TY - JOUR
TI - The intermediate polar cataclysmic variable GK Persei 120 years after
the nova explosion: a first dynamical mass study
AU - Alvarez-Hernandez, A.
AU - Torres, M. A. P.
AU - Rodriguez-Gil, P. and
AU - Shahbaz, T.
AU - Anupama, G. C.
AU - Gazeas, K. D.
AU - Pavana, M.
AU - Raj,
AU - A.
AU - Hakala, P.
AU - Stone, G.
AU - Gomez, S.
AU - Jonker, P. G.
AU - Ren,
AU - J-J
AU - Cannizzaro, G.
AU - Pastor-Marazuela, I
AU - Goff, W. and
AU - Corral-Santana, J. M.
AU - Sabo, R.
JO - Monthly Notices of the Royal Astronomical Society
PY - 2021
VL - 507
TODO - 4
SP - 5805-5819
PB - Oxford University Press
SN - 0035-8711, 1365-2966
TODO - 10.1093/mnras/stab2547
TODO - accretion, accretion discs; binaries: close; stars: individual: GK
Persei (Nova Persei 1901); novae, cataclysmic variables
TODO - 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.
ER -