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Shock modification at the rim of SN 1006

38° COSPAR Scientific Assembly 18-25 July 2010 Bremen, Germany. Shock modification at the rim of SN 1006. Marco Miceli University of Palermo, INAF-OAPa. Collaborators: F. Bocchino, A. Decourchelle, G. Maurin, S. Orlando, J. Ballet and the “SN 1006 team”

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Shock modification at the rim of SN 1006

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  1. 38° COSPAR Scientific Assembly 18-25 July 2010 Bremen, Germany Shock modification at the rim of SN 1006 Marco Miceli Universityof Palermo, INAF-OAPa Collaborators: F. Bocchino, A. Decourchelle, G. Maurin, S. Orlando, J. Ballet and the “SN 1006 team” F. Acero, G. Cassam Chenai, G. Dubner, E. Giacani, E. Helder, D. Kosenko, J. Vink

  2. Introduction We focus on thermal limbs of SN 1006 to study how particle acceleration modifies the thermodynamical properties of the shocked ISM. We take advantage of the deep XMM-Newton observations presented in the Decourchelle’s talk Thermal X-ray emission as a tracer of shock modification Energy drain+pressure of rel. particles (g=4/3) larger compressibility, and lower post shock temperature (e. g. Decourchelle et al. 2000, Blasi 2002 ) low T, high EM? high T, low EM? MiceliM.: Shock modification in SN 1006, Cospar 2010

  3. The quest for the shocked ISM No detection of X-ray emitting ISM in accelerating SNRs (e. g. Cassam-Chenai et al. 2004 for RX J1713.7-3946 and Cassam-Chenai & Hughes 2007 for Tycho) In archive observations of SN 1006, spectra are well described by one thermal component (ejecta), and one non-thermal component (synchrotron, SRCUT),ISM is statistically not needed (Acero et al. 2007, Miceli et al. 2009): no constrains for the ISM properties. How can we test the presence of “modified” ISM? Direct proof: failed, no detection of X-ray thermal emission Unmodified shock Indirect proof:small distance BW-CD (Miceli et al. 2009), observed also in Tycho SNR (Warren et al. 2005) projected BW/CD Miceli et al. 2009 angle MiceliM.: Shock modification in SN 1006, Cospar 2010

  4. 0.5-0.8 keV The new spectra MOS 1 Archive XMM-Newton observations • SRCUT + 1 Thermal component: c2=371.4 (234 d.o.f.) • SRCUT + 2 Thermal components: c2=309.9 (231 d.o.f.) The additional thermal component (with solar abunances significantly improves the quality of the fits! Detection of shocked ISM? WARNING: preliminary results, to be further investigated MiceliM.: Shock modification in SN 1006, Cospar 2010 New XMM-Newton observations

  5. ISM properties Are these values reasonable? In collisionless shocks at high Mach Te/Tp <<1 (e.g. Ghavamian et al. 2007). In SN 1006 Te/Tp < 0.07 (Ghavamian et al. 02), i.e.Te<3 keV, for vsh=5000 km/s (Katsuda et al. 09) Ellison et al 2010 0 300 time (yr) 900 1200 MiceliM.: Shock modification in SN 1006, Cospar 2010

  6. Azimuthal and radial profiles 0.5-0.8 keV 2-4.5 keV a b,b’,b” c,c’,c” a b c MiceliM.: Shock modification in SN 1006, Cospar 2010

  7. Conclusions • The new XMM data allow us to perform a very detailed analysis • We have detected the thermal X-ray emission from the shocked ISM • Further checks and tests are necessary (BKG subtraction, proton flares, etc.) • T, n, and tNEI of the shocked ISM are in agreement with those expected • Azimuthal profiles suggest larger shock modification in non-thermal limbs MiceliM.: Shock modification in SN 1006, Cospar 2010

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