A triplet of the only pulsation mode detected in the DAV star G132-12
| Autor: | Wen-Chao Su, Jiangtao Wang, Yang Pan, Shi-Jie Zhao, Carmen Ayala-Loera, Jian-Xing Chen, Jian-Ning Fu, L. Fox-Machado |
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| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Rotation period
Physics Line-of-sight Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences White dwarf Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Type (model theory) symbols.namesake Stars Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Fourier analysis Excited state symbols Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Instability strip Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics |
| Popis: | 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. |
| Databáze: | OpenAIRE |
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