Version 1
: Received: 8 April 2024 / Approved: 8 April 2024 / Online: 9 April 2024 (07:11:44 CEST)
How to cite:
Gabitova, I.A.; Miroshnichenko, A.S.; Zharikov, S.V.; Amantayeva, A.; Khokhlov, S.A. Doppler Tomography of the Circumstellar Disk of the Be Star κ Draconis. Preprints2024, 2024040580. https://doi.org/10.20944/preprints202404.0580.v1
Gabitova, I.A.; Miroshnichenko, A.S.; Zharikov, S.V.; Amantayeva, A.; Khokhlov, S.A. Doppler Tomography of the Circumstellar Disk of the Be Star κ Draconis. Preprints 2024, 2024040580. https://doi.org/10.20944/preprints202404.0580.v1
Gabitova, I.A.; Miroshnichenko, A.S.; Zharikov, S.V.; Amantayeva, A.; Khokhlov, S.A. Doppler Tomography of the Circumstellar Disk of the Be Star κ Draconis. Preprints2024, 2024040580. https://doi.org/10.20944/preprints202404.0580.v1
APA Style
Gabitova, I.A., Miroshnichenko, A.S., Zharikov, S.V., Amantayeva, A., & Khokhlov, S.A. (2024). Doppler Tomography of the Circumstellar Disk of the Be Star κ Draconis. Preprints. https://doi.org/10.20944/preprints202404.0580.v1
Chicago/Turabian Style
Gabitova, I.A., Ainash Amantayeva and Serik A. Khokhlov. 2024 "Doppler Tomography of the Circumstellar Disk of the Be Star κ Draconis" Preprints. https://doi.org/10.20944/preprints202404.0580.v1
Abstract
κ Draconis is a binary system with a classical Be star as the primary component. Its emission-line spectrum consists of hydrogen lines, notably the Hα line with a peak intensity ratio (V/R) variations phase-locked with the orbital period P = 61.55 days. Among binaries demonstrating the Be phenomenon, κ Dra stands out as one of a few systems with a discernible mass of its secondary component. Based on more than 200 spectra obtained in 2014 − 2023, we verified the physical parameters and constructed the mass function. We used part of these data obtained in 2014 − 2021 to investigate regions in the circumstellar disk of the primary component that emit the Hα line using the Doppler tomography method. The results show that the disk has a non-uniform density distribution with a prominent enhancement at Vy≈ 99 km s−1 and Vx≈−6 km s−1 that corresponds to a cloud-like source of the double-peaked Hα line profile. We argue that this enhancement’s motion is responsible for the periodic variations of the Hα V/R ratio, which is synchronised in orbital phase with the radial velocity (RV) of absorption lines from the atmosphere of the primary component.
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
,
