From the June 2018 issue

What produces the radio waves from a pulsar, and why do they form beams?

Fr. Taylor Reynolds Rome, Italy
By | Published: June 27, 2018
Pulsars emit cones of bright radio emission from their magnetic poles as they rotate rapidly. Because these stellar remnants can spin so quickly, their outermost magnetic field lines cannot move fast enough and do not reconnect.
ESA/ATG Medialab
Pulsars are rapidly rotating, highly magnetic compact stars. The rotating magnetic field of a pulsar acts as a generator, accelerating energetic charged particles that then stream along the field lines. A pulsar’s magnetic field is like that of a typical bar magnet, emanating from one pole and returning to the other, with an important exception: To keep up with the rotation of the star, magnetic field lines that extend to a sufficiently large distance would need to move at the speed of light, which is impossible. The limit at which the field lines can no longer rotate fast enough is called the pulsar’s “light cylinder.” Field lines that extend beyond this limit remain “open” rather than returning to the star, as illustrated in the image to the upper right.

Particles accelerated by the pulsar stream along these open field lines and produce radiation that stimulates a cascade of additional particles, which radiate as well. Because the particles are moving relativistically (close to the speed of light), their radiation is beamed in the direction of their motion. The bulk of a pulsar’s radio emission is produced at some particular height above the magnetic pole and confined to a narrow beam defined by the field line orientation at that height (which points largely upward). As the star rotates, if this beam crosses the path of the observer, it is seen as a radio pulse. The cross-section of the beam can be complicated, meaning that the pulse shape can depend on which part of the beam crosses the observer’s line of sight.

The exact details of where in the open-field region the particles create this radio emission is still under investigation. While many models suggest it is formed close to the poles, recent studies indicate that the emission may occur closer to the edges of the light cylinder. Further studies are ongoing to better understand the details of the process, particularly at higher energies.

Pat Slane 
Senior Astrophysicist, 
Smithsonian Astrophysical Observatory and Lecturer, 
Department of Astronomy, Harvard University, 
Cambridge, Massachusetts