Tomographic Simulations of Accretion Disks in Cataclysmic Variables - Flickering and Wind

TL;DR

This paper simulates accretion disk Doppler maps in cataclysmic variables, including winds and flickering, to understand their effects on observed line profiles and improve interpretation of Doppler tomography.

Contribution

It introduces the first detailed simulations of accretion disk Doppler maps with winds and flickering effects in cataclysmic variables, enhancing understanding of their spectral features.

Findings

Optically thick lines and diffuse emission are key to single-peaked profiles.

Wind parameters significantly affect H-alpha line profiles.

Simulations suggest future models should include these effects for accurate Doppler tomography.

Abstract

Both continuum and emission line flickering are phenomena directly associated with the mass accretion process. In this work we simulate accretion disk Doppler maps including the effects of winds and flickering flares. Synthetic flickering Doppler maps are calculated and the effect of the flickering parameters on the maps is explored. Jets and winds occur in many astrophysical objects where accretion disks are present. Jets are generally absent among the cataclysmic variables (CVs), but there is evidence of mass loss by wind in many objects. CVs are ideal objects to study accretion disks and consequently to study the wind associated with these disks. We also present simulations of accretion disks including the presence of a wind with orbital phase resolution. Synthetic H-alpha line profiles in the optical region are obtained and their corresponding Doppler maps are calculated. The effect of the wind simulation parameters on the wind line profiles is also explored. From this study we verified that optically thick lines and/or emission by diffuse material into the primary Roche lobe are necessary to generate single peaked line profiles, often seen in CVs. The future accounting of these effects is suggested for interpreting Doppler tomography reconstructions.