PlumX Metrics
Embed PlumX Metrics

Css j213934.3-050020: A new double-mode high-amplitude δ scuti-type pulsating star

Publications of the Astronomical Society of the Pacific, ISSN: 0004-6280, Vol: 133, Issue: 1023
2021
  • 4
    Citations
  • 0
    Usage
  • 3
    Captures
  • 0
    Mentions
  • 0
    Social Media
Metric Options:   Counts1 Year3 Year

Metrics Details

Article Description

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 log g–T 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 = 6.8195 day, the first overtone f = 8.8709 day and 4 harmonics or linear combinations. The mass of J213934 is estimated as-0.27 1.83 M⊙. 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.

Provide Feedback

Have ideas for a new metric? Would you like to see something else here?Let us know