Ultra-wideband radio observations unravel polarization mystery of millisecond pulsar

In our galaxy of the Milky Way, in the direction of the Vulpecula constellation, a cosmic “headlight” called PSR B1937 + 21 turns at an amazing rate of 642 revolutions per second. He emits electromagnetic impulses that compete with the accuracy of atomic clocks.

For the first time, a Chinese research team captured the complete polarization model of the PSR B1937 + 21 Pulse and main interpretation of the frequency. Discovery, reported in The astrophysical newspaperprovides crucial evidence of the radiation mechanisms operating under extreme physical conditions.

Using the 64-meter Murriyang 64-meter radio telescope in Australia equipped with an ultra-width receiver, PH.D. The Wang Zhen student of the Xinjiang (Xao) Astronomical Observatory of the Chinese Academy of Sciences (Case), under the direction of his supervisors, Professor Yuan Jianping and Professor Wen Zhigang, led the three years supported observations.

The researchers unveiled the radiation secrets of the PSR B1937 + 21: the degree of linear polarization of the main impulse decreases as the frequency increases, while the interpulse shows the opposite trend; The degree of circular polarization of the two emission regions is strengthening with an increasing frequency; And the main intensity ratio to interpulse follows a power spectrum with an index of 0.52 ± 0.02.

Discovered in 1982 as one of the first pulsars in milliseconds, the PSR B1937 + 21 has an ultra-short rotation period of 1.558 millisecond. Its magnetic field strength is simply a thousandth of nineteenth-milling of ordinary pulsars, suggesting a possible spin-up via the accretion of a complementary star.

The researchers used an ultra-liner reception system covering 704-4032 MHz, increasing the Signal / Noise 20 ratio by integrating multi-year data. In addition, flow density measures, analysis of dispersion measurement (DM) and Faraday rotation measures were used to deduce the properties of the intermediate interstellar environment.

The results have confirmed that the height of emissions decreases as the frequency increases, which manifests itself as a narrowed pulse width. The results also suggest that the main impulse and the interpulse probably come from different regions of the magnetosphere. These results provide observational support for the “relativistic radiation model”.

These results will advance research on the magnetospheric physics of the neutronic star and plasma radiation mechanisms, while offering more precise synchronization references for the detection of gravitational waves.