Illustration of supernova remnant S147 and pulsar J0538+2817 [Image: NAOC]

Pulsars — another name for fast-spinning neutron stars — originate from the imploded cores of massive dying stars through supernova explosion.

Now, more than 50 years after the discovery of pulsars and confirmation of their association with supernova explosions, the origin of the initial spin and velocity of pulsars is finally beginning to be understood.

Based on observations from the Five-hundred-meter Aperture Spherical radio Telescope (FAST), Dr. Yao Jumei, a member of a team led by Dr. Li Di from the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC), found the first evidence for three-dimensional (3D) spin-velocity alignment in pulsars.

The study was published in Nature Astronomy on May 6, and marks the beginning of in-depth pulsar research with FAST.

For decades, scientists have found observational evidence for spin-velocity alignment in young pulsars. The relationship thus revealed between pulsars’ spin axis and spatial velocity vectors, however, has largely been restricted to a 2D sky plane perpendicular to the line of sight, due to difficulty in constraining radial velocity.

Focusing on PSR J0538+2817 in the supernova remnant (SNR) S147 and using the scintillation technique, Dr. Yao obtained its radial location with respect to the SNR boundary and its radial velocity for the first time. “Then we got the 3D velocity by combining the transverse velocity measured by Very Long Baseline Interferometers,” said Dr. Yao. The polarization analysis resulted in the direction of the 3D spin axis. The best fit angle between these two vectors was found to be about 10 degrees, which is the first such measurement in 3D.

FAST is currently the world’s most sensitive single aperture radio telescope. “This represents a tour-de-force in pulsar data analysis. Through FAST observation, our team has accomplished more detections, which promise to further help reveal the origin of pulsar spin-kick,” said Dr. Li, chief scientist of FAST and one of the corresponding authors of the study.

This work was supported by the International Partnership Program of the Chinese Academy of Sciences (CAS).

Major collaborators include those from the Xinjiang Astronomical Observatory of CAS, the Australia Telescope National Facility, the University of California, the Max Planck Institute for Radio Astronomy, and Oberlin College. 

Source: National Astronomical Observatories,

Chinese Academy of Sciences