A model-independent irreducible tensor approach is presented for the np fusion reaction. Appropriate spin-observables are identified to determine empirically the initial spin singlet and triplet contributions to the ...

With the availability of very high-resolution stellar spectra, even small differences between line profiles resulting from complete redistribution and partial frequency redistribution may be important in the quantitative ...

The dynamical consequences of radiative energy transport on the evolution of gas confined to small-scale magnetic structures on the Sun are studied. Convective collapse, which transforms weak-field structures into intense ...

A general expression for the gravity darkening of the tidally and non-uniformly rotating Roche components of close binary systems is used to calculate the uniform rotational effects on line profiles in an expanding atmosphere. ...

The equation of radiative transfer in spherically symmetric shells with arbitrary internal sources is solved. The equation of transfer is integrated on a discrete grid of angle and radius. The size in angle coordinates is ...

We studied the transfer of line radiation in the distorted and expanding atmospheres of close binary components. We assumed that the distortion of the atmosphere is caused by self rotation and tidal force exerted by the ...

We report results from our 1-D radiative transfer modelling of dust in the hydrogen-deficient planetary nebula IRAS 18333–2357 located in the globular cluster M22. A spectral energy distribution was constructed from ...

We present a radiative transfer analysis of circumstellar dust shells around the Post-AGB stars HD 179821, HD 56126, HD 101584 and early R star HD 100764, using the code DUSTY. Parameters like mass-loss, shell inner radius, ...

The radiative transfer equation with Compton scattering is solved for spherically symmetric shells. The purpose of the study is to determine how gamma rays or X-rays change their energies and how they become reflected and ...

We present here the observations of the equatorial coronal hole made at 109 MHz on February 25, 1999 with the Gauribidanur Radioheliograph. The brightness temperature of this coronal hole is about 1:7£105 K.We compare our ...