Thermal X-ray emission from massive, fast rotating, highly magnetized white dwarfs
arXiv:1611.07653 · doi:10.1093/mnras/stw3047
Abstract
There is solid observational evidence on the existence of massive, , highly magnetized white dwarfs (WDs) with surface magnetic fields up to G. We show that, if in addition to these features, the star is fast rotating, it can become a rotation-powered pulsar-like WD and emit detectable high-energy radiation. We infer the values of the structure parameters (mass, radius, moment of inertia), magnetic field, rotation period and spin-down rates of a WD pulsar death-line. We show that WDs above the death-line emit blackbody radiation in the soft X-ray band via the magnetic polar cap heating by back flowing pair-created particle bombardment and discuss as an example the X-ray emission of soft gamma-repeaters and anomalous X-ray pulsars within the WD model.
arXiv commentTo appear in MNRAS
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