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Period versus magnetic field diagram of various pulsars. Dots are radio pulsars, triangles are SNR pulsars, circles are millisecond pulsars, and diamonds are magnetars. The dashed-dotted and solid lines are spin-up and death lines, respectively.
Source publication
Supernova 1987A is a core collapse supernova in the Large Magellanic Cloud, inside which the product is most likely a neutron star. Despite the most sensitive available detection instruments from radio to γ-ray wavebands being exploited in the pass thirty years, there have not yet been any pulse signals detected. By considering the density of the m...
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... the plasma oscillation frequency may reach or pass the radio radiation frequency, resulting in that the radio signal from the pulsar cannot be detected. We suggest that there may be a crablike pulsar formed in SN 1987A with the period of í µí± i ∼ 20 ms and magnetic field of í µí°µ i ∼ 5 × 10 12 G (see its period-magnetic field position in Fig. 1). The radio emission beam of the pulsar should sweep across the earth, while this radio signal cannot be detected due to the high particle density in the pulsar gaps, which cut off the propagation of the pulsar radio waves. We predict that with the further expansion of the SNR and the spin down of the pulsar, its radio pulse signal ...
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Citations
The mass of the stellar precursor of supernova (SN) 1987A and the burst of neutrinos observed at the moment of the explosion are consistent with the core-collapse formation of a neutron star. However, no compelling evidence for the presence in SN 1987A of a compact object of any kind has been found yet in any band of the electromagnetic spectrum, prompting questions on whether the neutron star survived and, if it did, on its properties. Starting from the analysis of recent Chandra observations, here we appraise the current observational situation. We derived limits on the X-ray luminosity of a compact object with a nonthermal, Crab-pulsar-like spectrum of the order of $\approx$$(1$-$5)\times10^{35}$ erg s$^{-1}$, corresponding to limits on the rotational energy loss of a possible X-ray pulsar in SN 1987A of $\approx$$(0.5$-$1.5)\times10^{38}$ erg s$^{-1}$. However, a much brighter X-ray source cannot be excluded if, as is likely, it is enshrouded in a cloud of absorbing matter with metallicity similar to that expected in the outer layers of a massive star towards the end of its life. We found that other limits obtained from various arguments and observations in other energy ranges either are unbinding or allow a similar maximum luminosity of the order of $\approx$$10^{35}$ erg s$^{-1}$. We conclude that while a pulsar alike the one in the Crab Nebula in both luminosity and spectrum is hardly compatible with the observations, there is ample space for an `ordinary' X-ray-emitting young neutron star, born with normal initial spin period, temperature and magnetic field, to be hiding inside the evolving remnant of SN 1987A.
The aspect of formation and evolution of the recycled pulsar (PSR J0737-3039 A/B) is investigated, taking into account the contributions of accretion rate, radius and spin-evolution diagram (B - P diagram) in double pulsar system. Accepting the spin-down age as a rough estimate (or often an upper limit) of the true age of the neutron star, we impose also the restrictions on the radius of this system. We calculate the radius of
the recycled pulsar PSR J0737-3039A ranges approximately from 8.14 to 25.74 km, and the composition of its neutron star nuclear matters is discussed in the mass-radius diagram.
