Friday, January 29, 2016

Flickering of Accreting White Dwarfs

Flickering of accreting white dwarfs: the remarkable amplitude - flux relation and disc viscocity


Zamanov et al


We analyze optical photometric data of short term variability (flickering) of accreting white dwarfs in cataclysmic variables (KR Aur, MV Lyr, V794 Aql, TT Ari, V425 Cas), recurrent novae (RS Oph and T CrB) and jet-ejecting symbiotic stars (CH Cyg and MWC 560). We find that the amplitude-flux relationship is visible over four orders of magnitude, in the range of fluxes from 1029 to 1033 erg s−1 \AA−1, as a "statistically perfect" correlation with correlation coefficient 0.96 and p-value ∼10−28. In the above range, the amplitude of variability for any of our 9 objects is proportional to the flux level with (almost) one and the same factor of proportionality for all 9 accreting white dwarfs with ΔF=0.36(±0.05)Fav, σrms=0.086(±0.011)Fav, and σrms/ΔF=0.24±0.02. Over all, our results indicate that the viscosity in the accretion discs is practically the same for all 9 objects in our sample, in the mass accretion rate range 2×10−11−2×10−7 M⊙ yr−1.

No comments:

Post a Comment

Note: Only a member of this blog may post a comment.