Issue |
A&A
Volume 692, December 2024
|
|
---|---|---|
Article Number | A27 | |
Number of page(s) | 12 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/202451004 | |
Published online | 29 November 2024 |
Searching for the mHz variability in the TESS observations of nova-like cataclysmic variables
Advanced Technologies Research Institute, Faculty of Materials Science and Technology in Trnava, Slovak University of Technology in Bratislava, Bottova 25, 917 24 Trnava, Slovakia
⋆ Corresponding author; andrej.dobrotka@stuba.sk
Received:
5
June
2024
Accepted:
13
September
2024
Aims. We investigated the fast optical variability of selected nova-like cataclysmic variables observed by the TESS satellite. We searched for break frequencies (fb) in the corresponding power density spectra (PDS). The goal is to study whether these systems in an almost permanent high optical state exhibit preferred fb around 1 mHz.
Methods. We selected non-interrupted light curve portions with durations of 5 and 10 days. We divided these portions into ten equally long light curve subsamples and calculated mean PDS. We searched for fb in the frequency interval from log(f/Hz) = −3.5 to −2.4. We defined as a positive detection when the fb was present in at least 50% of the light curve portions with a predefined minimum number of detections.
Results. We have measured fb in 15 nova-like systems and confirmed that the value of this frequency is clustered around 1 mHz with a maximum of the distribution between log(f/Hz) = −2.95 and −2.84. The confidence that this maximum is not a random feature of a uniform distribution is at least 96%. This is a considerable improvement on the previous value of 69%. We discuss the origin of these fb in the context of the sandwich model in which a central hot X-ray corona surrounds a central optically thick disc. This scenario could be supported by a correlation between the white dwarf mass and fb; the larger the mass, the lower the frequency. We see such a tendency in the measured data; however, the data are too scattered and based on a low number of measurements. Finally, it appears that systems with detected fb have a lower inclination than 60–75°. In higher-inclination binaries, the central disc is not seen and the PDS is dominated by red noise. This also supports the inner disc regions as being the source of the observed fb.
Key words: accretion / accretion disks / novae / cataclysmic variables / white dwarfs
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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