Astrophys. J., 866, 160-160 (2018/October-3)
Pulse morphology of the Galactic Center magnetar PSR J1745-2900.
PEARLMAN A.B., MAJID W.A., PRINCE T.A., KOCZ J. and HORIUCHI S.
Abstract (from CDS):
We present results from observations of the Galactic Center magnetar, PSR J1745-2900, at 2.3 and 8.4 GHz with the NASA Deep Space Network 70 m antenna, DSS-43. We study the magnetar's radio profile shape, flux density, radio spectrum, and single pulse behavior over a ∼1 year period between MJDs 57233 and 57621. In particular, the magnetar exhibits a significantly negative average spectral index of <α>=-1.86±0.02 when the 8.4 GHz profile is single-peaked, which flattens considerably when the profile is double-peaked. We have carried out an analysis of single pulses at 8.4 GHz on MJD 57479 and find that giant pulses and pulses with multiple emission components are emitted during a significant number of rotations. The resulting single pulse flux density distribution is incompatible with a log-normal distribution. The typical pulse width of the components is ∼1.8 ms, and the prevailing delay time between successive components is ∼7.7 ms. Many of the single pulse emission components show significant frequency structure over bandwidths of ∼100 MHz, which we believe is the first observation of such behavior from a radio magnetar. We report a characteristic single pulse broadening timescale of <τd>=6.9±0.2ms at 8.4 GHz. We find that the pulse broadening is highly variable between emission components and cannot be explained by a thin scattering screen at distances >= 1 kpc. We discuss possible intrinsic and extrinsic mechanisms for the magnetar's emission and compare our results to other magnetars, high magnetic field pulsars, and fast radio bursts.
© 2018. The American Astronomical Society. All rights reserved.
Galaxy: center - pulsars: individual: PSR J1745-2900 - scattering - stars: magnetars - stars: neutron
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