Analysis of IUE spectra for the star V1016 Ori

We analyze IUE spectra of the star 1016 Ori. Together with previously obtained visible spectra, they have allowed the wavelength range from 1150 to 7000 Å to be studied. Atmospheric parameters of the star were refined: logg=4.5(1), T _eff=30000(1000) K, and ξ_t=15(5) km s^?1. We measured the equivalent widths of ～500 lines and used them to compute the chemical composition. It turned out that the He, B, Mg, P, and S abundances were nearly solar; Ne, Ti, and Cr were overabundant; and C, N, O, Al, Si, Mn, Fe, Ni, and Zn were underabundant.     

Some consequences of inhomogeneous dust formation in the principal shell of a nova

It is pointed out that dust formation in the principal shell of a nova in the equatorial belt only and the orientation of this belt relative to the line of sight may lead to an overestimation of the interstellar extinction and, consequently, to an overestimation of the luminosity of the nova. The orientation of the dust belt must also be taken into account in evaluating its contribution to the bolometric luminosity of the nova.Translated fromAstrofizika, Vol. 39, No. 2, pp. 237–241, April–June, 1996.     

Behavior of the Line Profiles of the Sodium Doublet and the Calcium Triplet in the Spectrum of R CrB in the Shallow Minima of 1998-1999

The behavior of profiles of the Na I D line and of the infrared Ca II triplet for the star R Coronae Borealis (R CrB) during shallow light minima of 1998-1999 is traced using high-resolution spectra. During a light maximum, the sodium lines had an absorption profile with a shift of —(2-4) km/sec. During a light minimum, a narrow emission feature, which has an almost constant absolute intensity and a shift of —(8-10) km/sec, and an intense circumstellar absorption feature, which has a variable profile and a variable relative shift corresponding to an increase to 220 km/sec in the velocity of mass ejection, appeared in the cores of absorption lines. For several days before the onset of a light minimum, all three calcium lines exhibited a narrow emission feature in the line core with a shift of —(1-5) km/sec. All the subsequent changes in a line involved mainly the shape of the absorption line profile. The narrow emission feature's absolute intensity and relative position were maintained during all our observations. The behavior of the Na I D line profiles can be described qualitatively within the framework of the model of a spherical dust shell.     

The system Bm Ori. V. Improved photometric elements

The times of individual minima taken from the literature are used to plot the dependence of O-C on revolution number for the eclipsing star BM Ori. A least squares fit of this plot yields the following photometric elements: Min I=JD2440265.331(5)+6.470524(3)·E. __________ Translated from Astrofizika, Vol. 51, No. 3, pp. 501–503 (August 2008).     

Infrared observations of the star R Cas

We present our JHKLM photometry for R Cas performed during 1988–2000. The pulsation period of R Cas is $P \approx 429\mathop .\limits^d 6$ , with the maximum IR brightness lagging behind the maximum visual brightness by ～0.2 P. The amplitude of light variations appreciably decreases with increasing wavelength at λ≤3 μm. At λ>3 μm, this decrease virtually ceases. There is a step on the ascending branch of IR JHK brightness. The K-L color index increases linearly with K magnitude: $K - L = 0.304K + 1\mathop .\limits^m 20$ . The color temperature dependence, T _K-L =f(K), is also linear: T _K?L = ?622K + 1100 K. In going from minimum to maximum, the K flux (as well as the bolometric flux) from the star and its color temperature T _K-L increase by a factor of ～2.2 and ～1.3, respectively.