X-ray Analysis And Modeling Of The Pulsar Wind Nebula In G0.9+0.1

Details X-ray Analysis And Modeling Of The Pulsar Wind Nebula In G0.9+0.1 X-ray Analysis And Modeling Of The Pulsar Wind Nebula In G0.9+0.1

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.3416h&link_type=abstract

American Astronomical Society, HEAD meeting #12, #34.16

Astronomy and Astrophysics

Astronomy

Scientific paper

The composite SNR G0.9+0.1 has been observed in different energy ranges. We performed a spatially resolved spectral study of the PWN in G0.9+0.1 using two observations with the XMM-Newton telescope. It shows that the spectral index within four annuli, covering the inner part of the PWN and centered on the assumed pulsar position, increases with growing distance to the pulsar. The surface brightness drops accordingly. A radially symmetric leptonic model was applied in order to reproduce the observed X-ray emission. With the adopted model we were able to reproduce the general characteristics of the spectra. Using the optimized parameter values, we compared the modeled inverse Compton radiation with the published H.E.S.S. very high energy γ-ray data.

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