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X-Ray Spectral Morphologies of Young Supernova Remnants John P. Hughes Rutgers University

X-Ray Spectral Morphologies of Young Supernova Remnants John P. Hughes Rutgers University. Parviz Ghavamian, Rutgers Pat Slane, CfA Sangwook Park, Penn State Gordon Garmire, Penn State Anne Decourchelle, Saclay. Cara Rakowski, Rutgers Jessica Warren, Rutgers

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X-Ray Spectral Morphologies of Young Supernova Remnants John P. Hughes Rutgers University

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  1. X-Ray Spectral Morphologies of Young Supernova RemnantsJohn P. HughesRutgers University • Parviz Ghavamian, Rutgers • Pat Slane, CfA • Sangwook Park, Penn State • Gordon Garmire, Penn State • Anne Decourchelle, Saclay • Cara Rakowski, Rutgers • Jessica Warren, Rutgers • Dave Burrows, Penn State • John Nousek, Penn State • Peter Roming, Penn State COSPAR Houston, TX

  2. Young Supernova Remnants • Nucleosynthesis • Explosion Mechanism: neutrino driven convection, jets ? • Progenitor mass, influence on environment • Compact objects, pulsars and pulsar wind nebula (PWN) • Cosmic ray acceleration • Dynamical evolution of SNRs • Physics of high Mach number shocks COSPAR Houston, TX

  3. Overturning Our View of Cas A Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109. COSPAR Houston, TX

  4. Oxygen-Rich SNR G292.0+1.8 Park et al 2001, ApJL, 564, L39 COSPAR Houston, TX

  5. Oxygen-Rich SNR G292.0+1.8 Ejecta Rich in O, Ne, and Mg, some Si [O]/[Ne] < 1 No Si-rich or Fe-rich ejecta COSPAR Houston, TX

  6. Oxygen-Rich SNR G292.0+1.8 Normal Composition, CSM Central bright bar – an axisymmetric stellar wind (Blondin et al, 1996) Thin, circumferential filaments enclose ejecta-dominated material – red/blue supergiant winbd boundary COSPAR Houston, TX

  7. Oxygen-Rich SNR G292.0+1.8 Point source Featureless power-law spectrum, photon index = 1.7 Surrounded by diffuse X-ray/radio nebula Off center, implied speed of ~800 km/s COSPAR Houston, TX

  8. PSR J1124-5916 in G292.0+1.8 • Discovered at Parkes (Camilo et al 2002) • P=0.1353140749 s, dP/dt=7.471E-13 • Characteristic age ~ 2900 yrs (SNR age ~ 1600 yrs) • Not detected in coherent FFT of Chandra HRC observation • 3.5 sigma detection from Zn2 test at radio parameters • Only ~130 pulsed events in 50 ks COSPAR Houston, TX

  9. PSR J1124-5916 • Image Analysis: point source and elliptical gaussian (small nebula) • Point source contains ~160 X-ray events • Pulsed fraction high ~80% • Unpulsed point source emission < 1.4E-3 cts/s • LBB< 1033 erg/s Below standard cooling curve for 2000 yr old PSR COSPAR Houston, TX

  10. DEM L71: Ejecta and Shock Physics Chandra/NASA Rutgers Fabry-Perot/NOAO Hard X-ray H alpha Soft X-ray Hughes, Ghavamian, Rakowski, and Slane, ApJL, in prep COSPAR Houston, TX

  11. Fe-Rich Ejecta COSPAR Houston, TX

  12. Properties of DEM L71 Ejecta • Outer rim: lowered abundances, ~0.2 solar (LMC ISM) • Core: enhanced Fe abundance, [Fe]/[O] > 5 times solar (ejecta) • Thick elliptical shell, 32” by 40” across (3.9 pc by 4.8 pc) • Dynamical mass estimate Wang & Chevalier 2001 r’ ~ 3.0 Mej = 1.1 Mch (n/0.5 cm-3) • EM mass estimate EM ~ ne nFe V MFe < 2 Msun • Main error: source of electrons Fe-rich, low mass SN Ia COSPAR Houston, TX

  13. DEM L71: Shock Physics Nonradiative Balmer-dominated shock Measure post-shock proton temperature X-ray emission from thermal bremsstralung Measure post-shock electron temperature COSPAR Houston, TX

  14. Nonradiative Balmer Shocks • Nonradiative means that a radiative (cooling) zone does not form • Low density (partially neutral) gas • High velocity shocks • Narrow component: cold H I overrun by shock, collisionally excited • Broad component: hot postshock protons that charge exchange with cold H I (Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980) Width of broad component yields post shock proton temperature Ghavamian, Rakowski, Hughes, and Williams 2002, ApJ, in prep. COSPAR Houston, TX

  15. Constraining the Electron Temperature • Fit NEI shock models to 3 spatial zones to follow evolution of Te • Study 5 azimuthal regions with sufficient Chandra statistics and broad Halpha component • Available data cannot constrain Te gradients • Data do determine mean Te • Suggest partial to compete temperature equilibration Rakowski, Ghavamian, Hughes, & Williams 2002, ApJ, in prep. COSPAR Houston, TX

  16. Results on Te/Tp from DEM L71 • Shows trend for higher equilibration for lower speed shocks • X-ray/Halpha results consistent with other purely Halpha ones COSPAR Houston, TX

  17. THE END COSPAR Houston, TX

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