The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study
: Alvarez-Hernandez A, Torres MAP, Rodriguez-Gil P, Shahbaz T, Anupama GC, Gazeas KD, Pavana M, Raj A, Hakala P, Stone G, Gomez S, Jonker PG, Ren JJ, Cannizzaro G, Pastor-Marazuela I, Goff W, Corral-Santana JM, Sabo R
Publisher: OXFORD UNIV PRESS
: 2021
: Monthly Notices of the Royal Astronomical Society
: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
: MON NOT R ASTRON SOC
: 507
: 4
: 5805
: 5819
: 15
: 0035-8711
DOI: https://doi.org/10.1093/mnras/stab2547
: https://research.utu.fi/converis/portal/detail/Publication/67638675
We present a dynamical study of the intermediate polar and dwarf nova cataclysmic variable GK Persei (Nova Persei 1901) based on a multisite optical spectroscopy and R-band photometry campaign. The radial velocity curve of the evolved donor star has a semi-amplitude K-2 = 126.4 +/- 0.9 km s(-1) and an orbital period P = 1.996872 +/- 0.000009 d. We refine the projected rotational velocity of the donor star to v(rot) sin i = 52 +/- 2 km s(-1) that, together with K-2, provides a donor star to white dwarf mass ratio q = M-2/M-1 = 0.38 +/- 0.03. We also determine the orbital inclination of the system by modelling the phase-folded ellipsoidal light curve and obtain i = 67 degrees +/- 5 degrees. The resulting dynamical masses are M-1 = 1.03(-0.11)(+0.16) M-circle dot and M-2 = 0.39(-0.06)(+0.07) M-circle dot at 68 per cent confidence level. The white dwarf dynamical mass is compared with estimates obtained by modelling the decline light curve of the 1901 nova event and X-ray spectroscopy. The best matching mass estimates come from the nova light curve models and an X-ray data analysis that uses the ratio between the Alfven radius in quiescence and during dwarf nova outburst.
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