A spectrophotometric catalogue of 60 selected southern stars

Abstract

Abstract.The absolute spectral energy distribution data for 60 stars of the southern hemisphere in the range 310-1105 nm with a step of 2.5 nm are given. The observations were made in the Chilean and the Bolivian expeditions. The absolute calibration of the data is based on Vega. For variable stars L2 Pup, V806 Cen and RR Seo, the individual spectral distributions in the range 495-1105 nm at different Julian Days are given.

Microvariability and fast variability of stars. II. The semiregular red giants L2 Pup, 2 Cen, η Gem, and σ Lib

“…This assumption is confirmed by spectrophotometric measurements [10,11]. According to those measurements, no deviations from a normal distribution were found in the energy curves for the star-component system (the component was not resolved), which indicates that the component belongs to the same (or to a close) spectral class as the principal star, specifically, to class M. This assumption was made in the earlier work of Ref.…”

Physical parameters of the continuum radiating layer of the star L2 Pup

“…Spectrophotometric observations of the star L2 Pup were made in Bolivia during 1988-1989 on the AZT-7 telescope in the 485-1105 nm spectral range [7]. Table 1 lists the sequence numbers N of the observations and the Julian dates of the observations.…”

Physical parameters of the continuum emission layer of Mira type stars. II. Radii and expansion velocities

“…Using the observed quasimonochromatic magnitudes [4,5] and the temperatures of the emitting layers obtained in Ref. 1 for RR SCO, we have calculated the ratio of the radii of the layers in different phases of its cycle relative to the radius at the emission maximum, R N /R 3 .…”

“…Figure 2 shows the relationships among the quasimonochromatic fluxes from the star, λ m [4,5], at two wavelengths If we assume that the increased size of the emitting layer after the maximum is related to its expansion, then the distance moved by the layer during the time t between observations is equal to R ∆ , and it is easy to determine the mean velocity of the layer's motion, v , as…”