Asteroseismology of the ultramassive ZZ Ceti star WD 0246+326

Abstract

The internal structures of pulsating white dwarfs can be explored only with asteroseismology. Time series photometric observations were made for the pulsating DA white dwarf (ZZ Ceti star) WD~0246+326 during 9 nights in 2014 with a bi-site observation campaign. Eleven frequencies were detected including 1 triplet, 2 doublets, and 4 single modes, which are identified as either $l=1$ or $l=2$ modes with the complementarity of frequencies present in the literature. From the multiplets, the rotation period of \astrobj{WD~0246+326} is derived as $3.78\pm 0.11$ days. The average period spacing of the l=1 modes $\Delta P=29.3\pm 0.2s$, implies that \astrobj{WD~0246+326} may be a massive ZZ Ceti star concerning the $\Delta P-M_{\ast }$ relationship for the DAVs. Preliminary analysis derives the stellar parameters of $M_{\ast }=0.98\pm 0.01$~${\mathrm{M}}_{\odot }$ and $T_{\mathrm{eff}}=11700\pm 100$~K by fitting the theoretical frequencies of the eigen modes to the observed ones.

arXiv comment17 pages, 5 figures

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Cited by in corpus (2)

• Photometric White Dwarf Rotation
• Seismic test of the mass-radius relationship of hydrogen-atmospheric white dwarf stars