The white dwarf binary V709 Cas shows refined periods (5.3329 h, 312.7478 s, 317.9267 s) and time-variable accretion geometry consistent with a two-pole disc-overflow accretor.
Measuring the masses of Intermediate Polars with NuSTAR: V709 Cas, NY Lup and V1223 Sgr
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abstract
The X-ray spectra of intermediate polars can be modelled to give a direct measurement of white dwarf mass. Here we fit accretion column models to NuSTAR spectra of three intermediate polars; V709 Cas, NY Lup and V1223 Sgr in order to determine their masses. From fits to 3-78 keV spectra, we find masses of $M_{\rm WD}=0.88^{+0.05}_{-0.04}M_{\odot}$, $1.16^{+0.04}_{-0.02}M_{\odot}$ and $0.75\pm0.02M_{\odot}$ for V709 Cas, NY Lup and V1223 Sgr, respectively. Our measurements are generally in agreement with those determined by previous surveys of intermediate polars, but with typically a factor $\sim2$ smaller uncertainties. This work paves the way for an approved NuSTAR Legacy Survey of white dwarf masses in intermediate polars.
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Long-term Optical Photometry of V709 Cas Using TESS : Refined Periods and Accretion Geometry
The white dwarf binary V709 Cas shows refined periods (5.3329 h, 312.7478 s, 317.9267 s) and time-variable accretion geometry consistent with a two-pole disc-overflow accretor.