Transitional millisecond pulsars (tMSPs) have emerged as a new class since the discovery
of the first such system over a decade ago. These systems switch between
a rotation-powered state and an accretion-powered state, and
provide clues to understanding the physical processes that spin-up neutron stars to
millisecond periods.
Recently, astronomers analysing simultaneous data obtained using the William Herschel Telescope (WHT) and the Gran
Telescopio Canarias (GTC), have been able to model the observed light curves and conclude that
the accretion of clumpy material through the magnetic barrier of the neutron star
can produce the observed near-IR/optical variability and correlations.
In the rotation-powered state, these systems have high
radio luminosities and the neutron star is detectable through its radio pulsations
as a millisecond pulsar (MSP). In the accretion-powered state, no pulsations have been detected at
radio wavelengths, and the systems is much brighter at optical and X-ray
wavelengths due to the presence of an accretion disc.
PSR J1023+0038 was the first member of the tMSPS to be discovered. Although it was originally
classified as a cataclysmic variable (a binary star system with a white dwarf primary), in 2007
the system was detected as a radio pulsar with a spin period of 1.69 ms, and hence it
was reclassified as an MSP. PSR J1023+0038 transitioned from a rotation-powered to an
accretion-powered state in 2013 June and has remained in this state so far.
In 2017 astronomers determined the timing properties of PSR J1023+0038 using data taken
simultaneously with ACAM on the WHT and CIRCE on the Gran
Telescopio Canarias (GTC), when the system was in the accretion-powered state. The
light curves, covering 14,000 s, showed rapid transitions, similar to the X-ray mode-switching
behaviour observed previously.