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Spatial/Spectral Studies of Supernova Remnants with Chandra and XMM-Newton John P. Hughes Rutgers University. New Pulsars and CCOs. 3C 58 and NS Cooling. Crab-like remnant Associated with SN 1181 65.68 ms PSR (Murray et al. 2002) Distance 3.2 kpc. - PowerPoint PPT Presentation
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May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 11
Spatial/Spectral Studies of Spatial/Spectral Studies of Supernova Remnants with Supernova Remnants with ChandraChandra and and XMM-NewtonXMM-Newton
John P. HughesJohn P. Hughes
Rutgers UniversityRutgers University
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 22
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)
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 33
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 44
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 55
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 66
Overturning Our View of Cas AOverturning Our View of Cas A
Hughes, Rakowski, Burrows, and Slane 2000, ApJL, 528, L109.
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 77
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 88
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 99
Oxygen-Rich SNR G292.0+1.8Oxygen-Rich SNR G292.0+1.8
Park et al 2001, ApJL, 564, L39
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1010
Oxygen-Rich SNR G292.0+1.8Oxygen-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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1111
Oxygen-Rich SNR G292.0+1.8Oxygen-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 wind boundary
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1212
Thermonuclear SupernovaeThermonuclear Supernovae SN Ia (Hoyle & Fowler 1960)SN Ia (Hoyle & Fowler 1960)
– No hydrogen, a solar mass of No hydrogen, a solar mass of 5656Ni, some Ni, some intermediate mass elements (O, Mg, Si, S,…)intermediate mass elements (O, Mg, Si, S,…)
– Subsonic burning (deflagration) of approx. Subsonic burning (deflagration) of approx. one Chandrasekhar mass of degenerate C/Oone Chandrasekhar mass of degenerate C/O
– C-O white dwarf accreting H/He-rich gas C-O white dwarf accreting H/He-rich gas from a companionfrom a companion
– No compact remnantNo compact remnant– Mean rate ~ 0.3 SNUMean rate ~ 0.3 SNU
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1313
Identifying Remnants of SN Identifying Remnants of SN IaIa
Balmer-dominated SNRs Balmer-dominated SNRs (partially neutral ISM)(partially neutral ISM)
Ejecta abundances (Si and Ejecta abundances (Si and Fe rich, poor in O and Ne)Fe rich, poor in O and Ne)
Remnant structure (uniform Remnant structure (uniform ISM, “smoother” ejecta, little ISM, “smoother” ejecta, little spectral variation)spectral variation)
Tycho
E0509-67.5
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1414
SN Ia Spectra and SN Ia Spectra and AbundancesAbundances
W7: Nomoto et al 1984, Thielemann et al 1993
WDD1: Iwamoto et al 1999
NEI fit: Warren et al 2003
Comparison to models O, Ne, Mg: relatively low Si, S, Ar, Ca: consistent Fe: very low (<0.1)
Other spectral results Fe: co-spatial with Si, but hotter and lower net
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1515
ISM Abundances of the LMCISM Abundances of the LMC
Using SNRs as a probe of the ISMUsing SNRs as a probe of the ISM 7 SNRs, ages from 2,000 yr to 20,000 7 SNRs, ages from 2,000 yr to 20,000
yryr Data from Data from ASCAASCA Spectra calculated for evolutionary Spectra calculated for evolutionary
models (Sedov solution)models (Sedov solution)– spatial variationspatial variation– temporal variationtemporal variation
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1616
LMC SNRs: Integrated AbundancesLMC SNRs: Integrated AbundancesFrom fits to ASCA global X-ray spectra of 7 evolved LMC
remnants
Hughes, Hayashi, & Koyama 1998, ApJ, 505, 732
N49BDEM L71
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1717
LMC Metal AbundancesLMC Metal Abundances
HHK95: ASCA X-ray SNRs
Duf84: UV/Optical spectra H II regions (Dufour 1984)
RD92: F supergiants (Mg, Si, Fe) (Russell & Bessel 1989)
H II regions, SNRs (O, Ne, S) (Russell & Dopita 1990)
SpecieSpeciess
HHK98HHK98 Duf84Duf84 RD92RD92
OO 8.21(7)8.21(7) 8.43(8)8.43(8) 8.35(6)8.35(6)
NeNe 7.55(8)7.55(8) 7.64(107.64(10))
7.61(5)7.61(5)
MgMg 7.08(7)7.08(7) . . .. . . 7.47(137.47(13))
SiSi 7.04(8)7.04(8) . . .. . . ~7.8~7.8
SS 6.77(13)6.77(13) 6.85(116.85(11))
6.70(9)6.70(9)
FeFe 7.01(11)7.01(11) . . .. . . 7.23(147.23(14))
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1818
DEM L71: Fe-Rich EjectaDEM L71: Fe-Rich Ejecta
Hughes, Ghavamian, Rakowski, & Slane 2003, ApJ, 582, L95
Middle-aged LMC SNRMiddle-aged LMC SNR–36” (8.7 pc) in radius36” (8.7 pc) in radius–4,000 yrs old4,000 yrs old
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 1919
Properties of DEM L71 EjectaProperties of DEM L71 Ejecta Outer rims: lowered abundances, ~0.2 solar (LMC ISM)Outer rims: 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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2020
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, submitted.
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2121
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2222
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, in press.
Data do determine mean Te
Suggest partial to complete temperature equilibration
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2323
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, in press.
Width of broad component yields post shock proton temperature
(Chevalier & Raymond 1978; Chevalier, Kirshner, & Raymond 1980)
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2424
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
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2525
Constellation-X Capabilities: Constellation-X Capabilities: Requirements for SNR studies Requirements for SNR studies
Spectral resolutionSpectral resolution– Velocity resolution <1000 km/s for O linesVelocity resolution <1000 km/s for O lines
Spatial resolutionSpatial resolution– <5” (minimum for LMC SNRs)<5” (minimum for LMC SNRs)
Significant low energy responseSignificant low energy response– Neutron star coolingNeutron star cooling
TimingTiming– <10’s msec for pulsar studies<10’s msec for pulsar studies
May 6, 2003May 6, 2003 Constellation-X WorkshopConstellation-X Workshop 2626
The EndThe End