@article{3031583,
    title = "The intermediate polar cataclysmic variable GK Persei 120 years after
the nova explosion: a first dynamical mass study",
    author = "Alvarez-Hernandez, A. and Torres, M. A. P. and Rodriguez-Gil, P. and and Shahbaz, T. and Anupama, G. C. and Gazeas, K. D. and Pavana, M. and Raj, and A. and Hakala, P. and Stone, G. and Gomez, S. and Jonker, P. G. and Ren, and J-J and Cannizzaro, G. and Pastor-Marazuela, I and Goff, W. and and Corral-Santana, J. M. and Sabo, R.",
    journal = "Monthly Notices of the Royal Astronomical Society",
    year = "2021",
    volume = "507",
    number = "4",
    pages = "5805-5819",
    publisher = "Oxford University Press",
    issn = "0035-8711, 1365-2966",
    doi = "10.1093/mnras/stab2547",
    keywords = "accretion, accretion discs; binaries: close; stars: individual: GK
Persei (Nova Persei 1901); novae, cataclysmic variables",
    abstract = "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."
}