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Abstract <p>This study presents a detailed analysis of five cataclysmic variable systems of the dwarf nova class: Gaia21djh, Gaia19bwr, Gaia21akq, Gaia21enu, and Gaia18cjn. Using photometric data from the TESS space telescope and the ASAS-SN sky survey archive, the superhump periods (<i>P</i><sub>sh</sub>) and orbital periods (<i>P</i><sub>orb</sub>) for three SU UMa-type systems were determined. For Gaia21djh, <i>P</i><sub>sh</sub> = 0.08214 days and <i>P</i><sub>orb</sub> = 0.0786 days were obtained; similar values were determined for Gaia19bwr and Gaia21akq. For Gaia18cjn and Gaia21enu, the presence of stable superhumps was not confirmed, although Gaia18cjn shows an orbital period of <i>P</i><sub>orb</sub> = 0.189 days. The analysis of physical parameters, including mass ratios <i>q</i>, component masses <i>M</i><sub>1</sub> and <i>M</i><sub>2</sub> and radii <i>R</i><sub>1</sub> and <i>R</i><sub>2</sub> showed that all SU&#xa0;UMa systems have low <i>q</i> values (&lt;0.3) consistent with tidal instability. For example, Gaia21akq has <i>q</i> = 0.24 ± 0.03, which supports previous theoretical models. The study of superoutburst parameters revealed significant variability in the duration of different phases. Gaia19bwr exhibited the longest plateau phase duration (<i>D</i><sub><i>P</i></sub> = 9.6 ± 1.7 days), while it was <i>D</i><sub><i>P</i></sub> = 6.5 ± 0.6 days for Gaia21akq. The largest superoutburst amplitudes were observed in Gaia21djh (<i>A</i><sub><i>SO</i></sub> = 4.3 ± 0.2) and Gaia19bwr (4.2 ± 0.3). The obtained results are consistent with the thermal-tidal instability model for SU UMa-type systems and highlight the importance of high-precision photometric observations in studying accretion disk dynamics.</p>

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Physical Parameters of Superhumps in Five Dwarf Nova Systems Based on TESS Observations

  • 期刊论文

  • 发表日期：

    2025年9月8日

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  • A. Dzygunenko,
  • O. Baransky,
  • V. Krushevska

摘要

Abstract

This study presents a detailed analysis of five cataclysmic variable systems of the dwarf nova class: Gaia21djh, Gaia19bwr, Gaia21akq, Gaia21enu, and Gaia18cjn. Using photometric data from the TESS space telescope and the ASAS-SN sky survey archive, the superhump periods (Psh) and orbital periods (Porb) for three SU UMa-type systems were determined. For Gaia21djh, Psh = 0.08214 days and Porb = 0.0786 days were obtained; similar values were determined for Gaia19bwr and Gaia21akq. For Gaia18cjn and Gaia21enu, the presence of stable superhumps was not confirmed, although Gaia18cjn shows an orbital period of Porb = 0.189 days. The analysis of physical parameters, including mass ratios q, component masses M1 and M2 and radii R1 and R2 showed that all SU UMa systems have low q values (<0.3) consistent with tidal instability. For example, Gaia21akq has q = 0.24 ± 0.03, which supports previous theoretical models. The study of superoutburst parameters revealed significant variability in the duration of different phases. Gaia19bwr exhibited the longest plateau phase duration (DP = 9.6 ± 1.7 days), while it was DP = 6.5 ± 0.6 days for Gaia21akq. The largest superoutburst amplitudes were observed in Gaia21djh (ASO = 4.3 ± 0.2) and Gaia19bwr (4.2 ± 0.3). The obtained results are consistent with the thermal-tidal instability model for SU UMa-type systems and highlight the importance of high-precision photometric observations in studying accretion disk dynamics.