6533b829fe1ef96bd128ad14

RESEARCH PRODUCT

SHOCK-CLOUD INTERACTION AND PARTICLE ACCELERATION IN THE SOUTHWESTERN LIMB OF SN 1006

A. DecourchelleS. OrlandoF. BocchinoG. DubnerF. AceroM. MiceliS. OrlandoF. BocchinoE. TrojaG. DubnerF. AceroM. Miceli

subject

Ciencias FísicasAstrophysics::High Energy Astrophysical PhenomenaHadronSynchrotron radiationAstrophysicsSpectral lineISM: cloudIndentationSupernova remnantISM: individual objects (SN 1006)acceleration of particleISM: supernova remnantAstrophysics::Galaxy Astrophysicsacceleration of particlesPhysicssupernova remnants X-rays: ISM [ISM]Astronomy and AstrophysicsX-rays: ISMShock (mechanics)Particle accelerationAstronomíaSpace and Planetary Scienceindividual objects: SN 1006 [ISM]clouds [ISM]CIENCIAS NATURALES Y EXACTASFermi Gamma-ray Space Telescope

description

The supernova remnant SN 1006 is a powerful source of high-energy particles and evolves in a relatively tenuous and uniform environment despite interacting with an atomic cloud in its northwestern limb. The X-ray image of SN 1006 reveals an indentation in the southwestern part of the shock front and the H I maps show an isolated (southwestern) cloud, having the same velocity as the northwestern cloud, whose morphology fits perfectly in the indentation. We performed spatially resolved spectral analysis of a set of small regions in the southwestern nonthermal limb and studied the deep X-ray spectra obtained within the XMM-Newton SN 1006 Large Program. We also analyzed archive H I data, obtained by combining single-dish and interferometric observations. We found that the best-fit value of N H derived from the X-ray spectra significantly increases in regions corresponding to the southwestern cloud, while the cutoff energy of the synchrotron emission decreases. The N H variation corresponds perfectly with the H I column density of the southwestern cloud, as measured from the radio data. The decrease in the cutoff energy at the indentation clearly reveals that the back side of the cloud is actually interacting with the remnant. The southwestern limb therefore presents a unique combination of efficient particle acceleration and high ambient density, thus being the most promising region for γ-ray hadronic emission in SN 1006. We estimate that such emission will be detectable with the Fermi telescope within a few years. Fil: Miceli, M.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia Fil: Acero, F.. National Aeronautics And Space Administration. Goddart Institute For Space Studies; Estados Unidos Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Decourchelle, A.. Universite Paris Diderot - Paris 7; Francia Fil: Orlando, S.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia Fil: Bocchino, F.. Istituto Nazionale Di Astrofísica. Osservatorio Astronómico Di Palermo; Italia

yearjournalcountryeditionlanguage
2014-02-20
10.1088/2041-8205/782/2/l33