V475 Sct (Nova Scuti 2003) Binary or Triple System?

Details V475 Sct (Nova Scuti 2003) Binary or Triple System? V475 Sct (Nova Scuti 2003) Binary or Triple System?

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.296..135c&link_type=abstract

Astrophysics and Space Science, Volume 296, Issue 1-4, pp. 135-139

Astronomy and Astrophysics

Astrophysics

Stars, Binaries, Novae

Scientific paper

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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