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Related Experiment Video

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Uncoupling Coriolis Force and Rotating Buoyancy Effects on Full-Field Heat Transfer Properties of a Rotating Channel
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CONSTRAINING RELATIVISTIC BOW SHOCK PROPERTIES IN ROTATION-POWERED MILLISECOND PULSAR BINARIES.

Zorawar Wadiasingh1, Alice K Harding2, Christo Venter1

  • 1Centre for Space Research, North-West University, Potchefstroom, South Africa.

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Summary

This study reveals two distinct modes in black widow and redback millisecond pulsar binaries, explaining their radio and X-ray emissions through intrabinary shock orientation and Doppler boosting.

Keywords:
X-rays: binariesbinaries: eclipsingpulsars: individual (J1023+0038, B1957+20)radiation mechanisms: non-thermal

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Area of Science:

  • Astronomy and Astrophysics
  • High-Energy Astrophysics
  • Compact Objects

Background:

  • Multiwavelength observations of Fermi Gamma-ray Space Telescope sources have identified numerous galactic-field millisecond pulsar binaries, including black widow and redback types.
  • Understanding the radio to X-ray emission from these rotation-powered systems requires a consistent physical framework.

Purpose of the Study:

  • To interpret the radio and X-ray phenomenology of black widow and redback millisecond pulsar binaries.
  • To propose a consistent framework based on intrabinary shock orientation and Doppler boosting.
  • To constrain binary inclination and shock geometry using radio eclipse data.

Main Methods:

  • Developing a geometric model for radio eclipses to constrain shock geometry (stand-off distance R0 and binary inclination).
  • Constructing synthetic X-ray synchrotron orbital light curves based on the geometric model.
  • Applying constraints from radio eclipses to archetypal systems like B1957+20 and J1023+0038.
  • Comparing synthetic X-ray light curves with observed data.

Main Results:

  • Advocating two distinct modes of intrabinary shock orientation, distinguished by phase-centered, double-peaked X-ray modulation due to Doppler boosting.
  • For B1957+20, radio eclipses constrain the shock stand-off R0 to ~0.15-0.3 binary separations, consistent with observed X-ray light curves.
  • For J1023+0038, radio eclipses suggest R0 ≲ 0.4, while X-ray light curves imply 0.1 ≲ R0 ≲ 0.3 (from the pulsar).
  • Occultation by the companion is a minor influence; significant Doppler factors are needed for double peaks.

Conclusions:

  • The proposed framework, incorporating shock geometry and Doppler boosting, successfully explains the observed radio and X-ray behavior of these pulsar binaries.
  • Parameter space degeneracies highlight the need for further model development, including transport effects.
  • Future X-ray phase-resolved spectroscopy is crucial for probing pulsar wind physics and relativistic shock acceleration, potentially revealing energy-dependent light curve variations.