January 8, 2003201st AAS Meeting1 Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High...
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Transcript of January 8, 2003201st AAS Meeting1 Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Physics: High...
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 11
Nucleosynthesis, Pulsars, Nucleosynthesis, Pulsars, Cosmic Rays, and Shock Cosmic Rays, and Shock
Physics: High Energy Physics: High Energy Studies of Supernova Studies of Supernova
Remnants with Remnants with ChandraChandra and and XMM-NewtonXMM-Newton
John P. HughesJohn P. Hughes
Rutgers UniversityRutgers University
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 22
Crab Nebula SN1054Crab Nebula SN1054Time 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
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 33
New Pulsars and CCOsNew Pulsars and CCOs
Cas ACas A CXOU CXOU J232327.9+584842J232327.9+584842
CCOCCO
PKS 1209-PKS 1209-51/5251/52
1E 1207.4-52091E 1207.4-5209 424 ms (X-424 ms (X-ray)ray)
G106.3+2.7G106.3+2.7 PSR J2229+6114PSR J2229+6114 51.6 ms 51.6 ms (radio)(radio)
IC 443IC 443 CXOU CXOU J061705.3+222127J061705.3+222127
CCOCCO
G292.0+1.8G292.0+1.8 PSR J1124-5916PSR J1124-5916 135 ms 135 ms (radio)(radio)
RX J0852.0-RX J0852.0-46224622
CXOU J085201.4-461753CXOU J085201.4-461753 CCOCCO
3C 583C 58 PSR J0205+6449PSR J0205+6449 65.7 ms (X-65.7 ms (X-ray)ray)
G54.1+0.3G54.1+0.3 PSR J1930+1852PSR J1930+1852 136 ms 136 ms (radio)(radio)
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 44
3C 58 and NS Cooling3C 58 and NS Cooling Crab-like remnantCrab-like remnant Associated with SN 1181Associated with SN 1181 65.68 ms PSR (Murray et 65.68 ms PSR (Murray et
al. 2002)al. 2002) Distance 3.2 kpcDistance 3.2 kpc Spectrum of central Spectrum of central
source (Slane et al. 2002)source (Slane et al. 2002)– Power law: Power law: = 1.7 = 1.7
– TTBBBB < 1.08 x 10 < 1.08 x 1066 K for 12 K for 12 km radius neutron starkm radius neutron star
Below “standard” NS Below “standard” NS cooling curvecooling curve
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 55
Nucleosynthesis in CC SNeNucleosynthesis in CC SNe Hydrostatic nucleosynthesisHydrostatic nucleosynthesis
– During hydrostatic evolution of starDuring hydrostatic evolution of star– Builds up shells rich in H, He, C, O, and SiBuilds up shells rich in H, He, C, O, and Si– Amount of C, O, Ne, Mg ejected varies strongly Amount of C, O, Ne, Mg ejected varies strongly
with progenitor masswith progenitor mass Explosive nucleosynthesisExplosive nucleosynthesis
– Some mechanism drives a shock wave with Some mechanism drives a shock wave with 10105151+ erg through the Fe-core+ erg through the Fe-core
– Burning front T’s of ~10Burning front T’s of ~1099 K cause explosive O- K cause explosive O- and Si-burningand Si-burning
– Only affects the central parts of the star – outer Only affects the central parts of the star – outer layers retain their pre-SN compositionlayers retain their pre-SN composition
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 66
Explosive NucleosynthesisExplosive Nucleosynthesis
ProcessProcess T (10T (1099 K)K) Main ProductsMain Products
Explosive complete Si-Explosive complete Si-burning burning 5.05.0 ““Fe”, HeFe”, He
Explosive incomplete Si-Explosive incomplete Si-burningburning 4.04.0 Si, S, Fe, Ar, CaSi, S, Fe, Ar, Ca
Explosive O-burningExplosive O-burning 3.33.3 O, Si, S, Ar, CaO, Si, S, Ar, Ca
Explosive Ne/C-burningExplosive Ne/C-burning 1.21.2 O, Mg, Si, NeO, Mg, Si, Ne
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 77
Typical Mass FractionsTypical Mass Fractions
ElemenElementt
Ex NeEx Ne Ex OEx O Ex Si-iEx Si-i Ex Si-cEx Si-c
OO 0.720.72 0.450.45
NeNe 0.130.13
MgMg 0.090.09 0.0050.005
SiSi 0.020.02 0.300.30 0.400.40
SS 0.200.20 0.250.25
ArAr 0.0250.025 0.060.06
CaCa 0.020.02 0.050.05
FeFe 0.200.20 0.700.70
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 88
Overturning Our View of Cas AOverturning Our View of Cas A
Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 99
Cas A - Doppler Imaging by Cas A - Doppler Imaging by XMMXMM
Similar velocity structures Similar velocity structures in different linesin different lines– SE knots blueshiftedSE knots blueshifted– N knots redshiftedN knots redshifted– Tight correlation between Tight correlation between
Si and S velocitiesSi and S velocities Fe Fe
– Note velocity distribution in Note velocity distribution in NN
– Extends to more positive Extends to more positive velocities than Si or Svelocities than Si or S
Willingale et al 2002, A&A, 381, 1039
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1010
Cas A – 3D Ejecta ModelCas 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
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1111
N63AN63A Middle-aged SNRMiddle-aged SNR
– 34” (8.2 pc) in radius34” (8.2 pc) in radius– 2000-5000 yrs old2000-5000 yrs old– 22ndnd brightest LMC SNR brightest LMC SNR
““Crescent”-shaped featuresCrescent”-shaped features– Similar to features in VelaSimilar to features in Vela– Clumps of high speed Clumps of high speed
ejectaejecta– Not ejecta dominatedNot ejecta dominated
Triangular hole Triangular hole – X-ray absorptionX-ray absorption– Approx. 450 solar mass Approx. 450 solar mass
cloudcloud– On near sideOn near side
No PSR or PWNNo PSR or PWN– LLXX < 4x10 < 4x103434 erg s erg s-1-1Warren, Hughes, & Slane, ApJ, in press (20 Jan
2003)
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1212
DEM L71DEM L71 Middle-aged SNRMiddle-aged SNR
– 36” (8.7 pc) in radius36” (8.7 pc) in radius– 4,000 yrs old4,000 yrs old
Rims: LMC compositionRims: LMC composition Core: [Fe]/[O] > 5 times solarCore: [Fe]/[O] > 5 times solar Ejecta mass: 1.5 MEjecta mass: 1.5 Msunsun
Hughes, Ghavamian, Rakowski, & Slane 2003, ApJ, 582, L95
SN Ia ejecta
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1313
N49BN49B Middle-aged SNRMiddle-aged SNR
– 80” (19 pc) in radius80” (19 pc) in radius– 5000-10,000 yrs old5000-10,000 yrs old
Bright and faint rimsBright and faint rims– LMC compositionLMC composition– ISM density varies by x10ISM density varies by x10
EjectaEjecta– Revealed by equivalent-width Revealed by equivalent-width
mapsmaps– Mg & Si rich, no strong O or NeMg & Si rich, no strong O or Ne
Park, Hughes, Slane, Burrows, Garmire, & Nousek 2003, ApJ, in prep.
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1414
SNR 0103-72.6SNR 0103-72.6 Middle-aged SNRMiddle-aged SNR
– 87” (25 pc) in radius87” (25 pc) in radius– >10,000 yrs old (?)>10,000 yrs old (?)
Circular rimCircular rim– SMC compositionSMC composition
Central bright regionCentral bright region– O, Ne, Mg, Si-rich ejectaO, Ne, Mg, Si-rich ejecta– No Fe enhancementNo Fe enhancement
Park, et al 2003, ApJ, in prep.
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1515
DEM L71: Shock PhysicsDEM L71: Shock PhysicsNonradiative Balmer-dominated shockMeasure post-shock proton temperature
X-ray emission from thermal bremsstralungMeasure post-shock electron temperature
H X-ray
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1616
Constraining the Electron Constraining the Electron TemperatureTemperature
Fit plasma shock models to 3 Fit plasma shock models to 3 spatial zones to follow evolution spatial zones to follow evolution of Tof Tee
Study 5 azimuthal regions with Study 5 azimuthal regions with sufficient Chandra statistics and sufficient Chandra statistics and broad Hbroad H component component
Available data cannot constrain TAvailable data cannot constrain Te e
gradientsgradients
Rakowski, Ghavamian, & Hughes 2003, ApJ, submitted
Data do determine mean Te
Suggest partial to compete temperature equilibration
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1717
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 2003, ApJ, submitted.
Width of broad component yields post shock proton temperature
(Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980)
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1818
Results on TResults on Tee/T/Tp p from DEM L71from DEM L71 Shows trend: higher equilibration for slower shocksShows trend: higher equilibration for slower shocks X-ray/HX-ray/H results consistent with other purely H results consistent with other purely H ones ones
January 8, 2003January 8, 2003 201st AAS Meeting201st AAS Meeting 1919
Future DirectionsFuture Directions
X-ray expansion (proper X-ray expansion (proper motion)motion)– Cas A: doneCas A: done– SN1006, Tycho: this yearSN1006, Tycho: this year– Magellanic Cloud SNRs: in a Magellanic Cloud SNRs: in a
few yearsfew years Ejecta census in LMC/SMC Ejecta census in LMC/SMC
SNRsSNRs– Probe the “Life Cycle of Probe the “Life Cycle of
Matter”Matter” Longer observations of PWNLonger observations of PWN
– Explore range of dynamical Explore range of dynamical variabilityvariability
More studies of shock physicsMore studies of shock physics– Explore variety of high Mach-Explore variety of high Mach-
number shocksnumber shocks