• Publications
  • Influence
Multiple Scattering in Clumpy Media. II. Galactic Environments
We present and discuss the results of new multiple-scattering radiative transfer calculations for three representative types of galactic environments, filled with either homogeneous or two-phase
The 1997 reference of diffuse night sky brightness
In the following we present material in tabular and graphical form, with the aim to allow the non-specialist to obtain a realistic estimate of the diffuse night sky brightness over a wide range of
Interstellar Depletions Updated: Where All the Atoms Went
Measures of the depletion of interstellar elements from the gas phase are usually derived by assuming that the general composition of the interstellar medium is identical to that of the Sun. A
Dust in the local interstellar wind
The gas-to-dust mass ratios found for interstellar dust within the solar system, versus values determined astronomically for the cloud around the solar system, suggest that large and small
The Amount of Interstellar Carbon Locked in Solid Hydrogenated Amorphous Carbon
Some form of hydrogenated amorphous carbon (HAC) is widely regarded as a likely component of dust in the diffuse interstellar medium of the Galaxy. The most direct observational evidence is the ∼2950
Dust and the transfer of stellar radiation within galaxies
We present and discuss models for the transfer of ultraviolet, visual, and near-infrared radiation within a variety of spherical geometries which are intended to approximate different types of dusty
Astrophysics of Dust
Currently ∼36 different absorption bands have been detected in the infrared spectra of cold, dense interstellar and circumstellar environments. These are attributed to the vibrational transitions of
Dust in Starburst Galaxies
To investigate the nature of starburst dust, we constructed a model of the stars and dust in starburst galaxies and applied it to 30 observed starburst spectral energy distributions (SEDs). The
Multiple scattering in reflection nebulae. I - A Monte Carlo approach. II - Uniform plane-parallel nebulae with foreground stars. III - Nebulae with embedded illuminating stars
A method is described which permits the calculation of the surface brightness distribution on a plane-parallel reflection nebula of uniform density, illuminated by a single star located in front of,