander
No associations
LandOfFree
Numerical modeling of the interstellar medium in galactic disks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Numerical modeling of the interstellar medium in galactic disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical modeling of the interstellar medium in galactic disks will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1260271