Compact binary millisecond pulsars, also known as “spiders”, host the most massive neutron stars ever observed to date. Expanding the currently known spider population holds the key to determining the maximum neutron star mass, which has crucial implications for astrophysics, nuclear physics and gravitational wave astronomy. Searching for the variable optical emission of their companions…
DetailsCompact binary millisecond pulsar systems can host some of the most massive neutron stars. These rapidly rotating neutron stars are orbited by a much less massive companion star, which can be heated by high energy particles from the pulsar wind, causing it to become irradiated. This, along with additional sources of heating from the surface…
DetailsPulsar radio emission, associated with rapidly spinning neutron stars, enables the estimation of their distances in the Galaxy through dispersion measure (DM). The DM quantifies the dispersive delay experienced by electromagnetic radiation as it traverses ionized matter, such as the interstellar medium (ISM). By measuring this delay across a range of frequencies, astronomers can obtain…
DetailsCompact binary millisecond pulsars are captivating celestial objects comprised of fast-spinning neutron stars orbiting closely with lighter companion stars. Neutron stars are ultra-dense remnants of massive stars resulting from supernova explosions at the culmination of their lifecycles. These binary pulsars exhibit distinct behaviors due to intense gravitational interactions between the stars. Pulsars emit particle “winds”…
DetailsWe present the first multi-band optical light curves of PSR J1622-0315, among the most compact known redback binary millisecond pulsars, with an orbital period Porb=3.9 h. We find a flux modulation with two maxima per orbital cycle and a peak-to-peak amplitude of about 0.3 mag, which we attribute to the ellipsoidal shape of the tidally distorted companion star. The optical colours imply a late-F to early-G spectral type companion and do not show any detectable temperature changes along the orbit. This suggests that the irradiation of the star’s inner face by the pulsar wind is unexpectedly missing despite its short orbital period.
DetailsArticle published on Gemini/Norwegian SciTech News 22nd December 2021
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