Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
Volume 133, Issue 1023, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/1538-3873/abf32d
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Funding
- National Natural Science Foundation of China (NSFC) [U1931103]
- Chinese Academy of Sciences (CAS) [U1931103]
- NSFC [11703016]
- Young Scholars Program of Shandong University, Weihai [20820171006]
- Open Research Program of Key Laboratory for the Structure and Evolution of Celestial Objects [OP201704]
- Universidad Nacional Autonoma de Mexico (UNAM)
- DGAPA [PAPIIT IN 100918]
- National Development and Reform Commission
- NASA's Science Mission directorate
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The analysis of multi-color passband CCD light curves and TESS satellite data of two binary stars reveals different levels of magnetic activity and evolutionary states.
The multi-color passband CCD light curves of ASAS J124343+1531.7 and LINEAR 2323566 were first obtained by the 0.84 m Ritchey-Chretien telescope with follow up observations by the WIYN 0.90 m Cassegrain telescope. The data from the Transiting Exoplanet Survey Satellite of ASAS J124343+1531.7 was also applied for subsequent analysis. By analyzing the data through the W-D program, their mass ratios and fill-out factors were determined as 3.758, 1.438 and 31.8%, 14.9%, respectively. ASAS J124343+1531.7 is a W-subtype median contact binary, while LINEAR 2323566 is a W-subtype shallow contact binary, and the asymmetric light curves prove that they both have the O'Connell effect, which is generally explained by magnetic activity. The equivalent widths of H- alpha lines were calculated, which show they certainly have magnetic activity. Moreover, LINEAR 2323566 has a stronger magnetic activity. The analysis of orbital period changes shows that ASAS J124343+1531.7 has a trend of secular period increase, which is generally explained by the mass transfer from the less massive to the more massive star. According to the estimated absolute parameters, their evolutionary states are discussed. The two components of ASAS J124343+1531.7 are both main sequence stars. While for LINEAR 2323566, the more massive star is a main sequence star, the less massive star has evolved out of main sequence and is over-luminous and over-sized.
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