G132-12: A one-mode ZZ Ceti star located at the blue edge of instability strip

Chen, Jianxing; Fu, Jian-Ning; Niu, Hubiao; Li, Chun

doi:10.1016/j.newast.2019.101276

Cited by 3 publications

(2 citation statements)

References 15 publications

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“…As the frequency intervals between the three frequencies of G132-12 are approximately equal and the average is 3.98 ± 0.65 µHz, we identify that the three frequencies as a triplet due to rotation with l = 1. s. The mode with the period of 212.7 s detected by Gianninas et al (2006) and the one with the period of 212.69 s detected by Chen et al (2019) should be the split mode with m = −1.…”

Section: Amplitude Spectra and Frequency Analysismentioning

confidence: 97%

A triplet of the only pulsation mode detected in the DAV star G132-12

Su,

Fu,

Chen

et al. 2021

Preprint

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Hydrogen atmosphere pulsating white dwarfs, also known as DAV stars, are the most abundant type of pulsating white dwarfs. High-temperature DAV stars exhibit in general a small number of pulsation modes and stable frequencies. G132-12 is one of the pulsating hydrogen atmosphere white dwarf stars which lies close to the blue edge of the instability strip. Previous researches reported that G132-12 might have only one pulsation mode with the period of 212.69 s. To study the pulsation properties of G132-12 in detail, we carried out a bi-site observation campaign in October 2019. Time series photometric data were collected during around 154 hours in total. A Fourier Analysis reveals 3 frequencies which are identified as the triplet of a l = 1 g-mode pulsation with the period of 212.499 s. The rotational period is derived as P rot = 35.0 ± 6.7 hours and the inclination of the rotational axis to the line of sight is 70 • . G132-12 could be an ideal target for measuring the cooling scale of this white dwarf star with only one excited pulsation mode detected.

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Section: Amplitude Spectra and Frequency Analysismentioning

confidence: 97%

A triplet of the only pulsation mode detected in the DAV star G132-12

Su,

Fu,

Chen

et al. 2021

Preprint

View full text Add to dashboard Cite

show abstract

“…There are usually a large number of nonlinear combination frequencies detected in the amplitude spectra; (iv) The cooler DAV stars have longer but more unstable pulsation periods. Meanwhile, outbursts start to be detected; (v) The coolest DAV stars tend to have the longest pulsation periods with relatively low amplitudes (< 1 mmag) (Hermes et al 2017;Chen et al 2019).…”

Section: Introductionmentioning

confidence: 99%

A triplet of the only pulsation mode detected in the DAV star G132–12

Chen

et al. 2021

Res. Astron. Astrophys.

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Hydrogen atmosphere pulsating white dwarfs, also known as DAV stars, are the most abundant type of pulsating white dwarfs. High-temperature DAV stars in general exhibit a small number of pulsation modes and stable frequencies. G132–12 is one of the pulsating hydrogen atmosphere white dwarf stars which lies close to the blue edge of the instability strip. Previous researches reported that G132–12 might have only one pulsation mode with the period of 212.69 s. To study the pulsation properties of G132–12 in detail, we carried out a bi-site observation campaign in October 2019. Time series photometric data were collected during around 154 h in total. A Fourier analysis reveals three frequencies which are identified as the triplet of an l = 1 g-mode pulsation with the period of 212.499 s. The rotational period is derived as P rot = 35.0 ± 6.7 h and the inclination of the rotational axis to the line of sight is 70°. G132–12 could be an ideal target for measuring the cooling scale of this white dwarf star with only one excited pulsation mode detected.

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Spectroscopic and photometric analysis of the eclipsing binary HIP 7666 with δ Scuti pulsations

Feng

Esamdin

et al. 2021

Monthly Notices of the Royal Astronomical Society

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New multi-color photometric observations were carried out on 22 nights in three observation missions between Oct. 2015 and Feb. 2016 for eclipsing binary HIP 7666. High- and low-resolution spectroscopic observations were also carried out in the winters of 2015, 2016, and 2019, respectively. The fully phase-covered light curves and radial velocity curves are presented. All times of light minima are used to calculate the orbital period (2.3722200(4) days) and new ephemerides. The photometric solution and stellar physical parameters are derived, showing that HIP 7666 is a detached binary with the absolute parameters M1 = 1.53(3) M⊙, R1 = 2.08(2) R⊙, log L1/L⊙ = 0.99(3), log g1 = 3.98(2), Mbol1 = 2.26(8), Teff, 1 = 7100(100) K for the primary, and M2 = 1.23(3) M⊙, R2 = 1.06(2) R⊙, log L2/L⊙ = 0.13(4), log g2 = 4.47(2), Mbol2 = 4.4(1), Teff, 2 = 6029(67) K for the secondary. The age of 1.69 Gyr and 1.755 Gyr are estimated from PARSEC isochrones and MESA evolutionary tracks, respectively. In H-R diagram, the primary component has evolved to the late stages, while the secondary still locates at the early stages of the main sequence. Frequency analysis yields three frequencies of f1 = 24.631(4) cd−1, f2 = 21.193(1) cd−1, and f3 = 28.07(7) cd−1. Comparisons between models and observations suggest that the primary component is most likely a p-mode non-radial δ Scuti oscillator.

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G132-12: A one-mode ZZ Ceti star located at the blue edge of instability strip

Cited by 3 publications

References 15 publications

A triplet of the only pulsation mode detected in the DAV star G132-12

A triplet of the only pulsation mode detected in the DAV star G132-12

A triplet of the only pulsation mode detected in the DAV star G132–12

Spectroscopic and photometric analysis of the eclipsing binary HIP 7666 with δ Scuti pulsations

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