spatial/spectral studies of supernova remnants with chandra and xmm-newton john p. hughes

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


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)


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


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


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


Overturning Our View of Cas AOverturning Our View of Cas A

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


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


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


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 wind boundary


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


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


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


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


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


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))


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


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


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.


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


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


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)


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


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


The EndThe End

spatial/spectral studies of supernova remnants with chandra and xmm-newton john p. hughes

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