THE COOL GALACTIC R Coronae BOREALIS VARIABLE DY Persei

Автор(и)

  • L. Zacs Institute of Atomic Physics and Spectroscopy, University of Latvia 19 Rainis blvd., Riga, LV-1586, Latvia, Latvia

DOI:

https://doi.org/10.18524/1810-4215.2005.18.98273

Ключові слова:

Stars, carbon, stars, winds, outflows, (stars, ) circumstellar matter, individual, DY Per

Анотація

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.

Посилання

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.

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Опубліковано

2017-04-10

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