XMM-NEWTON OBSERVATIONS OF YOUNG AND ENERGETIC PULSAR J2022+3842

We report on XMM-Newton EPIC observations of the young pulsar J2022+3842, with a characteristic age of 8.9 kyr. We detected X-ray pulsations and found the pulsation period P approximately 48.6 ms, and its derivative P approximately 8.6 x 10 super(-14), which is two times larger than previously repor...

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Bibliographic Details
Published in:The Astrophysical journal 2014-08, Vol.790 (2), p.1-8, Article 103
Main Authors: ARUMUGASAMY, P, Pavlov, G G, Kargaltsev, O
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
DENSITY
Derivatives
EFFICIENCY
EMISSION
MAGNETIC FIELDS
NEBULAE
NEUTRONS
PHOTONS
PULSARS
Pulsation
PULSATIONS
ROTATION
SPECTRA
SPIN
STARS
STELLAR WINDS
X RADIATION
X-rays
XMM (spacecraft)
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Summary:We report on XMM-Newton EPIC observations of the young pulsar J2022+3842, with a characteristic age of 8.9 kyr. We detected X-ray pulsations and found the pulsation period P approximately 48.6 ms, and its derivative P approximately 8.6 x 10 super(-14), which is two times larger than previously reported values. The pulsar exhibits two very narrow (FWHM ~ 1.2 ms) X-ray pulses each rotation, separated by approximately 0.48 of the period, with a pulsed fraction of approximately 0.8. Using the correct values of P and P, we calculate the pulsar's spin-down power E = 3.0 x 10 super(37) erg s super(-1) and magnetic field B = 2.1 x 10 super(12) G. The pulsar spectrum is well modeled with a hard power-law (PL) model (photon index [Gamma] = 0.9 + or - 0.1, hydrogen column density n sub(H) = (2.3 + or - 0.3) x 10 super(22) cm super(-2)). We detect a weak off-pulse emission, which can be modeled with a softer PL ([Gamma] approximately 1.7 + or - 0.7), that is poorly constrained because of contamination in the EPIC-pn timing mode data. The pulsar's X-ray efficiency in the 0.5-8 keV energy band, [eta] sub(PSR) = L sub(PSR)/E = 2 x 10 super(-4)(D/10kpc) super(2), is similar to those of other pulsars. The XMM-Newton observation did not detect extended emission around the pulsar. Our re-analysis of Chandra X-ray Observatory archival data shows a hard, [Gamma] approximately 0.9 + or - 0.5, spectrum and a low efficiency, [eta] sub(PWN) ~ 2 x 10 super(-5)(D/10kpc) super(2), for the compact pulsar wind nebula, unresolved in the XMM-Newton images.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/790/2/103