BSN-VII: Photometric Light Curve Study of Three Cool, Large-Amplitude, Low Mass, W-Subtype Contact Binaries
Abstract
We present a comprehensive photometric study of three W UMa-type contact binary systems, V1104 Her, V1284 Her, and V2822 Ori, based on a combination of ground-based observations and space-based TESS photometry. The light curves were modeled using the BSN application under a contact configuration, with parameters and their uncertainties estimated through the Markov Chain Monte Carlo (MCMC) approach. The derived solutions indicate that the target systems are in a shallow-contact configuration. The target systems are classified as W-subtype contact binaries, with the more massive component cooler than its companion. The light curve of V1284 Her shows a pronounced O'Connell effect, which is reproduced by introducing a cool starspot on the primary component. Absolute parameters were estimated using the empirical parameter relationship between orbital period and semi-major axis, yielding component masses in the range $0.48−0.86\,M_\odot$ and confirming the low-mass nature of the systems. Orbital period variations were investigated using eclipse timings from the literature, ground-based observations, and TESS data by examining both linear and cyclic models. Statistical model comparison indicates that the cyclic model provides a better description of the eclipse timings for V1104 Her and V1284 Her, whereas the linear model is preferred for V2822 Ori, although the difference between the two models is relatively small.
Versions
Related
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BibTeX
@misc{poro2026bsnvii,
title = {{BSN-VII: Photometric Light Curve Study of Three Cool, Large-Amplitude, Low Mass, W-Subtype Contact Binaries}},
author = {Atila Poro and Raul Michel and Diana Zadkhosh and Ava Ekrami Fard and Kian Farhadi Sangdehi and Anica Lekic and Maxime Cellier and Chloé Da Graca Baptista and Paul Pointier and Fahri Alicavus and Elham Sarvari and Neslihan Alan},
howpublished = {arXiv},
year = {2026},
month = aug,
doi = {10.48550/arxiv.2608.29393},
eprint = {2608.29393},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2608.29393},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - BSN-VII: Photometric Light Curve Study of Three Cool, Large-Amplitude, Low Mass, W-Subtype Contact Binaries
AU - Atila Poro
AU - Raul Michel
AU - Diana Zadkhosh
AU - Ava Ekrami Fard
AU - Kian Farhadi Sangdehi
AU - Anica Lekic
AU - Maxime Cellier
AU - Chloé Da Graca Baptista
AU - Paul Pointier
AU - Fahri Alicavus
AU - Elham Sarvari
AU - Neslihan Alan
PY - 2026
DA - 2026/08/29
PB - arXiv
DO - 10.48550/arxiv.2608.29393
UR - https://arxiv.org/abs/2608.29393
AB - We present a comprehensive photometric study of three W UMa-type contact binary systems, V1104 Her, V1284 Her, and V2822 Ori, based on a combination of ground-based observations and space-based TESS photometry. The light curves were modeled using the BSN application under a contact configuration, with parameters and their uncertainties estimated through the Markov Chain Monte Carlo (MCMC) approach. The derived solutions indicate that the target systems are in a shallow-contact configuration. The target systems are classified as W-subtype contact binaries, with the more massive component cooler than its companion. The light curve of V1284 Her shows a pronounced O'Connell effect, which is reproduced by introducing a cool starspot on the primary component. Absolute parameters were estimated using the empirical parameter relationship between orbital period and semi-major axis, yielding component masses in the range $0.48−0.86\,M_\odot$ and confirming the low-mass nature of the systems. Orbital period variations were investigated using eclipse timings from the literature, ground-based observations, and TESS data by examining both linear and cyclic models. Statistical model comparison indicates that the cyclic model provides a better description of the eclipse timings for V1104 Her and V1284 Her, whereas the linear model is preferred for V2822 Ori, although the difference between the two models is relatively small.
ER -