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

October 10, 2002October 10, 2002 COSPAR Houston, TXCOSPAR Houston, TX 11

X-Ray Spectral X-Ray Spectral Morphologies of Young Morphologies of Young Supernova RemnantsSupernova Remnants

John P. HughesJohn P. HughesRutgers UniversityRutgers 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


Young Supernova RemnantsYoung Supernova Remnants

NucleosynthesisNucleosynthesis Explosion Mechanism: neutrino driven convection, jets ?Explosion Mechanism: neutrino driven convection, jets ? Progenitor mass, influence on environmentProgenitor mass, influence on environment Compact objects, pulsars and pulsar wind nebula (PWN)Compact objects, pulsars and pulsar wind nebula (PWN) Cosmic ray accelerationCosmic ray acceleration Dynamical evolution of SNRsDynamical evolution of SNRs Physics of high Mach number shocksPhysics of high Mach number shocks


Overturning Our View of Cas AOverturning Our View of Cas A

Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.


Oxygen-Rich SNR G292.0+1.8Oxygen-Rich SNR G292.0+1.8

Park et al 2001, ApJL, 564, L39



Ejecta

Rich in O, Ne, and Mg, some Si

[O]/[Ne] < 1

No Si-rich or Fe-rich ejecta



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


Oxygen-Rich SNR G292.0+1.8Oxygen-Rich SNR G292.0+1.8Point source

Featureless power-law spectrum, photon index = 1.7

Surrounded by diffuse X-ray/radio nebula

Off center, implied speed of ~800 km/s


PSR J1124-5916 in G292.0+1.8PSR 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-13P=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 observationNot detected in coherent FFT of Chandra HRC observation 3.5 sigma detection from Z3.5 sigma detection from Znn

22 test at radio parameters test at radio parameters Only ~130 pulsed events in 50 ksOnly ~130 pulsed events in 50 ks


PSR J1124-5916PSR J1124-5916 Image Analysis: point source and elliptical gaussian (small Image Analysis: point source and elliptical gaussian (small

nebula)nebula) Point source contains ~160 X-ray eventsPoint source contains ~160 X-ray events Pulsed fraction high ~80%Pulsed fraction high ~80% Unpulsed point source emission < 1.4E-3 cts/sUnpulsed point source emission < 1.4E-3 cts/s LLBBBB< 10< 103333 erg/s erg/s

Below standard cooling curve for 2000 yr old PSRBelow standard cooling curve for 2000 yr old PSR


DEM L71: Ejecta and Shock DEM L71: Ejecta and Shock PhysicsPhysics

H alphaSoft X-ray

Hughes, Ghavamian, Rakowski, and Slane, ApJL, in prep

Rutgers Fabry-Perot/NOAOChandra/NASA

Hard X-ray


Fe-Rich EjectaFe-Rich Ejecta


Properties of DEM L71 EjectaProperties 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’ ~ 3.0Mej = 1.1 Mch (n/0.5 cm-3)

Wang & Chevalier 2001

EM mass estimateEM mass estimate

EM ~ ne nFe VMFe < 2 Msun

Main error: source of Main error: source of electronselectrons

Fe-rich, low mass SN Ia


DEM L71: Shock PhysicsDEM L71: Shock PhysicsNonradiative Balmer-dominated shockMeasure post-shock proton temperature

X-ray emission from thermal bremsstralungMeasure post-shock electron temperature


Nonradiative Balmer ShocksNonradiative Balmer Shocks

Nonradiative means that a radiative Nonradiative means that a radiative (cooling) zone does not form(cooling) zone does not form

Low density (partially neutral) gasLow density (partially neutral) gas High velocity shocksHigh velocity shocks Narrow component: cold H I overrun Narrow component: cold H I overrun

by shock, collisionally excitedby shock, collisionally excited Broad component: hot postshock Broad component: hot postshock

protons that charge exchange with protons that charge exchange with cold H Icold 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)


Constraining the Electron Constraining the Electron TemperatureTemperature

Fit NEI shock models to 3 spatial Fit NEI shock models to 3 spatial zones to follow evolution of Tzones to follow evolution of Tee

Study 5 azimuthal regions with Study 5 azimuthal regions with sufficient Chandra statistics and sufficient Chandra statistics and broad Halpha componentbroad Halpha component

Available data cannot constrain Available data cannot constrain TTe e gradientsgradients

Rakowski, Ghavamian, Hughes, & Williams 2002, ApJ, in prep.

Data do determine mean Te

Suggest partial to compete temperature equilibration


Results on TResults on Tee/T/Tp p from DEM L71from DEM L71

Shows trend for higher equilibration for lower speed shocksShows trend for higher equilibration for lower speed shocks X-ray/Halpha results consistent with other purely Halpha onesX-ray/Halpha results consistent with other purely Halpha ones


THE ENDTHE END

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