Aug 27, 2019
Astrophysicists have discovered that the pulsar wind nebula (PWN) surrounding the famous pulsar B0540-69 brightened gradually after the pulsar experienced a sudden spin-down rate transition (SRT). This discovery, made by a group of astrophysicists led by GE Mingyu and LU Fangjun at the Institute of High Energy Physics (IHEP) of the Chinese Academy of Sciences, provides important clues to the spin-down mechanism and the magnetic field structure of the pulsar, as well as the physical properties of the PWN. The results were published in Nature Astronomy.
Pulsars are highly magnetized neutron stars born from supernova explosions of massive stars. They typically have radii about 10 km and surface magnetic field strengths around 1 trillion Gauss. According to classic pulsar theory, an isolated pulsar loses energy through magnetic dipole radiation and thus slows down. However, more and more theorists believe that the main way an isolated pulsar loses its rotational energy is through a relativistic wind consisting of electrons, positrons and possibly magnetic field. If the wind is strong enough, it will eventually form a detectable PWN through interaction with the surrounding materials. The famous Crab nebula is such a PWN, with a size of several light-years, i.e., about a hundred thousand times the distance from Earth to the Sun.
PSR B0540-69 is located in the Large Magellanic Cloud galaxy, a satellite galaxy about 160,000 light-years from our Milky Way. In December 2011, the spin-down rate of this pulsar suddenly increased by 36% and has remained almost constant since then, which means the energy release rate of the pulsar has also increased by 36%. Unlike other pulsars with similar spin-down rate transitions, which are accompanied by pulse profile and/or flux changes and are attributed to changes in the magnetospheres, no variation in either the pulse profile or flux has been detected from PSR B0540-69, making the cause of its SRT a mystery.
GE stated, “Using data obtained by a few X-ray astronomical satellites, we find that the X-ray PWN around PSR B0540-69 brightened gradually up to 32±8% over the prior flux during the period of about 400 days since the SRT (Fig. 2). We show that the SRT most likely resulted from a sudden enhancement of the magnetic field in the pulsar magnetic pole region, which does not significantly affect the pulsed X-ray emission but increases pulsar wind power and hence PWN X-ray emission.” This is the first time that PWN brightening has been observationally connected with the pulsar spin-down rate transition, implying that the pulsar wind is the main factor slowing down the pulsar spin. “The 400-day time scale of the flux increase corresponds to a magnetic field strength of about 0.8 milli-Gauss in the PWN. This is also the first direct measurement of the magnetic field and is consistent with the value estimated before under some assumptions,” LU added.
The other investigators on this project include YAN Linli of Anhui Jianzhu University, WENG Shanshan of Nanjing Normal University, ZHANG Shuangnan ,WANG Lingjun and ZHANG Wei of the Institute of High Energy Physics, Q. Daniel Wang of the University of Massachusetts, and LI Zijian from the Hebei University of Engineering.
Fig. 1: An illustration of the pulsar and pulsar wind nebula (PWN) system (not to scale). The relativistic wind from the central pulsar is terminated by a shock at a radius of about one light-year and starts to radiate. The typical size of a PWN is a few light-years. The image of the Large Magellanic Cloud galaxy shown in the lower left was taken by YE Ziyi. (Image by IHEP)
Fig. 2: The evolution of the X-ray fluxes of PSR B0540-69 and its pulsar wind nebula (PWN) measured by various instruments. (a) Evolution of the overall X-ray flux of the pulsar+PWN, which increased significantly after the spin-down rate transition (SRT). (b) The near-constant flux of the pulsed X-ray emission. (c) The photon indices of PSR+PWN obtained with different instruments. The dotted vertical line denotes the SRT epoch. (Image by IHEP/Nature Astronomy)
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