V475 Sct (Nova Scuti 2003) – Binary or Triple System? |
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| Authors: | Drahomír Chochol Theodor Pribulla Nataly A Katysheva Sergei Yu Shugarov Igor M Volkov |
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| Institution: | (1) Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Slovakia;(2) Sternberg State Astronomical Institute, Universitetskij Prosp. 13, Moscow, 119992, Russia |
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| Abstract: | UBV RI photometry and 4600–9000 Å spectroscopy of nova V475 Sct taken in the first 3 month after discovery is presented. The object can be classified as a Fe II type slow nova with t 2,V = 48 days, t 3,V = 53 days. The absolute magnitude of the nova at maximum, its colour excess and distance were determined. The observed 13.4 day periodicity of flares can be explained by the mass transfer bursts from the red to the white dwarf, probably caused by the periastron passage of a third body. Two sets of absorptions are seen in the P Cyg-type Hα line profile. They arise in the expanding shell of the nova. |
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| Keywords: | stars binaries novae |
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