Attenuation of Ultraviolet Radiation by Dust in Interstellar Clouds

Details Attenuation of Ultraviolet Radiation by Dust in Interstellar Clouds Attenuation of Ultraviolet Radiation by Dust in Interstellar Clouds

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994rmxaa..29..202e&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 29, 202

Astronomy and Astrophysics

Astronomy

1

Dust, Extinction, Radiative Transfer Scattering

Scientific paper

Se han obtenido soluciones de la ecuación de transporte para la dispersión coherente, no conservativa y anisotrópica para estimar la precisión de métodos aproximados, usados en modelos de nubes en que la luz es atenuada principalmente por el polvo. En los cálculos se ha aplicado el metodo de armónicos esféricos para distintos parámetros del polvo. Se ha explorado la posibilidad de descubrir cambios en las caracterísiticas del polvo mediante observaciones de regiones fotodisociadas. Se muestra que para altos valores del albedo de dispersión simple y del parametro de asimetria de Ia función de fase que son adecuados para el polvo galáctico, no es posible determinar variaciones de más de un factor de 2 en el cociente de gas a polvo. Solutions to the transfer equation for coherent, non-conservative, anisotropic scattering have been obtained in order to estimate the accuracy of approximate methods used in models of clouds where light is attenuated mostly by dust. In the calculations the spherical harmonic method has been applied for different grain parameters. The possibility of discovering changes of dust characteristics through observations of photodissociation regions has been considered. It is shown that for the high values of the single scattering albedo and the asymmetry parameter of the phase function for redistribution that appear to be appropriate for galactic dust, it is not possible to determine variations of more than a factor of 2 in the gas to dust ratio.

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