2014/10/31 by K. Y. Ekşi, K. Yavuz Ekşı, İ. C. Andaç +8 · 2 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Compact star #Eddington luminosity #Galaxy #High-pressure geophysics and materials #Luminosity #Magnetar #Magnetic field #Neutron star #Physics #Pulsar #Pulsars and Gravitational Waves Research #RADIUS #X-ray binary #astro-ph.HE
paper · pdf · doi:10.1093/mnrasl/slu199
published as MNRAS 448, L40-L42 (2015) · MNRAS Letters accepted, 4 pages, 1 figure
arxiv created 2014/12/12 · openalex publication_date 2015/01/10 · arxiv updated 2015/01/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract The recent detection of pulsations from the ultraluminous X-ray source (ULX) NuSTAR J095551+6940.8 in M82 by Bachetti et al. indicates that the object is an accreting neutron star in a high-mass X-ray binary (HMXB) system. The super-Eddington luminosity of the object implies that the magnetic field is sufficiently strong to suppress the scattering cross-section unless its beam is viewed at a favourable angle. We show that the torque equilibrium condition for the pulsar indicates that the dipole magnetic field of the neutron star is 6.7 × 1013 G, two orders of magnitude higher than that estimated by Bachetti et al., and further point to the possibility that even stronger magnetic fields could well be in the higher multipoles. This supports the recent view that magnetars descent from HMXBs if the magnetic field decays an order of magnitude during the process of transition.