1. October 10, 2002COSPAR Houston, TX1 X-Ray Spectral Morphologies of Young Supernova Remnants John P. Hughes Rutgers University  Cara Rakowski, Rutgers  Jessica Warren, Rutgers  Dave Burrows, Penn State  John Nousek, Penn State  Peter Roming, Penn State  Parviz Ghavamian, Rutgers  Pat Slane, CfA  Sangwook Park, Penn State  Gordon Garmire, Penn State  Anne Decourchelle, Saclay

2. October 10, 2002COSPAR Houston, TX2 Young Supernova Remnants Nucleosynthesis Nucleosynthesis Explosion Mechanism: neutrino driven convection, jets ? Explosion Mechanism: neutrino driven convection, jets ? Progenitor mass, influence on environment Progenitor mass, influence on environment Compact objects, pulsars and pulsar wind nebula (PWN) Compact objects, pulsars and pulsar wind nebula (PWN) Cosmic ray acceleration Cosmic ray acceleration Dynamical evolution of SNRs Dynamical evolution of SNRs Physics of high Mach number shocks Physics of high Mach number shocks

3. October 10, 2002COSPAR Houston, TX3 Overturning Our View of Cas A Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.

4. October 10, 2002COSPAR Houston, TX4 Oxygen-Rich SNR G292.0+1.8 Park et al 2001, ApJL, 564, L39

5. October 10, 2002COSPAR Houston, TX5 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

6. October 10, 2002COSPAR Houston, TX6 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

7. October 10, 2002COSPAR Houston, TX7 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

8. October 10, 2002COSPAR Houston, TX8 PSR J1124-5916 in G292.0+1.8 Discovered at Parkes (Camilo et al 2002) Discovered at Parkes (Camilo et al 2002) P=0.1353140749 s, dP/dt=7.471E-13 P=0.1353140749 s, dP/dt=7.471E-13 Characteristic age ~ 2900 yrs (SNR age ~ 1600 yrs) Characteristic age ~ 2900 yrs (SNR age ~ 1600 yrs) Not detected in coherent FFT of Chandra HRC observation Not detected in coherent FFT of Chandra HRC observation 3.5 sigma detection from Z n 2 test at radio parameters 3.5 sigma detection from Z n 2 test at radio parameters Only ~130 pulsed events in 50 ks Only ~130 pulsed events in 50 ks

9. October 10, 2002COSPAR Houston, TX9 PSR J1124-5916 Image Analysis: point source and elliptical gaussian (small nebula) Image Analysis: point source and elliptical gaussian (small nebula) Point source contains ~160 X-ray events Point source contains ~160 X-ray events Pulsed fraction high ~80% Pulsed fraction high ~80% Unpulsed point source emission < 1.4E-3 cts/s Unpulsed point source emission < 1.4E-3 cts/s L BB < 10 33 erg/s L BB < 10 33 erg/s Below standard cooling curve for 2000 yr old PSR

10. October 10, 2002COSPAR Houston, TX10 DEM L71: Ejecta and Shock Physics H alpha Soft X-ray Hughes, Ghavamian, Rakowski, and Slane, ApJL, in prep Rutgers Fabry-Perot/NOAO Chandra/NASA Hard X-ray

11. October 10, 2002COSPAR Houston, TX11 Fe-Rich Ejecta

12. October 10, 2002COSPAR Houston, TX12 Properties of DEM L71 Ejecta Outer rim: lowered abundances, ~0.2 solar (LMC ISM) Outer rim: lowered abundances, ~0.2 solar (LMC ISM) Core: enhanced Fe abundance, [Fe]/[O] > 5 times solar (ejecta) Core: enhanced Fe abundance, [Fe]/[O] > 5 times solar (ejecta) Thick elliptical shell, 32” by 40” across (3.9 pc by 4.8 pc) Thick elliptical shell, 32” by 40” across (3.9 pc by 4.8 pc) Dynamical mass estimate Dynamical mass estimate r’ ~ 3.0 M ej = 1.1 M ch (n/0.5 cm -3 ) Wang & Chevalier 2001 EM mass estimate EM mass estimate EM ~ n e n Fe V M Fe < 2 M sun Main error: source of electrons Main error: source of electrons Fe-rich, low mass SN Ia

13. October 10, 2002COSPAR Houston, TX13 DEM L71: Shock Physics Nonradiative Balmer-dominated shock Measure post-shock proton temperature X-ray emission from thermal bremsstralung Measure post-shock electron temperature

14. October 10, 2002COSPAR Houston, TX14 Nonradiative Balmer Shocks Nonradiative means that a radiative (cooling) zone does not form Nonradiative means that a radiative (cooling) zone does not form Low density (partially neutral) gas Low density (partially neutral) gas High velocity shocks High velocity shocks Narrow component: cold H I overrun by shock, collisionally excited Narrow component: cold H I overrun by shock, collisionally excited Broad component: hot postshock protons that charge exchange with cold H I Broad component: hot postshock protons that charge exchange with cold H I Ghavamian, Rakowski, Hughes, and Williams 2002, ApJ, in prep. Width of broad component yields post shock proton temperature (Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980)

15. October 10, 2002COSPAR Houston, TX15 Constraining the Electron Temperature Fit NEI shock models to 3 spatial zones to follow evolution of T e Fit NEI shock models to 3 spatial zones to follow evolution of T e Study 5 azimuthal regions with sufficient Chandra statistics and broad Halpha component Study 5 azimuthal regions with sufficient Chandra statistics and broad Halpha component Available data cannot constrain T e gradients Available data cannot constrain T e gradients Rakowski, Ghavamian, Hughes, & Williams 2002, ApJ, in prep. Data do determine mean T e Suggest partial to compete temperature equilibration

16. October 10, 2002COSPAR Houston, TX16 Results on T e /T p from DEM L71 Shows trend for higher equilibration for lower speed shocks Shows trend for higher equilibration for lower speed shocks X-ray/Halpha results consistent with other purely Halpha ones X-ray/Halpha results consistent with other purely Halpha ones

17. October 10, 2002COSPAR Houston, TX17 THE END