Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/101660
Title: Extensive photometry of the intermediate polar V1033 Cas (IGR J00234+6141)
Authors: Kozhevnikov, V. P.
Issue Date: 2019
Publisher: Springer
Citation: Kozhevnikov V. P. Extensive photometry of the intermediate polar V1033 Cas (IGR J00234+6141) / V. P. Kozhevnikov. — DOI 10.1007/s10509-019-3700-3 // Astrophysics and Space Science. — 2019. — Vol. 364. — Iss. 11. — 208.
Abstract: To measure the spin period of the white dwarf in V1033 Cas with high precision, we performed extensive photometry. Observations were obtained over 34 nights in 2017. The total duration of the observations was 143 h. We found that the spin period of the white dwarf is equal to 563.11633±0.00010s. Using this period, we derived the oscillation ephemeris with a long validity of 100 years. The spin oscillation semi-amplitude was stable and was equal to 95.5±1.3mmag. This is a very large semi-amplitude of the spin oscillation among intermediate polars, which have similar and lesser spin periods. This large semi-amplitude suggests that the system is noticeably inclined. The spin pulse profile was sinusoidal with high accuracy. This may mean that the spin oscillation is produced by a single accretion curtain whereas the second accretion curtain may be obscured by the accretion disc. Despite the large amount of our observations, we did not detect sidebands. The semi-amplitudes of the undetected sideband oscillations do not exceed 10 mmag. The absence of sideband oscillations seems puzzling. We detected the orbital variability of V1033 Cas with a period of 4.0243±0.0028h and with a semi-amplitude of 55±4mmag. The orbital variability semi-amplitude seems large and also suggests that the system is noticeably inclined. Using our oscillation ephemeris and the times of spin pulse maximum obtained in the past, we found that the spin period is very stable. d P/ d t is most probably less than − 4 × 10 − 12. This contradicts the assumption that the white dwarf in V1033 Cas is not spinning at equilibrium. Our spin period and our oscillation ephemeris can be used for further investigations of the stability of the spin period in V1033 Cas. © 2019, Springer Nature B.V.
Keywords: NOVAE, CATACLYSMIC VARIABLES
STARS: INDIVIDUAL: V1033 CAS
STARS: OSCILLATIONS
URI: http://hdl.handle.net/10995/101660
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85075572411
PURE ID: 11349051
a67ad7e2-522f-4310-9bd4-8e44fc270114
ISSN: 0004640X
DOI: 10.1007/s10509-019-3700-3
Appears in Collections:Научные публикации, проиндексированные в SCOPUS и WoS CC

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