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The 2015 outburst of the accreting millisecond pulsar IGR J17511-3057 as seen by INTEGRAL, Swift and XMM-Newton | A. Papitto
; E. Bozzo
; C. Sanchez-Fernandez
; P. Romano
; D. F. Torres
; C. Ferrigno
; J. J. E. Kajava
; E. Kuulkers
; | Date: |
1 Sep 2016 | Abstract: | We report on INTEGRAL, Swift and XMM-Newton observations of IGR J17511-3057
performed during the outburst that occurred between March 23 and April 25,
2015. The source reached a peak flux of 0.7(2)E-9 erg/cm$^2$/s and decayed to
quiescence in approximately a month. The X-ray spectrum was dominated by a
power-law with photon index between 1.6 and 1.8, which we interpreted as
thermal Comptonization in an electron cloud with temperature > 20 keV . A broad
({sigma} ~ 1 keV) emission line was detected at an energy (E =
6.9$^{+0.2}_{-0.3}$ keV) compatible with the K{alpha} transition of ionized
Fe, suggesting an origin in the inner regions of the accretion disk. The
outburst flux and spectral properties shown during this outburst were
remarkably similar to those observed during the previous accretion event
detected from the source in 2009. Coherent pulsations at the pulsar spin period
were detected in the XMM-Newton and INTEGRAL data, at a frequency compatible
with the value observed in 2009. Assuming that the source spun up during the
2015 outburst at the same rate observed during the previous outburst, we derive
a conservative upper limit on the spin down rate during quiescence of 3.5E-15
Hz/s. Interpreting this value in terms of electromagnetic spin down yields an
upper limit of 3.6E26 G/cm$^3$ to the pulsar magnetic dipole (assuming a
magnetic inclination angle of 30{deg}). We also report on the detection of
five type-I X-ray bursts (three in the XMM-Newton data, two in the INTEGRAL
data), none of which indicated photospheric radius expansion. | Source: | arXiv, 1609.0187 | Services: | Forum | Review | PDF | Favorites |
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