The Anatomy Of A Magnetar: XMM Monitoring Of Transient AXP XTE J1810-197

Details The Anatomy Of A Magnetar: XMM Monitoring Of Transient AXP XTE J1810-197 The Anatomy Of A Magnetar: XMM Monitoring Of Transient AXP XTE J1810-197

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0764g&link_type=abstract

American Astronomical Society, HEAD meeting #9, #7.64; Bulletin of the American Astronomical Society, Vol. 38, p.360

Astronomy and Astrophysics

Astronomy

Scientific paper

The transient anomalous X-ray pulsar (TAXP) XTE J1810-197 is a unique
object whose remarkable properties offer great promise for deciphering
the emission mechanism(s) of magnetars. This 5.54s pulsar was
discovered in early 2003 during an outburst that has, as of 2006, faded
near to quiescence, based on historic data. TAXP XTE J1810-197 is,
most surprisingly, a highly variable radio pulsar with a unusual flat
spectrum. This is the first confirmed example of radio flux from an
AXP. Herein, we report on our semi-annual XMM monitoring campaign that
has followed the pulsar for the last 3 years as its spectrum
evolved. Fitting a double blackbody model we find that the component
luminosities followed an exponential decay law with κ(BB1) = 870
days and κ(BB2) = 280 days, respectively. The temperatures of
these components cooled at a rate of 22% per year from the nearly
constant value recorded prior to 2004 March of kT(BB1) = 0.25 keV and
kT(BB2) = 0.67 keV, respectively. The latest data show that the
luminosity and temperature of the cooler component have effectively
returned to their quiescent levels and that its pulsed fraction, which
has steadily decreased with time, is now consistent with the previous
lack of detected pulsations in quiescence. We use the energy dependence
of the fading emission to decouple the pulsed components to solve for the
viewing and emitting geometry of XTE J1810-197. Finally, we consider
the emission mechanism(s) of XTE J1810-197 in the context of the
coronal loop magnetar model of Beloborodov & Thompson (2006).
This research is supported by XMM-Newton grant NNG05GJ61G and
NASA ADP grant ADP04-0059-0024.

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