Astrophys. J., 676, 1178-1183 (2008/April-1)
Outburst of the 2 s anomalous X-ray pulsar 1E 1547.0-5408.
HALPERN J.P., GOTTHELF E.V., REYNOLDS J., RANSOM S.M. and CAMILO F.
Abstract (from CDS):
Following our discovery of radio pulsations from the newly recognized anomalous X-ray pulsar (AXP) 1E 1547.0-5408, we initiated X-ray monitoring with the Swift X-ray telescope and obtained a single target-of-opportunity observation with the Newton X-ray Multi-Mirror Mission (XMM-Newton). In comparison with its historic minimum flux of 3x10–13 ergs/cm2/s, the source was found to be in a record high state, fX(1-8 keV)=5x10–12 ergs/cm2/s, or LX=1.7x1035(d/9 kpc)2 ergs/s, and declining by 25% in 1 month. Extrapolating the decay, we bound the total energy in this outburst to 1042 ergs<E<1043 ergs. The spectra (fitted with a Comptonized blackbody) show that an increase in the temperature and area of a hot region, to 0.5 keV and ∼16% of the surface area of the neutron star, respectively, are primarily responsible for its increase in luminosity. The energy, spectrum, and timescale of decay are consistent with a deep crustal heating event, similar to an interpretation of the X-ray turn-on of the transient AXP XTE J1810-197. Simultaneous with the 4.6 hr XMM-Newton observation, we observed at 6.4 GHz with the Parkes telescope, measuring the phase relationship of the radio and X-ray pulse. The X-ray pulsed fraction of 1E 1547.0-5408 is only ∼7%, while its radio pulse is relatively broad for such a slow pulsar, which may indicate a nearly aligned rotator. As also inferred from the transient behavior of XTE J1810-197, the only other AXP known to emit in the radio, the magnetic field rearrangement responsible for this X-ray outburst of 1E 1547.0-5408 is probably the cause of its radio turn-on.
ISM: individual (G327.24-0.13) - pulsars: individual (1E 1547.0-5408) - pulsars: individual (PSR J1550-5418) - Stars: Pulsars: Individual: Alphanumeric: XTE J1810-197 - Stars: Neutron
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