DY Centauri

DY Centauri

A blue band light curve for DY Centauri, adapted from Schaefer (2016)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
Right ascension 13h 25m 34.08s[2]
Declination −54° 14′ 43.1″[2]
Apparent magnitude (V) 13.2[3]
Characteristics
Spectral type C-Hd/B5-6Ie[4]
Variable type RCB (inactive)[1]
Astrometry
Radial velocity (Rv)21.30 ± 0.45[5] km/s
Distance23000 ly
(7000[6] pc)
Absolute magnitude (MV)-3[6]
Orbit[5](disputed)[7]
Period (P)39.66779 ± 0.0088 days
Eccentricity (e)0.44 ± 0.10
Periastron epoch (T)2445104.3364 ± 1.715
Argument of periastron (ω)
(secondary)		344.5 ± 16.7°
Semi-amplitude (K1)
(primary)		13.26 ± 1.18 km/s
Details
Mass0.8[5] M☉
Radius8[5] R☉
Surface gravity (log g)2.50 ± 0.12[3] cgs
Temperature24800 ± 600[3] K
Rotational velocity (v sin i)40 ± 5[3] km/s
Other designations
DY Centauri, 2MASS J13253407-5414431, AAVSO 1319–53[8]
Database references
SIMBADdata

DY Centauri is a variable star in the constellation Centaurus. From its brightness, it is estimated to be 7000 parsecs (23000 light-years) away from Earth.[6]

DY Centauri is classified as a R Coronae Borealis variable (RCB), a rare class of supergiant stars which show rapid and irregular decreases in brightness due to the formation of dust clouds on the stellar surface. However, DY Centauri is not an active RCB star anymore, and the last registered obscuration event was in 1934. This seems to be related to evolutionary changes in the star, represented by a very fast horizontal movement across the top of the HR diagram. Spectroscopic and photometric evidence show DY Centuari has increased its effective temperature from 5800 K in 1906 to 24800 K in 2010, while maintaining constant luminosity.[1] As consequence, its visual apparent magnitude has faded from about 11.75 in the beginning of the 20th century to 13.2 in 2010 (due to changes in the bolometric correction),[3] while its radius is calculated to have decreased from 100 R☉ to 8 R☉,[5] and rotation increased 2-fold, approaching critical velocity at which the star could be disrupted.[7] There are only three other known stars with this behavior, called hot RCB stars,[1] The DY Centauri is possibly experiencing an aftermath of the late thermal pulse during the asymptotic giant branch evolution stage.[7]

DY Centauri has a peculiar chemical composition and is poor in hydrogen and rich in helium and carbon, being identified as an extreme helium star (EHe). In comparison to other RCB and EHe stars, however, its hydrogen content is relatively high.[3][9] In the future, it is likely that the primary will evolve to a B subdwarf, a class of stars frequently found in binary systems.[5]

The spectrum of DY Centauri indicates the presence of a low density expanding nebula around it, formed by gas ionized by ultraviolet radiation from the star.[10] The nebula has an estimated dimension of 1.2 arcseconds and, from its expansion velocity, was probably created about a thousand years ago.[6]

  1. ^ a b c d Cite error: The named reference Schaefer2016 was invoked but never defined (see the help page).
  2. ^ a b Cite error: The named reference 2MASS was invoked but never defined (see the help page).
  3. ^ a b c d e f Cite error: The named reference Pandey2014 was invoked but never defined (see the help page).
  4. ^ Cite error: The named reference GCSSC was invoked but never defined (see the help page).
  5. ^ a b c d e f Cite error: The named reference Rao2012 was invoked but never defined (see the help page).
  6. ^ a b c d Cite error: The named reference Rao2013 was invoked but never defined (see the help page).
  7. ^ a b c Cite error: The named reference Jeffery2020 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Jeffery1993 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Rao1993 was invoked but never defined (see the help page).