UBV observations of R CrB-type variables and related objects

1980 ◽  
Vol 70 (2) ◽  
pp. 489-491 ◽  
Author(s):  
N. Kameswara Rao
Keyword(s):  
R Crb Type

scholarly journals A snapshot of the inner dusty regions of a R CrB-type variable

2007 ◽  
Vol 466 (2) ◽  
pp. L1-L4 ◽  
Author(s):  
I. C. Leão ◽  
P. de Laverny ◽  
O. Chesneau ◽  
D. Mékarnia ◽  
J. R. De Medeiros
Keyword(s):  
Type Variable ◽  
R Crb Type

Relation between Light Weakening and Equivalent Widths of Circumstellar NaI D-Lines in Stars with R CRB-Type Variability

2003 ◽  
Vol 12 (3) ◽  
Author(s):  
A. E. Rosenbush ◽  
A. V. Bondar
Keyword(s):  
High Resolution ◽  
Interstellar Medium ◽  
Similar Relation ◽  
Line Region ◽  
R Crb Type

AbstractHigh-resolution spectra in the NaI D-line region for tar­get stars with R Coronae Borealis type variability are analyzed. Two types of relations between light weakening and equivalent widths of circumstellar lines are found, one of them being considerably different from a similar relation for the interstellar medium.

scholarly journals SALT revisits DY Cen: a rapidly evolving strontium-rich single helium star

2020 ◽  
Vol 493 (3) ◽  
pp. 3565-3579 ◽  
Author(s):  
C Simon Jeffery ◽  
N Kameswara Rao ◽  
David L Lambert
Keyword(s):  
High Surface ◽  
Rapid Evolution ◽  
High Resolution Spectroscopy ◽  
Pulsation Period ◽  
Surface Hydrogen ◽  
Type Variable ◽  
Binary Orbit ◽  
R Crb Type ◽  
Helium Star ◽  
Process Element

ABSTRACT The hydrogen-deficient star DY Cen has been reported as an R CrB-type variable, an extreme helium star (with some hydrogen), and as a single-lined spectroscopic binary. It has been associated with a dramatic change in visual brightness and colour corresponding to a change in effective temperature ( Teff) of some 20 000 K in the last century. To characterize the binary orbit and  Teff changes more precisely, new high-resolution spectroscopy has been obtained with SALT. The previous orbital period is not confirmed; previous measurements may have been confused by the presence of pulsations. Including data from earlier epochs (1987, 2002, and 2010), self-consistent spectral analyses from all four epochs demonstrate an increase in  Teff from 18 800 to 24 400 K between 1987 and 2015. Line profiles demonstrate that the surface rotation has increased by a factor of 2 over the same interval. This is commensurate with the change in  Teff and an overall contraction. Rotation will exceed critical if contraction continues. The 1987 spectrum shows evidence of a very high abundance of the s-process element strontium. The very rapid evolution, non-negligible surface hydrogen and high surface strontium point to a history involving a very late thermal pulse. Observations over the next 30 yr should look for a decreasing pulsation period, reactivation of R CrB-type activity as the star seeks to shed angular momentum and increasing illumination by emission lines from nebular material ejected in the past.

scholarly journals Distribution of Light Minima of R Coronae Borealis Type Stars

1985 ◽  
Vol 87 ◽  
pp. 173-176
Author(s):  
A.E. Rosenbush
Keyword(s):  
Light Curves ◽  
Dust Formation ◽  
Time Intervals ◽  
Poisson Statistics ◽  
Carbon Abundance ◽  
Irregular Variable ◽  
R Crb Type ◽  
The Moment

Deep light minima of R CrB type stars are considered to occur due to the carbon abundance excess in the atmospheres of these stars, and condensation of carbon into graphite dust leads to light decrease (Zhilyaev et al., 1978). The cause and conditions of dust formation are not clear. Therefore, it is necessary to find out regularities in the occuring of light minima and to search for correlations between different parameters of this type stars. This paper deals with the time intervals between the series of consecutive light minima.A long series of observations of the R Coronae Borealis variables brightness allowed to study repeatedly their light curves in order to obtain their periodicity or other parameters in occuring of deep light minima. The work by Sterne (1935) was the first, in which the conclusion was made that R CrB is an irregular variable. Next investigations contained the analyses of light curves and calculations of the number of minima planned in the definite intervals, f.ex., 0-300, 300-600 days etc. (Howarth, 1977; 1978). Other papers (Tempesti et al., 1975) considered the duration of minima and maxima states. In all these investigations the time was counted off from the moment when a star reached a definite light decrease magnitude, f.ex., Δ m = 1m. The conclusions obtained were similar: the considered parameters were in agreement with Poisson statistics.

Infrared emission in R CrB type stars

Nature ◽  
1974 ◽  
Vol 252 (5480) ◽  
pp. 214-215 ◽  
Author(s):  
NAPOLEON MARON
Keyword(s):  
Infrared Emission ◽  
R Crb Type
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