Abstract
Time-resolved, optical spectrophotometric observations of the Hα emission line in the cataclysmic variable V442 Oph are presented, and a long-term orbital ephemeris is derived. A method designed to quantify and locate the line-flickering activity in accretion disks is proposed on the basis of Doppler tomography techniques, and the line profile variability is explored. We found that the stochastic emission-line fluctuations in this system are the result of flaring activity at specific locations in the accretion disk. Such activity seems to be inhibited or damped for intrinsic gas velocities below 250 km s-1.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
