The temporal and spatial behavior of the K I 7699 line profile is investigated. In particular, the asymmetries of the line profile at several residual intensities have been measured using the bisector method. Similar shapes are found in the bisector of the mean line profile as those obtained before for different positions on the solar disk. However

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Observations from a sample of six regions of star formation in the 244 GHz, J = 5-4 rotational transition of CS, together with previous results for lower frequencies, indicate that the line temperatures for this transition in the cases of OMC-1, M17 SW, W3(OH) and Ori B are consistent with constant density, large velocity gradient models. This in

Calculations of accreting magnetized neutron star atmospheres heated by the gradual deceleration of protons via Coulomb collisions are presented. Self consistent determinations of the temperature and density structure for different accretion rates are made by assuming hydrostatic equilibrium and energy balance, coupled with radiative transfer. The

An attempt is made to find the zodiacal cloud shape out of the ecliptic, on the basis of the Mujica et al (1980) establishment of the optical homogeneity of the medium in the ecliptic plane by means of ecliptic density and scattering functions. The consistency of the profile obtained is checked through the calculation of the brightness curves

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