Physical parameters of superhumps in five dwarf nova systems based on TESS observations
| Dzygunenko, A, Baransky, O, Krushevska, V |
| Kinemat. fiz. nebesnyh tel (Online) 2025, 41(5):3-18 |
| https://doi.org/10.15407/kfnt2025.05.003 |
| Language: Ukrainian |
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, we determined the superhump periods (Psh) and orbital periods (Porb) for three SU UMa-type systems. For Gaia21djh, we obtained Psh = 0.08214 days and Porb = 0.0786 days; 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, M2, and radii R1, 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 for Gaia21akq it was DP = 6.5 ± 0.6 days. 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. |
| Keywords: cataclysmic variables, dwarf novae, outbursts, photometry, superhumps, TESS |
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