## Detalles de publicación

PP 06051

## Galactic Interstellar Gas Cloud Mass Functions: A Simple Quantitative Approach

Instituto de Astrofisica de Canarias

We present here a simple approach to understanding the gas cloud mass distribution

function by simulating formation and destruction of gas clouds and gas

clumps in the ISM. We include as relevant processes coagulation to form

bigger clouds, as well as disruption by collisions and the removal of gas

by collapse to form stars. We evolve initial sets of preexisting gas clumps

with a range of initial distribution functions (flat, Gaussian, fractal)

for their physical parameters, and with different geometrical forms

(spherical or elongated) for the individual clouds, and constrain them within

an imaginary box representing gravitational bounding, applying the kinematic laws of non-elastic collisions. The

results agree well with observations of the mass distribution function of

Galactic giant gas clouds if we choose a Gaussian for the initial distribution

function, and initial gas clouds which are quasi-spherical.

function by simulating formation and destruction of gas clouds and gas

clumps in the ISM. We include as relevant processes coagulation to form

bigger clouds, as well as disruption by collisions and the removal of gas

by collapse to form stars. We evolve initial sets of preexisting gas clumps

with a range of initial distribution functions (flat, Gaussian, fractal)

for their physical parameters, and with different geometrical forms

(spherical or elongated) for the individual clouds, and constrain them within

an imaginary box representing gravitational bounding, applying the kinematic laws of non-elastic collisions. The

results agree well with observations of the mass distribution function of

Galactic giant gas clouds if we choose a Gaussian for the initial distribution

function, and initial gas clouds which are quasi-spherical.