An eccentric wave in the circumstellar disc of the Be/X-ray binary X Persei
| العنوان: | An eccentric wave in the circumstellar disc of the Be/X-ray binary X Persei |
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| المؤلفون: | N. A. Tomov, U. Wolter, K. A. Stoyanov, Dragomir Marchev, M. F. Bode, V. D. Marchev, L. Iliev, R. K. Zamanov, Ivanka Stateva, Y. M. Nikolov |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 499:3650-3659 |
| بيانات النشر: | Oxford University Press (OUP), 2020. |
| سنة النشر: | 2020 |
| مصطلحات موضوعية: | High Energy Astrophysical Phenomena (astro-ph.HE), Physics, media_common.quotation_subject, X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, circumstellar matter, stars: emission-line, Be, Asymmetry, stars: winds, outflows, X-rays: binaries, Astrophysics - Solar and Stellar Astrophysics, stars: individual: X Per, Space and Planetary Science, Eccentric, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, Eccentricity (mathematics), Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Planetary ring, media_common |
| الوصف: | We present spectroscopic observations of the Be/X-ray binary X Per obtained during the period December 2017 - January 2020 (MJD~58095 - MJD~58865). In December 2017 the $H\alpha$, $H\beta$, and HeI 6678 emission lines were symmetric with violet-to-red peak ratio $V/R \approx 1$. During the first part of the period (December 2017 - August 2018) the V/R-ratio decreased to 0.5 and the asymmetry developed simultaneously in all three lines. In September 2018, a third component with velocity $\approx 250$~km~s$^{-1}$ appeared on the red side of the HeI line profile. Later this component emerged in $H\beta$, accompanied by the appearance of a red shoulder in $H\alpha$. Assuming that it is due to an eccentric wave in the circumstellar disc, we find that the eccentric wave appeared first in the innermost part of the disc, it spreads out with outflowing velocity $v_{wave} \approx 1.1 \pm 0.2 $~km~s$^{-1}$, and the eccentricity of the eccentric wave is $e_{wave} \approx 0.29 \pm 0.07$. A detailed understanding of the origin of such eccentricities would have applications to a wide range of systems from planetary rings to AGNs. Comment: MNRAS (accepted) |
| تدمد: | 1365-2966 0035-8711 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_dedup___::e66c54244e4a61c050d1c4c496f56963 https://doi.org/10.1093/mnras/staa3065 |
| حقوق: | OPEN |
| رقم الأكسشن: | edsair.doi.dedup.....e66c54244e4a61c050d1c4c496f56963 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 13652966 00358711 |
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