dc.contributor.author |
Alvarez-Hernandez, A |
|
dc.contributor.author |
Torre, M. A. P |
|
dc.contributor.author |
Rodriguez-Gil, P |
|
dc.contributor.author |
Shahbaz, T |
|
dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Gazeas, K. D |
|
dc.contributor.author |
Pavana, M |
|
dc.contributor.author |
Raj, A |
|
dc.contributor.author |
Hakala, P |
|
dc.contributor.author |
Stone, G |
|
dc.contributor.author |
Gomez, S |
|
dc.contributor.author |
Jonker, P. G |
|
dc.contributor.author |
Ren, J.- J |
|
dc.contributor.author |
Cannizzaro, G |
|
dc.contributor.author |
Pastor-Marazuela, I |
|
dc.contributor.author |
Goff, W |
|
dc.contributor.author |
Corral-Santana, J. M |
|
dc.contributor.author |
Sabo, R |
|
dc.date.accessioned |
2021-09-28T05:20:12Z |
|
dc.date.available |
2021-09-28T05:20:12Z |
|
dc.date.issued |
2021-11 |
|
dc.identifier.citation |
Monthly notices of the Royal Astronomical Society, Vol. 507, No. 4, pp. 5805–5819 |
en_US |
dc.identifier.issn |
1365-2966 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7863 |
|
dc.description |
Restricted Access |
en_US |
dc.description.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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Oxford University Press on behalf of Royal Astronomical Society |
en_US |
dc.rights |
© The Royal Astronomical Society |
|
dc.rights.uri |
https://doi.org/10.1093/mnras/stab2547 |
|
dc.subject |
Accretion |
en_US |
dc.subject |
Accretion discs |
en_US |
dc.subject |
Binaries: close |
en_US |
dc.subject |
Stars: individual: GK Persei (Nova Persei 1901) |
en_US |
dc.subject |
Novae |
en_US |
dc.subject |
Cataclysmic variables |
en_US |
dc.title |
The intermediate polar cataclysmic variable GK Persei 120 years after the nova explosion: a first dynamical mass study |
en_US |
dc.type |
Article |
en_US |