Not Available

Recent data on, and interpretations of the Kleinmann-Low nebula are examined. It is suggested that associated high velocity gas is radiatively accelerated by a protostar in an early stage of premain-sequence contraction.

We have developed an automatic procedure to determine Teff and log g from the comparison of observational data with their theoretical values. After a description of the method we compare our results for a sample of 100 O-type stars with the classifications of Conti and Walborn and with the determinations of Morrison by photometric indices. The

A method for the determination of the intensity of the solar light scattered by a unit volume of interplanetary space and thus the density and phase functions of interplanetary dust is presented. The method involves the calculation of the scattered light intensity as a function of sun-particle distance and elongation angle from a partly assumed

Procedures were developed for extracting low resolution spectra while correcting for halation effects and scattered light within the instrument. To correct for halation, the spectra were extracted from the line-by-line images. Perpendicular scans of the image were fitted using an iterative least squares procedure with a known form function. The

Observations are reported of the J = 2 → 1 transitions of CO and 12C18O at 230 and 219 GHz respectively from a number of galactic sources. A map of the central 1/2° × 1/2° of the Orion A molecular cloud is presented. The spectra are interpreted to derive molecular densities and abundance ratios in the molecular clouds observed.