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Magnetar
About: Magnetar is a research topic. Over the lifetime, 2905 publications have been published within this topic receiving 106806 citations.
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TL;DR: In this article, the authors deduced a general formula for pressure of degenerate and relativistic electrons, P-e, which is suitable for superhigh magnetic fields, and discussed the quantization of Landau levels of electrons, and considered the quantum electrodynamic (QED) effects on the equations of states (EOSs) for different matter systems.
Abstract: Based on our previous work, we deduce a general formula for pressure of degenerate and relativistic electrons, P-e, which is suitable for superhigh magnetic fields, discuss the quantization of Landau levels of electrons, and consider the quantum electrodynamic (QED) effects on the equations of states (EOSs) for different matter systems. The main conclusions are as follows: P-e is related to the magnetic field B, matter density rho, and electron fraction Y-e; the stronger the magnetic field, the higher the electron pressure becomes; the high electron pressure could be caused by high Fermi energy of electrons in a superhigh magnetic field; compared with a common radio pulsar, a magnetar could be a more compact oblate spheroid-like deformed neutron star (NS) due to the anisotropic total pressure; and an increase in the maximum mass of a magnetar is expected because of the positive contribution of the magnetic field energy to the EOS of the star.
35 citations
TL;DR: In this paper, it was shown that after many radio pulsars evolve into magnetars, i.e., strongly magnetized and slowly rotating neutron stars, after many glitches, and that the surface magnetic field is increased after each glitch.
Abstract: Glitches are common phenomena in pulsars. After each glitch, there is often a permanent increase in the pulsar's spin-down rate. Therefore, a pulsar's present spin-down rate may be much higher than its initial value and the characteristic age of a pulsar based on its present spin-down rate and period may be shorter than its true age. At the same time, the permanent increase of its spin-down rate implies that the pulsar's surface magnetic field is increased after each glitch. Consequently, after many glitches some radio pulsars may evolve into magnetars, i.e., strongly magnetized and slowly rotating neutron stars.
35 citations
TL;DR: In this paper, the authors presented new X-ray timing and spectral results on the 8.0-second Xray pulsar CXOUJ010043.1-721134 from a series of observations using the Chandra X-Ray Observatory.
Abstract: We present new X-ray timing and spectral results on the 8.0-second X-ray pulsar CXOU J010043.1-721134 from a series of observations using the Chandra X-ray Observatory. We find a spin period in 2004 January of 8.020392pm0.000009 seconds. Comparison of this to 2001 Chandra observations implies a period derivative dot{P} = (1.88 pm 0.08) times 10^{-11} s s^{-1}, leading to an inferred dipole surface magnetic field of 3.9 times 10^{14} G. The spectrum is well fit to an absorbed blackbody of temperature kT = 0.38pm0.02 keV with a power law tail of photon index Gamma = 2.0pm0.6. We find that the source has an unabsorbed X-ray flux (0.5-10 keV) of 4(+2-1) times 10^{-13} erg cm^{-2} s^{-1} and a corresponding X-ray luminosity of ~2 times 10^{35} erg s^{-1} for a distance of 60 kpc. These properties support classification of CXOU J010043.1-721134 as the seventh confirmed anomalous X-ray pulsar,the eleventh confirmed magnetar, and the first magnetar to be identified in the Small Magellanic Cloud.
35 citations
TL;DR: In this paper, the early peak and late-time slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P0 -sim 20 ms, while the intermediate-time (50 \lesssim t -lesssim 300 days) linear decline is caused by radioactive decay of 56Ni.
Abstract: Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe Some SNe Ic-BL are associated with long-duration (\gtrsim 2 s) gamma-ray bursts (GRBs) Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far Here we report the finding that the early peak (t \lesssim 50 days) and late-time (t \gtrsim 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P0 \sim 20 ms, while the intermediate-time (50 \lesssim t \lesssim 300 days) linear decline is caused by radioactive decay of 56Ni The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars
35 citations
35 citations