Discovery of eclipses in the cataclysmic variable MASTER OT J232100.42+494614.0
Abstract
I performed photometric observations of the poorly studied cataclysmic variable MASTER OT J232100.42+494614.0 and discovered eclipses. I observed nine eclipses over two groups of closely spaced nights, separated by a 12-month interval. I precisely calculated the orbital period of the system to be Porb=0.212371533+\-0.000000069 days. For the eclipses, I created an ephemeris that is accurate for a long time span and suitable for analysing changes in the orbital period. The star's brightness outside of the eclipses varied between 15.61+\-0.02 and 18.04+\-0.05 mag. As the brightness decreased, the eclipses became more profound whereas its width remained unchanged. The average depth of eclipses was 1.36+\-0.03 mag, and the average width at half-depth was 0.0512(15) phases. I calculated the possible inclination of the orbit to be between 72.8 and 76.3 degrees, and the range of the average absolute V-band magnitude of the disc to be between 6.37+\-0.35 and 6.68+\-0.35 mag. Although the light curve of MASTER OT J232100.42+494614.0 from the ZTF survey showed insufficiently large outbursts with amplitudes less than 2.5 mag, it should be classified as a dwarf nova, as the average disc brightness and mass transfer rate are below the threshold for thermal instability.
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BibTeX
@misc{kozhevnikov2026discovery,
title = {{Discovery of eclipses in the cataclysmic variable MASTER OT J232100.42+494614.0}},
author = {V. P. Kozhevnikov},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.22443},
eprint = {2610.22443},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.22443},
}
RIS
TY - UNPB
TI - Discovery of eclipses in the cataclysmic variable MASTER OT J232100.42+494614.0
AU - V. P. Kozhevnikov
PY - 2026
DA - 2026/10/15
PB - arXiv
DO - 10.48550/arxiv.2610.22443
UR - https://arxiv.org/abs/2610.22443
AB - I performed photometric observations of the poorly studied cataclysmic variable MASTER OT J232100.42+494614.0 and discovered eclipses. I observed nine eclipses over two groups of closely spaced nights, separated by a 12-month interval. I precisely calculated the orbital period of the system to be Porb=0.212371533+\-0.000000069 days. For the eclipses, I created an ephemeris that is accurate for a long time span and suitable for analysing changes in the orbital period. The star's brightness outside of the eclipses varied between 15.61+\-0.02 and 18.04+\-0.05 mag. As the brightness decreased, the eclipses became more profound whereas its width remained unchanged. The average depth of eclipses was 1.36+\-0.03 mag, and the average width at half-depth was 0.0512(15) phases. I calculated the possible inclination of the orbit to be between 72.8 and 76.3 degrees, and the range of the average absolute V-band magnitude of the disc to be between 6.37+\-0.35 and 6.68+\-0.35 mag. Although the light curve of MASTER OT J232100.42+494614.0 from the ZTF survey showed insufficiently large outbursts with amplitudes less than 2.5 mag, it should be classified as a dwarf nova, as the average disc brightness and mass transfer rate are below the threshold for thermal instability.
ER -