DY Per (CGCS 372) was suspected to be an R CrB star based on the photometry by Alksnis (1994). Subsequent photometric monitoring revealed a number of sudden light declines typical for R CrB variables superimposed on the 792-day cycle of long-period light variations (Alksnis et al. 2002). However, the temperature of this star is much lower than average for other R CrB stars. Moreover, the luminosity of DY Per was suspected to be lower than usually for R CrBs. Keenan & Barnbaum (1997) estimated Teff ≃ 3500 K using the standard criteria of spectral classification and a giant luminosity. DY Per was classified as R8, C4,5, C5,4p, and C-Hd 4.5 C26 (Keenan & Barnbaum, 1997). Alcock et al. (2001) revealed four stars similar to the Galactic variable DY Per among eight RCBs discovered in the Large Magellanic Cloud.
Stars; carbon; stars; winds; outflows; (stars;) circumstellar matter; stars; individual; DY Per
Alcock, C, Allsman R.A., Alves D.R., et al.: 2001, ApJ, 554, 298.
Alksnis A.: 1994, BaltA, 3, 410.
Alksnis A., Larionov V.M., Larionova L.V., et al.: 2002, BaltA, 11, 487.
Keenan P.C., Barnbaum C: 1997, PASP, 109, 969.
Zacs L., Chen W.P., Alksnis O., et al.: 2005, A&A, 438, L13.