Álvarez-Hernández, A ; Torres, M A P ; Rodríguez-Gil, P ; Shahbaz, T ; Anupama, G C ; Gazeas, K D ; Pavana, M ; Raj, A ; Hakala, P ; Stone, G ; Gomez, S ; Jonker, P G ; Ren, J-J ; Cannizzaro, G ; Pastor-Marazuela, I ; Goff, W ; Corral-Santana, J M ; Sabo, R (2021) The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study Monthly Notices of the Royal Astronomical Society, 507 (4). pp. 5805-5819. ISSN 0035-8711
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Official URL: http://doi.org/10.1093/mnras/stab2547
Related URL: http://dx.doi.org/10.1093/mnras/stab2547
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 K2=126.4±0.9kms−1 and an orbital period P=1.996872±0.000009d. We refine the projected rotational velocity of the donor star to vrotsini=52±2kms−1 that, together with K2, provides a donor star to white dwarf mass ratio q = M2/M1 = 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° ± 5°. The resulting dynamical masses are M1=1.03+0.16−0.11M⊙ and M2=0.39+0.07−0.06M⊙ 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 Alfvén radius in quiescence and during dwarf nova outburst.
Item Type: | Article |
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Source: | Copyright of this article belongs to The Royal Astronomical Society |
Keywords: | accretion, accretion discs, binaries: close, stars: individual: GK Persei (Nova Persei 1901), novae, cataclysmic variables |
ID Code: | 130582 |
Deposited On: | 01 Dec 2022 10:58 |
Last Modified: | 01 Dec 2022 10:58 |
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