English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We model the pulse profiles and the phase resolved spectra of the anomalousX-ray pulsar 1E 1048.1-5937 obtained with XMM-Newton to map its surfacetemperature distribution during an active and a quiescent epoch. We develop andapply a model that takes into account the relevant physical and geometricaleffects on the neutron star surface, magnetosphere, and spacetime. Using thismodel, we determine the observables at infinity as a function of pulse phasefor different numbers and sizes of hot spots on the surface. We show that thepulse profiles extracted from both observations can be modeled with a singlehot spot and an antipodal cool component. The size of the hot spot changes from$\approx 80^{\circ}$ in 2007, 3 months after the onset of a dramatic fluxincrease, to $\approx 30^{\circ}$ during the quiescent observation in 2011,when the pulsed fraction returned to the pre-outburst $\approx$ 65\% level. Forthe 2007 observation, we also find that a model consisting of a single 0.4 keVhot spot with a magnetic field strength of $1.8 \times 10^{14}$ G accounts forthe spectra obtained at three different pulse phases but under predicts theflux at the pulse minimum, where the contribution to the emission from thecooler component is non-negligible. The inferred temperature of the spot staysapproximately constant between different pulse phases, in agreement with auniform temperature, single hot spot model. These results suggest that theemitting area grows significantly during outbursts but returns to itspersistent and significantly smaller size within a few year timescale.

Mapping the Surface of the Magnetar 1E 1048.1-5937 in Outburst and Quiescence Through Phase Resolved X-ray Spectroscopy