Numerical Modeling of Thermal andNon-thermal Emission from SNRs

Towards a Synergy of Gamma-ray and X-ray Observations

Herman Lee (RIKEN)(Part of preliminary results are removed)
13年9月4日水曜日

Collaborators
Dan Patnaude (CfA)
Pat Slane (CfA)
Don Ellison (NCSU)
Hiro Nagataki (RIKEN)
Masaomi Ono (RIKEN)
Daniel Castro (MIT)Jack Hughes (Rutgers U)
Kris Eriksen (Rutgers U)
And you!

Behold!
The multi-wavelength era has comeTycho’s SNR
IRX-ray(thermal)

IC 443IR

opticalX-ray(synch)

FermiFermi

Plenty of data now available, and lots more to come.
But synergy of data in different energy bands is lacking.
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SNRs are complex stuff

SN1006 Chandra
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3

SNRs are complex stuff
All aspects linked together(non-linear)
Need multi-λ info andcomprehensive models
SN1006 Chandra
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3Outline
1. Our recipe for modeling broadbandemission from SNR shells using ourpowerful numerical tool
2. Recent work on detailed calculations ofthermal X-ray emission from SNRs
3. Applications to future missions including
CTA and Astro-H

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A recipe to model SNR emission properly

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BroadbandSpectrum
The 1st hurdle any model
must pass throughHL+ 2013 ApJ

X-ray GeVRadiosynchthermalπ0

SNR Vela Jr.
Need update fromSuzaku

sec.

epree+
cursorResort to next hurdles if still
can’t single out best model

ICbremMust check consistency:• Radio to TeV flux
• Spectral shapes• Inferred CR energetics• Required B-field, CSM, ESN

TeVesc. p6
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Thermal X-ray constrains
Gamma-ray origin

HL+ 2013 ApJ

SNR Vela Jr.

Hurdle #1.5
In SNRs, thermal X-ray
flux is coupled tobroadband emission!
Very important:
Predicted thermal flux
must not violate X-rayobservations

Thermal lines

Need update fromSuzaku

Thermal cont.

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Radial emission profile probes
Gamma-ray origin & CR accel efficiency
Hurdle #2
Radio, X-ray and TeVmorphology
constrain CR accel.
and E loss history

TeV
Models & H.E.S.S.
(no fitting)

CTA prediction (0o.02)
SNR Vela Jr.
H.E.S.S.
Aharonian et al (2007)

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HL+ 2013 ApJ8

X-ray synchrotron index distribution
constrains gamma-ray origin

Kishishita & Uchiyama 2013
XMM-Newton

SNR Vela Jr.
Synch Index

Hadronic and leptonic
models often predictvery different synchindex distributions(e.g. CSM, B-field)

Hurdle #3
XMM Newton
Best-fit leptonic

BDS ~ a few μG? Filaments?
Unsettled mystery
Best-fit hadronic

Radius [RFS]
HL+ 2013 ApJ
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FS9

What do we learn?
• A best-fit broadband model passing all theobservation hurdles tells us the gamma-ray
origin of a SNR (i.e. CR ion or e , or both)
Note: Leptonic does NOT mean there is no CR ion• But the ultimate goal is to constrain totalenergy in CR different types of SNR can
produce in its lifetime (hadronic and leptonicmodels often predict very different values)• Sometimes though, the progenitor nature ofa SNR is not even clear

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Detailed study of thermal
X-ray from SNR ejecta and shell
Purposes:
1. Unambiguously reveal progenitor properties(e.g. metallicity in type Ia’s and core-collapses)

Patnaude+ 2012 on Kepler’s
progenitor and CSM usingChandra X-ray spectrum

2. Constrain explosive nucleosynthesis in various SNe
3. Correlate with CSM environments and broadband
emission, better understanding of SNR populations

Key:
1. Future X-ray spectroscopy by Astro-H SXS!
2. Self-consistent simulation of X-ray spectra by a CR +hydrodynamical model using inputs from SN simulations(connect SN and SNR phase)ρAn asymmetric
explosive
nucleosynthesis
model of a 16.3
Msun star(Ono,Nagataki, Ito,HL+ 2013)

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Following ionization
fractions of key elements
like O, Si, S and Fe using
full NEI coupled withhydro is crucial

log(Ion fraction)log(Ion fraction)

Non-equilibrium
ionization in
SNR ejecta

nISM = 0.2 cm-3
nISM = 2.0 cm-3

RS
Siliconiil mer
Pyr
na

CD
R [RRS]CDRS

OxygenR [RRS12]

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Heavy iontemperatureequilibration

Test cal. of equilibration in a Lagrangian cellTion
TpTe

Individual heavy
ion temperatures
must be followed to
predict line profiles

Core-collapseTime

ThermonuclearTime

Preliminary

e- temperaturecontrols NEI rates
and continuum inshocked ejecta
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Progenitor models
and X-ray spectra from SNR ejecta
CCPreliminary

500yr nISM = 0.2 cm-3Core-collapse
O Fe LNeSiSFe K

Type Ia

Ia
data from Carles Badenes (private comm.)

Type Ia (sub-energetic)
0.3keV

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1412keVTime evolutionII) X-ray spectrum
Preliminary
We can explore
evolutionary relation
between thermal X-ray
and non-thermal emission
as the multi-λ sample ofSNRs increases in size

Synch
time
timeThermalCore-collapse

Shockedejecta

ShockedCSM
Type Ia

Type Ia (sub-energetic)
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Synergy of future super telescopes
for SNR researchHi-res X-ray spectroscopy• Ejecta/CSM composition from faint lines• Unveil progenitor properties of Ia andcore-collapse SNRs
• SN explosion mechanisms, matter
mixing and nucleosynthesis• Broadened line profiles:
gas dynamics, temperature equilibration
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Hi-sensitivity, hi-res imaging• Many new gamma-ray SNR discoveries• Low-noise spectrum measurementfrom ~20GeV to >100 TeV• Measure roll-over region of CR spectra!
• 3x better TeV morphology measurement
to contrast with radio/IR/X-ray images
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Summary• We stressed the importance of synergy ofmulti-wavelength data to understand SNRemission and their contribution to CR• We introduced our strategy on modelingcurrent and future SNR observations using
our powerful numerical tool

• We elaborated on examples of new SNR
sciences achievable by next-generation
telescopes in conjunction with our code.

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