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Crab Nebula SN1054

Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High Energy Studies of Supernova Remnants with Chandra and XMM-Newton John P. Hughes Rutgers University. Crab Nebula SN1054. Time spacing ~6 weeks Polar jet, torus, inner ring (~0.2 pc) Highly dynamic Wisps move at ~0.5c

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Crab Nebula SN1054

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  1. Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High Energy Studies of Supernova Remnants with Chandra and XMM-Newton John P. Hughes Rutgers University 201st AAS Meeting

  2. 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 201st AAS Meeting

  3. New Pulsars and CCOs 201st AAS Meeting

  4. 3C 58 and NS Cooling • Crab-like remnant • Associated with SN 1181 • 65.68 ms PSR (Murray et al. 2002) • Distance 3.2 kpc • Spectrum of central source (Slane et al. 2002) • Power law: G = 1.7 • TBB < 1.08 x 106 K for 12 km radius neutron star • Below “standard” NS cooling curve 201st AAS Meeting

  5. Nucleosynthesis in CC SNe • 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 • Some mechanism drives a shock wave with 1051+ erg through the Fe-core • Burning front T’s of ~109 K cause explosive O- and Si-burning • Only affects the central parts of the star – outer layers retain their pre-SN composition 201st AAS Meeting

  6. Explosive Nucleosynthesis 201st AAS Meeting

  7. Typical Mass Fractions 201st AAS Meeting

  8. Overturning Our View of Cas A Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109. 201st AAS Meeting

  9. Cas A - Doppler Imaging by XMM • Similar velocity structures in different lines • SE knots blueshifted • N knots redshifted • Tight correlation between Si and S velocities • Fe • Note velocity distribution in N • Extends to more positive velocities than Si or S Willingale et al 2002, A&A, 381, 1039 201st AAS Meeting

  10. Cas A – 3D Ejecta Model “Plane of the sky” “Rotated” Red: Si Ka Green: S Ka Blue: Fe Ka Circle: Main shock Fe-rich ejecta lies outside Si/S-rich ejecta 201st AAS Meeting

  11. N63A • Middle-aged SNR • 34” (8.2 pc) in radius • 2000-5000 yrs old • 2nd brightest LMC SNR • “Crescent”-shaped features • Similar to features in Vela • Clumps of high speed ejecta • Not ejecta dominated • Triangular hole • X-ray absorption • Approx. 450 solar mass cloud • On near side • No PSR or PWN • LX < 4x1034 erg s-1 Warren, Hughes, & Slane, ApJ, in press (20 Jan 2003) 201st AAS Meeting

  12. DEM L71 • Middle-aged SNR • 36” (8.7 pc) in radius • 4,000 yrs old • Rims: LMC composition • Core: [Fe]/[O] > 5 times solar • Ejecta mass: 1.5 Msun SN Ia ejecta Hughes, Ghavamian, Rakowski, & Slane 2003, ApJ, 582, L95 201st AAS Meeting

  13. N49B • Middle-aged SNR • 80” (19 pc) in radius • 5000-10,000 yrs old • Bright and faint rims • LMC composition • ISM density varies by x10 • Ejecta • Revealed by equivalent-width maps • Mg & Si rich, no strong O or Ne Park, Hughes, Slane, Burrows, Garmire, & Nousek 2003, ApJ, in prep. 201st AAS Meeting

  14. SNR 0103-72.6 • Middle-aged SNR • 87” (25 pc) in radius • >10,000 yrs old (?) • Circular rim • SMC composition • Central bright region • O, Ne, Mg, Si-rich ejecta • No Fe enhancement Park, et al 2003, ApJ, in prep. 201st AAS Meeting

  15. DEM L71: Shock Physics Nonradiative Balmer-dominated shock Measure post-shock proton temperature X-ray emission from thermal bremsstralung Measure post-shock electron temperature Ha X-ray 201st AAS Meeting

  16. Constraining the Electron Temperature • Fit plasma shock models to 3 spatial zones to follow evolution of Te • Study 5 azimuthal regions with sufficient Chandra statistics and broad Ha component • Available data cannot constrain Te gradients • Data do determine mean Te • Suggest partial to compete temperature equilibration Rakowski, Ghavamian, & Hughes 2003, ApJ, submitted 201st AAS Meeting

  17. 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 2003, ApJ, submitted. 201st AAS Meeting

  18. Results on Te/Tp from DEM L71 • Shows trend: higher equilibration for slower shocks • X-ray/Ha results consistent with other purely Ha ones 201st AAS Meeting

  19. Future Directions • 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 • Probe the “Life Cycle of Matter” • Longer observations of PWN • Explore range of dynamical variability • More studies of shock physics • Explore variety of high Mach-number shocks 201st AAS Meeting

  20. The End 201st AAS Meeting

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