elemental composition and distribution in supernova ...€¦ · elemental composition and...
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Elemental Composition and Distribution in Supernova Remnants : X-ray Spectroscopy
Anne DecourchelleService d'Astrophysique
CEA Saclay, France
I - X-ray morphology of the interaction region
II - Spatially resolved X-ray spectroscopy of the ejecta
III -Spectroscopy of the forward shock: particle acceleration
Collaborators:
G. Cassam-Chenai (PhD student, CEA Saclay)
J. Ballet, J.L. Sauvageot (CEA Saclay)
U. Hwang, R. Petre (NASA Goddard)
J. Hughes (Rutgers Univ.), D. Ellison (NCSU)
<----------Ejecta --------->
2 shocksInterstellar medium
Contact discontinuity
Young supernova remnants
SN material ejected at high velocity⇒ Heating of the ejecta and ISM
Progenitor/supernova:
-Nucleosynthesis products
-Element mixing-Density structure
Shock physics:-Non-equipartition between Te and Ti
-Particle acceleration
Interaction with the ambient medium:
-Rayleigh-Taylor instabilities
X-ray morphology of the interaction region
Remnants of type II
supernova
Cas A
E0102.2-7219(SMC)
Chandra
5 arcmin
Continuum 4-6 keVGotthelf et al. 2001, ApJ 552, L39
Color image: 0.6-1.6 keV, 1.6-1.2 keV, 2.2-7.5 keV
X (Chandra) / Visible (HST) / Radio (ATCA)Gaetz et al. 2000, ApJ 534, L47
Rayleigh-Taylor instabilities at the interface
40 arcsecHughes et al. 2000, ApJ 528,
L109
Cas A: D = 3.4 kpc
E0102.2-7219: D = 60 kpc
Type : SN Ia (white dwarf deflagration) Distance ~ 2.3 kpc
=> Production of heavy elements (O, Ne, Mg, Si, S, Ar, Ca, Fe)
8 arcmin
Remnants of type Ia supernova: Tycho (SN 1572)
X-ray Chandra 0.5-10 keVRadio VLA 6 cm
DeLaney et al., 2002, ApJ 580, 914
Kepler's Supernova Remnant (SN 1604): SN type ?
SN I a ? Light curve (Baade 1943) and Large distance above the Galactic planeSN II ? Circumstellar medium suggested by optical observations
Distance ~ 5 kpc
3 arcmin
Dwarkadas and Chevalier 1998, ApJ 497, 807
RADIUS
DENSITYprofile without particle accelerationExponential =>SN Ia Power law => SN II Constant profile=> plateau
Arnett 1988, ApJ 331, 377
Ejecta
Log R (cm)
RADIUS
Blondin and Ellison 2001, ApJ 560, 244Decourchelle, Ellison, Ballet 2000, ApJ 543, L57
Initial conditions for SN 1987A:
Interaction structuredepends on the
initial profiles of density
X-ray spatially resolved spectroscopy of the ejecta
Decourchelle et al., 2001, A&A 365, L218
Fe-L Mg S
ArCa
Fe-K
Fe XVII
Ne X Lyα
Mg XI Heα
Si XIII Heα
Si XIV Lyα
Ca
Fe Kα
SAr
Cassam-Chenai, Decourchelle, Ballet et al., 2003, A&A submitted
Kepler
Si
EPIC PN
EPIC MOS1EPIC MOS2
Mg S
ArCa
Fe-K
O Ne Fe
Fe-L
Tycho
Cas A
Willingale et al., 2002, A&A
Overall X-ray spectra obtained with XMM-
Newton
Si
ChandraCas A
Abundance ratios : core collapse of a 12 M starWillingale et al., 2002 A&A 381, 1039
Abundance maps
S/Si Ar/Si Ca/Si
Mapping heavy
elements
Heating of the gas
Particle acceleration
Interaction with the
interstellar medium
Fe K image FeL contours 4-6 keV
Fe L Si K
XMM-NEWTON
Kepler's SNR
Si K
Fe L
NorthSpatial distribution of silicon and iron
Si K
Fe LSouth
Fe L image and Si K contours
Cas A Tycho Kepler
Azimuthally averaged radial profile
Nucleosynthesis products
=> Asymmetrical line emission
=> Similar global repartition
except in particular locations.
Azimuthally averaged radial profile
Fe L image and Fe K contours
Cas A Tycho Kepler
Fe L
Fe K
Iron K EQW + Fe Lcontours
Chandra XMM-Newton XMM-Newton
Spatial distributionof Fe K and L lines
=> Higher temperature
toward the interior for Tycho
and Kepler
=> Constraints on the initial
density profile
Exponential
Constant density
Power law
Good overall correlation between the Si K and Fe L images
- except in particular knots in Tycho and Kepler
- except in the southeast of Cas A: inversion between Fe and Si layers
Fe K emission peaks distinctly at a lower radius than Fe L
-> higher temperature towards the reverse shock: constraints on the initial density profile
North/south asymmetry in the line emission:
Tycho: spatial variations of the elemental abundances or/and temperature
Kepler: spatial variations of the ambient density
Temperaturein models
X-ray spectroscopy of the forward shock: particle acceleration
Thermal component: kT ~ 3.5 keV and net ~ 4 1010 cm-3sNon-thermal component:RIM: 84 % of the 4-6 keV continuum, power law α ~ 2.2INSIDE: 11% of the 4-6 keV continuum, power law α > 4.5
=>width of the rim inconsistent with thermal emission=> X-ray synchrotron due to limited lifetime
of the ultrarelativistic electrons.
Vink and Laming 2003, ApJ 584, 758
VLA radioX-ray continuumChandra
(x 10)
Spectrum of the forward shock in Cas A
No emission line features !
Thermal interpretation:
kT = 2.1 keV and net = 108 cm-3s => strong ionization delay but problem with the morphology
Non-thermal interpretation:
X-ray power law: α ~ 2.8
Rolloff frequency: ν ~7 1016 Hz
=> maximum electron energies ~ 1-12 TeV
Hwang, Decourchelle, Holt, Petre 2002, ApJ 581, 1101
Broad band x-raysRadio 22cmX-ray Continuum
Chandra Chandra
Spectrum of the forward shock in Tycho
Shocked ejecta:=> thermal non ionization equilibrium emission
Shocked ambient medium:=> synchrotron emission using radio constraintsMaximum energy of accelerated electrons ~ 60 TeV
Shocked ejecta
Shocked ambient medium
XMM Continuum
Chandra Continuum
Cassam-Chenai, Decourchelle, Ballet, et al. 2003, A&A submitted
Spectrum of the forward shock in Kepler
SNRs with different characteristics :
- Forward shock traced by the high energy continuum emission in Tycho and Kepler and located close to the contact discontinuity unlike Cas A: in all cases, spectra and morphology indicates a nonthermal origin -> electrons up to energies of 1-60 TeV
- Discovery of particularly bright and hard continuum knots on the eastern and western edges of Tycho -> possible sites of efficient acceleration ?
- Different asymmetries in the line emission and in the high energy continuum:asymmetry of the explosion in Cas A, effect of abundances or/and of temperature in Tycho, density variation in the ambient medium for Kepler
- Iron K line at a smaller radius than iron L line : higher temperature towards the reverse shock -> constraints on the density profile
A DETAILED SPECTRAL ANALYSIS AT SMALL SCALE IS REQUIRED TO QUANTIFY ABUNDANCES/ TEMPERATURE BUT MODEL DEPENDENT
CONCLUSIONS