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<p>Long-period radio transients (LPTs) represent a recently uncovered class of Galactic radio sources exhibiting minutes to hours periodicities and highly polarized pulses of seconds to minutes duration. Their phenomenology does not fit exactly in any other class, although it might resemble that of radio magnetars or white dwarf (WD) pulsars. Two LPTs with confirmed multi-wavelength counterparts have now been identified as WD – M dwarf binaries. Moreover, WD pulsars (also WD – M dwarf systems), such as AR Scorpii and J1912−44, are known to exhibit short-period pulsations in hour-timescale orbits. Here we investigate the longest-lived LPT known, GPM J1839−10. We use a 36-year timing baseline to infer an ~8.75-h orbital period from radio data alone, and we show that it can be modelled in the same geometric framework as has been proposed for WD pulsars. Radio emission is triggered when the magnetic axis of a rotating WD intersects the wind from its companion, which naturally predicts the peculiar pulse modulation. Applying this to the WD pulsar J1912−44 successfully reproduces the emission profile and geometry as well. Our results indicate analogous emission-site geometries in these related classes of binary system, a possibility we extend to the broader LPT and WD pulsar population.</p>

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A binary model of long-period radio transients and white dwarf pulsars

  • 期刊论文

  • 发表日期：

    2026年1月30日

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  • Csanád Horváth,
  • Nanda Rea,
  • Natasha Hurley-Walker,
  • Samuel J. McSweeney,
  • Richard A. Perley,
  • Emil Lenc

摘要

Long-period radio transients (LPTs) represent a recently uncovered class of Galactic radio sources exhibiting minutes to hours periodicities and highly polarized pulses of seconds to minutes duration. Their phenomenology does not fit exactly in any other class, although it might resemble that of radio magnetars or white dwarf (WD) pulsars. Two LPTs with confirmed multi-wavelength counterparts have now been identified as WD – M dwarf binaries. Moreover, WD pulsars (also WD – M dwarf systems), such as AR Scorpii and J1912−44, are known to exhibit short-period pulsations in hour-timescale orbits. Here we investigate the longest-lived LPT known, GPM J1839−10. We use a 36-year timing baseline to infer an ~8.75-h orbital period from radio data alone, and we show that it can be modelled in the same geometric framework as has been proposed for WD pulsars. Radio emission is triggered when the magnetic axis of a rotating WD intersects the wind from its companion, which naturally predicts the peculiar pulse modulation. Applying this to the WD pulsar J1912−44 successfully reproduces the emission profile and geometry as well. Our results indicate analogous emission-site geometries in these related classes of binary system, a possibility we extend to the broader LPT and WD pulsar population.