Outer disc edge: properties of low frequency aperiodic variability in ultracompact interacting binaries

TL;DR

This paper presents the first low frequency power spectral analysis of an ultracompact accreting white dwarf, revealing a low frequency break linked to the outer disk regions, aiding understanding of accretion flow dynamics.

Contribution

It introduces the first detection of low frequency variability in an ultracompact binary, connecting spectral features to accretion disk properties and providing a new observational constraint.

Findings

Detected a low frequency break at ~6.8e-7 Hz.

Identified a higher frequency component at ~1.3e-4 Hz.

Linked the low frequency break to the outer disk regions.

Abstract

Flickering, and more specifically aperiodic broad-band variability, is an important phenomenon used in understanding the geometry and dynamics of accretion flows. Although the inner regions of accretion flows are known to generate variability on relatively fast timescales, the broad-band variability generated in the outer regions have mostly remained elusive due to their long intrinsic variability timescales. Ultra-compact AM CVn systems are relatively small when compared to other accreting binaries and are well suited to search and characterise low frequency variability. Here we present the first low frequency power spectral analysis of the ultracompact accreting white dwarf system SDSS J1908$+$3940. The analysis reveals a low frequency break at $\sim 6.8 \times 10^{-7} $ Hz in the time-averaged power spectrum as well as a second higher frequency component with characteristic frequency of $\sim 1.3 \times 10^{-4} $ Hz. We associate both components to the viscous timescales within the disc through empirical fits to the power spectrum as well as analytical fits using the fluctuating accretion disk model. Our results show that the low frequency break can be associated to the disk outer regions of a geometrically thin accretion flow. The detection of the low frequency break in SDSS J1908$+$3940 provides a precedent for further detection of similar features in other ultracompact accreting systems. More importantly, it provides a new observable that can help constrain simulations of accretion flows.