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• W3150047417 endingPage "101604" @default.
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• W3150047417 abstract "We present a study of the LAMOST spectra and public photometric data for four AM CVn binaries with orbital periods ranging from 17 to 41 min. The prototypical star AM CVn displays short-term brightness fluctuations, which most likely arise from its superhump modulation. The superhump period of PTF1J0719+4858 is identified to be 1659.85(13) s, slightly longer than its orbital period. We find a short-lived dip in the phase-folded light curve centered on a phase of ∼ 0.5 during the 2008 March outburst of YZ LMi. This dip can be interpreted as the obscuration of the accretion flow or inner disc. The superhump period of V493 Gem has a positive period derivative during the middle stage, which can be seen in most SU UMa-type cataclysmic variables (CVs). By applying the growing superhump method we determined its mass ratio to be q=0.0315(24). The quiescent spectra of both PTF1J0719+4858 and V493 Gem show clear metal lines and reveal a possible white dwarf donor. We also discussed the theoretical values of the donor mass and the mass transfer rate of these two systems." @default.
• W3150047417 created "2021-04-13" @default.
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• W3150047417 date "2021-08-01" @default.
• W3150047417 modified "2023-09-24" @default.
• W3150047417 title "LAMOST spectra and photometric behaviour of four AM CVn binaries" @default.
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• W3150047417 doi "https://doi.org/10.1016/j.newast.2021.101604" @default.
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