Issue |
A&A
Volume 437, Number 3, July III 2005
|
|
---|---|---|
Page(s) | 997 - 1005 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20052633 | |
Published online | 30 June 2005 |
Three XMM-Newton observations of the anomalous X-ray pulsar 1E 1048.1–5937: Long term variations in spectrum and pulsed fraction
1
Istituto di Astrofisica Spaziale e Fisica Cosmica, Sezione di Milano “G.Occhialini”, via Bassini 15, 20133 Milano, Italy e-mail: tiengo@mi.iasf.cnr.it
2
Università degli Studi di Milano, Dipartimento di Fisica, via Celoria 16, 20133 Milano, Italy
3
Università di Padova, Dipartimento di Fisica, via Marzolo 8, 35131 Padova, Italy
4
Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking Surrey, RH5 6NT, UK
5
INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio Catone, Roma, Italy
6
SRON – National Institute for Space Research, Sorbonnelaan, 2, 3584 CA, Utrecht, The Netherlands
Received:
3
January
2005
Accepted:
12
March
2005
We report the results of a recent (July 2004) XMM-Newton Target of Opportunity observation of the Anomalous X-ray Pulsar
1E 1048.1–5937 together with a detailed re-analysis of previous observations
carried out in 2000 and 2003. In July 2004 the source had a 2–10 keV
flux of 6.2 10-12 erg cm-2 s-1 and a pulsed
fraction PF = 0.68. Comparison of the three data sets shows the
presence of an anti-correlation between flux and pulsed fraction,
implying that previous estimates of the source energetics based on
the assumption of a large and constant pulsed fraction might be
significantly underestimated. The source spectrum is well described
by a power law plus blackbody model (kT ~ 0.63 keV, photon index
Γ ~ 2.7–3.5) or, alternatively, by the sum of two blackbodies of which the hotter is Comptonized by relativistic electrons. In this case the temperatures are
~ 0.2–0.3 keV and
~ 0.4–0.5 keV and the emitting area of the cooler
component is consistent with the whole neutron star surface. The
long-term luminosity variation of a factor
2 is accompanied by
relatively small variations in the spectral shape. Phase-resolved
spectroscopy indicates a harder spectrum together with the pulse
maximum. No spectral features have been detected with 4σ
limits on the equivalent width in the range ~10–220 eV,
depending on line energy and width.
Key words: stars: individual: 1E 1048.1–5937 / X-rays: stars
© ESO, 2005
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