@article {28362,
	title = {The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study},
	volume = {507},
	year = {2021},
	month = {2021/11/1},
	pages = {5805 - 5819},
	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 $K_2=126.4 \pm 0.9 \, \mathrm{km}\, \mathrm{s}^{-1}$ and an orbital period $P=1.996872 \pm 0.000009 \, \mathrm{d}$. We refine the projected rotational velocity of the donor star to $v_\mathrm{rot} \sin i = 52 \pm 2 \, \mathrm{km}\, \mathrm{s}^{-1}$ that, together with K<SUB>2</SUB>, provides a donor star to white dwarf mass ratio q = M<SUB>2</SUB>/M<SUB>1</SUB> = 0.38 {\textpm} 0.03. We also determine the orbital inclination of the system by modelling the phase-folded ellipsoidal light curve and obtain i = 67{\textdegree} {\textpm} 5{\textdegree}. The resulting dynamical masses are $M_{1}=1.03^{+0.16}_{-0.11} \, \mathrm{M}_{\odot }$ and $M_2 = 0.39^{+0.07}_{-0.06} \, \mathrm{M}_{\odot }$ 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 Alfv{\'e}n radius in quiescence and during dwarf nova outburst.},
	keywords = {Accretion, accretion discs, Astrophysics - Solar and Stellar Astrophysics, binaries: close, CATACLYSMIC VARIABLES, Novae, stars: individual: GK Persei (Nova Persei 1901)},
	isbn = {0035-8711},
	url = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.5805A},
	author = {{\'A}lvarez-Hern{\'a}ndez, A. and Torres, M. A. P. and Rodr{\'\i}guez-Gil, P. and Shahbaz, T. and Anupama, G. C. and Gazeas, K. D. and Pavana, M. and Raj, A. and Hakala, P. and Stone, G. and Gomez, S. and Jonker, P. G. and Ren, J. -J. and Cannizzaro, G. and Pastor-Marazuela, I. and Goff, W. and Corral-Santana, J. M. and Sabo, R.}
}
