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• W3159058150 abstract "Abstract CSS J213934.3-050020 (hereafter J213934) was originally found as an EW-type eclipsing binary star with a period of 0.225456 days by Catalina Real-time Transient Survey. With the stellar atmospheric parameters from the LAMOST, it is found that the temperature is much higher than those of normal EW-type binaries and does not follow the period–temperature relation of EW-type eclipsing binary stars. To study the physical properties of the variable star, new B and V light curves were obtained by using the 70 cm telescope at the Lijiang station of Yunnan Observatories. It is detected that this variable star is a high-amplitude δ Scuti-type pulsating star rather than an EW-type eclipsing binary. On the <?CDATA $mathrm{log}gmbox{--}T$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mi>log</mml:mi> <mml:mi>g</mml:mi> <mml:mo>–</mml:mo> <mml:mi>T</mml:mi> </mml:math> diagram, J213934 lies inside the classical Cepheid instability strip where most δ Scuti stars are located. The results of pulsating frequency analysis show the fundamental frequency f 0 = 6.8195 day −1 , the first overtone f 1 = 8.8709 day −1 and 4 harmonics or linear combinations. The mass of J213934 is estimated as <?CDATA ${1.83}_{-0.21}^{+0.27}{M}_{odot }$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:msubsup> <mml:mrow> <mml:mn>1.83</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.21</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.27</mml:mn> </mml:mrow> </mml:msubsup> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> . The period is revised as 0.11272960 days by using 16 new determined times of light maximum. Meanwhile, it is discovered that its O − C curve shows an upward parabolic variation and a sinusoidal variation. The upward parabolic variation may be a part of a cyclic change or a long-time pulsation period increase caused by its evolution. The sinusoidal variation may be caused by the light-travel-time effect via the presence of a companion star." @default.
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• W3159058150 date "2021-04-29" @default.
• W3159058150 modified "2023-10-14" @default.
• W3159058150 title "CSS J213934.3-050020: A New Double-mode High-amplitude δ Scuti-type Pulsating Star" @default.
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• W3159058150 doi "https://doi.org/10.1088/1538-3873/abf32a" @default.
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