1. January 8, 2003201st AAS Meeting1 Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High Energy Studies of Supernova Remnants with Chandra and XMM-Newton John P. Hughes Rutgers University

2. January 8, 2003201st AAS Meeting2 Crab Nebula SN1054 Time spacing ~6 weeks Polar jet, torus, inner ring (~0.2 pc) Highly dynamic Wisps move at ~0.5c (Hester et al 2002) PSR spin energy, relativistic wind Nature of wisps still debated

3. January 8, 2003201st AAS Meeting3 New Pulsars and CCOs Cas A CXOU J232327.9+584842 CCO PKS 1209-51/52 1E 1207.4-5209 424 ms (X-ray) G106.3+2.7 PSR J2229+6114 51.6 ms (radio) IC 443 CXOU J061705.3+222127 CCO G292.0+1.8 PSR J1124-5916 135 ms (radio) RX J0852.0-4622 CXOU J085201.4-461753 CCO 3C 58 PSR J0205+6449 65.7 ms (X-ray) G54.1+0.3 PSR J1930+1852 136 ms (radio)

4. January 8, 2003201st AAS Meeting4 3C 58 and NS Cooling Crab-like remnant Crab-like remnant Associated with SN 1181 Associated with SN 1181 65.68 ms PSR (Murray et al. 2002) 65.68 ms PSR (Murray et al. 2002) Distance 3.2 kpc Distance 3.2 kpc Spectrum of central source (Slane et al. 2002) Spectrum of central source (Slane et al. 2002) –Power law:  = 1.7 –T BB < 1.08 x 10 6 K for 12 km radius neutron star Below “standard” NS cooling curve Below “standard” NS cooling curve

5. January 8, 2003201st AAS Meeting5 Nucleosynthesis in CC SNe Hydrostatic nucleosynthesis Hydrostatic nucleosynthesis –During hydrostatic evolution of star –Builds up shells rich in H, He, C, O, and Si –Amount of C, O, Ne, Mg ejected varies strongly with progenitor mass Explosive nucleosynthesis Explosive nucleosynthesis –Some mechanism drives a shock wave with 10 51 + erg through the Fe-core –Burning front T’s of ~10 9 K cause explosive O- and Si- burning –Only affects the central parts of the star – outer layers retain their pre-SN composition

6. January 8, 2003201st AAS Meeting6 Explosive Nucleosynthesis Process T (10 9 K) Main Products Explosive complete Si-burning 5.0 “Fe”, He Explosive incomplete Si-burning 4.0 Si, S, Fe, Ar, Ca Explosive O-burning 3.3 O, Si, S, Ar, Ca Explosive Ne/C-burning 1.2 O, Mg, Si, Ne

7. January 8, 2003201st AAS Meeting7 Typical Mass Fractions Element Ex Ne Ex O Ex Si-i Ex Si-c O0.720.45 Ne0.13 Mg0.090.005 Si0.020.300.40 S0.200.25 Ar0.0250.06 Ca0.020.05 Fe0.200.70

8. January 8, 2003201st AAS Meeting8 Overturning Our View of Cas A Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.

9. January 8, 2003201st AAS Meeting9 Cas A - Doppler Imaging by XMM Similar velocity structures in different lines Similar velocity structures in different lines –SE knots blueshifted –N knots redshifted –Tight correlation between Si and S velocities Fe Fe –Note velocity distribution in N –Extends to more positive velocities than Si or S Willingale et al 2002, A&A, 381, 1039

10. January 8, 2003201st AAS Meeting10 Cas A – 3D Ejecta Model Red: Si K  Green: S K  Blue: Fe K  Circle: Main shock “Plane of the sky” “Rotated” Fe-rich ejecta lies outside Si/S-rich ejecta

11. January 8, 2003201st AAS Meeting11 N63A Middle-aged SNR Middle-aged SNR –34” (8.2 pc) in radius –2000-5000 yrs old –2 nd brightest LMC SNR “Crescent”-shaped features “Crescent”-shaped features –Similar to features in Vela –Clumps of high speed ejecta –Not ejecta dominated Triangular hole Triangular hole –X-ray absorption –Approx. 450 solar mass cloud –On near side No PSR or PWN No PSR or PWN – L X < 4x10 34 erg s -1 Warren, Hughes, & Slane, ApJ, in press (20 Jan 2003)

12. January 8, 2003201st AAS Meeting12 DEM L71 Middle-aged SNR Middle-aged SNR –36” (8.7 pc) in radius –4,000 yrs old Rims: LMC composition Rims: LMC composition Core: [Fe]/[O] > 5 times solar Core: [Fe]/[O] > 5 times solar Ejecta mass: 1.5 M sun Ejecta mass: 1.5 M sun Hughes, Ghavamian, Rakowski, & Slane 2003, ApJ, 582, L95 SN Ia ejecta

13. January 8, 2003201st AAS Meeting13 N49B Middle-aged SNR Middle-aged SNR –80” (19 pc) in radius –5000-10,000 yrs old Bright and faint rims Bright and faint rims –LMC composition –ISM density varies by x10 Ejecta Ejecta –Revealed by equivalent-width maps –Mg & Si rich, no strong O or Ne Park, Hughes, Slane, Burrows, Garmire, & Nousek 2003, ApJ, in prep.

14. January 8, 2003201st AAS Meeting14 SNR 0103-72.6 Middle-aged SNR Middle-aged SNR –87” (25 pc) in radius –>10,000 yrs old (?) Circular rim Circular rim –SMC composition Central bright region Central bright region –O, Ne, Mg, Si-rich ejecta –No Fe enhancement Park, et al 2003, ApJ, in prep.

15. January 8, 2003201st AAS Meeting15 DEM L71: Shock Physics Nonradiative Balmer-dominated shock Measure post-shock proton temperature X-ray emission from thermal bremsstralung Measure post-shock electron temperature HH X-ray

16. January 8, 2003201st AAS Meeting16 Constraining the Electron Temperature Fit plasma shock models to 3 spatial zones to follow evolution of T e Fit plasma shock models to 3 spatial zones to follow evolution of T e Study 5 azimuthal regions with sufficient Chandra statistics and broad H  component Study 5 azimuthal regions with sufficient Chandra statistics and broad H  component Available data cannot constrain T e gradients Available data cannot constrain T e gradients Rakowski, Ghavamian, & Hughes 2003, ApJ, submitted Data do determine mean T e Suggest partial to compete temperature equilibration

17. January 8, 2003201st AAS Meeting17 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 2003, ApJ, submitted. Width of broad component yields post shock proton temperature (Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980)

18. January 8, 2003201st AAS Meeting18 Results on T e /T p from DEM L71 Shows trend: higher equilibration for slower shocks Shows trend: higher equilibration for slower shocks X-ray/H  results consistent with other purely H  ones X-ray/H  results consistent with other purely H  ones

19. January 8, 2003201st AAS Meeting19 Future Directions X-ray expansion (proper motion) X-ray expansion (proper motion) –Cas A: done –SN1006, Tycho: this year –Magellanic Cloud SNRs: in a few years Ejecta census in LMC/SMC SNRs Ejecta census in LMC/SMC SNRs –Probe the “Life Cycle of Matter” Longer observations of PWN Longer observations of PWN –Explore range of dynamical variability More studies of shock physics More studies of shock physics –Explore variety of high Mach- number shocks

20. January 8, 2003201st AAS Meeting20 The End