Gamma-ray radiation from type IIb supernova remnants prospect for - - PowerPoint PPT Presentation

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gamma ray radiation from type iib supernova remnants
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Gamma-ray radiation from type IIb supernova remnants prospect for the Cerenkov Telescope Array A.marcowith (L.U.P.M.) In collaboration with M.Renaud (L.U.P.M.), V. Dwarkadas (Chicago university) & V. Tatischeff (C.S.N.S.M. Orsay)

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A.marcowith (L.U.P.M.) In collaboration with M.Renaud (L.U.P.M.), V. Dwarkadas (Chicago university) & V. Tatischeff (C.S.N.S.M. Orsay)

Gamma-ray radiation from type IIb supernova remnants prospect for the Cerenkov Telescope Array

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10/3/12 PHNE Meeting IAP 2

  • utlines
  • Introduction:

– Types and frequencies of supernovae (SN) – Type IIb SN: properties.

  • A test case: SN 1993J:

– Radio observations – Particle acceleration and magnetic field

  • Gamma-ray radiation from 1993J type objects:

– Pair opacity calculation – Observability by CTA – Other objects

  • Conclusions
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Types of Supernovae

All inject ~1051 ergs !

Cappellaro & Turatto’01

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Cappellaro & Turatto’01

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Cappellaro & Turatto’01

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SN rates

Cappellaro’99, vdBergh & Tamman’91 Smartt+09, Li+11

Milky way Ia 0.4+/-0.2 II 1.5+/-1 About 2 SN/century

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Type iib SN

  • Intermediary between II (H rich) and Ib/Ic (H poor).
  • Several well-known objects: SN1993J, Cassiopeia A
  • Mass loss by wind stripping (masses ~ 25 solar masses) or

interaction with a companion (rather favored, Claeys+11) (masses ~ 15 solar masses)

  • Rare events:

– vdBergh et al’05 3%+/-1% of core collapse Sne in 140 Mpc limited distance 1.5%+/-1.5% in 30 Mpc limited distance – Smartt’09 5.4+/-2.7% in 28 Mpc limited distance ~ one every millenary at a rate of SN 2/century

  • ! May enter in sequence MS=>RSG=>WNH=>SNIIb

– WNH Wolf-Rayet (Nitrogen, Hydrogen) associated with high loss rate (above 10-5 solar masses) and fast winds (2000 km/s) – But for other models SNIIb are not associated with any WR phases (e.g. Meynet+11)

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Maximum CR energy in type II SNR

  • Galactic CRs at PeV and beyond could be produced

right after the SN explosion; when the BW is propagating into the massive star wind (other models exist; e.g. Bykov’01, Parizot,A.M.+04)

  • For protons (Voelk & Biermann ’88, Bell & Lucek’01,

Ptuskin+10)

=> Hints toward slow winds, fast shocks, high loss mass rates: interesting case of iib SNR SN1993J Emax =3.5x1017eV (vsh,2E4)2 (Md,-5)1/2 (PCR,0.1ρu)(vw,10)-1/2)

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A test case: SN 1993J

  • Type IIb SN (Filippenko et al. 1993) discovered by F.

Garcia on 1993 March 28th in M81

– DCepheids = 3.63 +/- 0.34 Mpc (Freedman et al. 1994) – DESM = 3.96 +/- 0.29 Mpc (Bartel et al. 2007)

  • 13-20 Msun RedSuperGiant (RSG) which had

lost most of its H envelope to a close binary companion (Maund et al. 2004)

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Radio follow-up

Bietenholz+03 VLBI images @ 8.4Ghz

Shell @ T >175 days

Initial Vexp~18000 +/- 1000 km/s

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Hydrodynamic simulations of a self- similar evolution (Chevalier’82, Bartel+08)

θout ∝ t(n-3)/(n-s)

N:ejecta (n>5) S:circumstellar medium

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Light curves & spectra

θout ∝ tm m ~ 0.93 t<1yr m ~ 0.82 t>1yr

Bietenholz+11

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Light curves & spectra

Marti-Vidal+11

Fit synchrotron self-absorbed model B~64G (R/1015cm)-1 N(E) ∝ E-2.1 Argue for a constant amplification wrt to an ambient toroidal magnetic field (Bjornsson & Fransson’98)

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Magnetic field amplification

  • MF 3 orders of magnitude above MF-

wind equipartition

Beq=(uwMd)1/2/r=2.5 mG (Md,-5)1/2(uw,10)1/2(r,15)-1

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Conclusions from radio data

  • Forward shock dynamics

– No strong evidences at the outer edge of deviation from circular shape. – Expansion well reproduced by hydrodynamical models. – Most of the radio emission coming from the forward shock (?)

  • Magnetic field

– evolution in r-1 or t-1 – Amplification

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Some assumptions

From the outburst time:

  • MF is amplified through the Bell mechanism

(Bell’04)

  • hadrons are accelerated as well as

electrons. ⇒ Gamma-ray radiation ?

  • Inverse Compton
  • Neutral pion decay (density profile of circum

stellar medium)

  • The latter likely dominant in strong MF.
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Circumstellar medium

  • Effective density behind the forward shock:

neff = Mdr

eff

4Rsh,out

2uwmH (1+ 4X)

Neff~3109 cm-3 at t=0 (outburst) Density scales as r-2 with r(t=0)=3.5 1014 cm (deduced from θout(t)); Uw=10 km/s (velocity at infinity)

  • Stromgren sphere (B2 star) Rs ~13pc

ne,cm-3

  • 2/3: likely fully ionized medium
  • nce the RSG phase starts.
  • questioned after (but see

Fransson+96)

NB: 10 years at 104 km/s is 0.1pc.

  • Magnetic field (magnetization)

B~1milli G @ 1016 cm => σ ~ 2 10-9 << 1.

Reville+06

Bell instability growth rate Vs ionization fraction

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Cosmic Ray acceleration i

  • Estimation by Voelk & Biermann’88

– Non amplified MF:

  • K1=(c2/3)* E/(ZeBback(rs))
  • Oblique shock case: K2 = K1/2

– Linear acceleration: rtot=r=4 – Stellar radius ~ 400 solar radii

  • Other estimation:

– Amplified MF:

  • K1(Bampl)
  • Tangled MF at the shock front K2< K1/2

– Non-linear effects rtot>4 – Stellar radius RSG > 1000 solar radii.

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Cosmic Ray acceleration II

  • Iterative Fit radio data with a

synchrotron model

  • 1D non-linear model (Berezhko

& Ellison’99) – Vsh(t), Bu(t), TCSM,ρu(t) => solutions : fp,fe

  • Solutions stay close to the

test-particle regime (Alfvèn heating included).

  • Acceleration efficiency

increases with time up to 25% Tatischeff’09

  • Downstream: self-similar model by Chevalier’82

two differents solutions for B: advection/damping εNT=FCR/1/2ρuvsh

3

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Synchrotron model fitting

  • Fit radio emission of very young

SNR:

SN1993J Tatischeff’09

A factors = attenuation by

  • Homogeneous circumstellar matter
  • Clumps in circumstellar matter
  • Internal Synchrotron-self

asborption

  • Synchrotron model => MF

=> 4 parameters (K1,α, K3(CSM), K5(SSA)) fitted with 6 different wavebands (fig) Consistent with b=1 (also in other young objects SN2008D Ib/c)

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Cosmic Ray acceleration II

  • Iterative Fit radio data with a

synchrotron model

  • 1D non-linear model (Berezhko

& Ellison’99) – Vsh(t), Bu(t), TCSM,ρu(t) => solutions : fp,fe

  • Solutions stay close to the

test-particle regime (Alfvèn heating included).

  • Acceleration efficiency

increases with time up to 25% Tatischeff’09

  • Downstream: self-similar model by Chevalier’82

two differents solutions for B: advection/damping εNT=FCR/1/2ρuvsh

3

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Cosmic Ray acceleration II

  • Iterative Fit radio data with a

synchrotron model

  • 1D non-linear model (Berezhko

& Ellison’99) – Vsh(t), Bu(t), TCSM,ρu(t) => solutions : fp,fe

  • Solutions stay close to the

test-particle regime (Alfvèn heating included).

  • Acceleration efficiency

increases with time up to 25% Tatischeff’09

  • Downstream: self-similar model by Chevalier’82

two differents solutions for B: advection/damping εNT=FCR/1/2ρuvsh

3

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Magnetic field amplification

  • Observations (based on SSA model): B(t) = 501G (T/1d)-1.16
  • Link to microphysics through streaming instability

(Bell’04) Downstream Bd =(1/3+2/3rsub

2)1/2 BNR

This produces BNR in t-1

  • Growth timescale (Bell instability)

BNR

2=8πξCR ρuvsh 3/2φ; φ=ln(pmax/pmin)

τ=3.3x10-2 days (φ/15)(εNT/0.1)-1(Emax,PeV)(tday)-1.34 ξCR ∝pinj/vsh

2;pinj ξCR∝vsh=> ξCR∝vsh

  • 1

+Long wavelengths Bykov+11

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Maximum particle energy

  • Fixing up- and downstream magnetic fields
  • Bohm diffusion regime

– Fixes the maximum energy by escape losses and time limited effect Tatischeff’09

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Gamma-ray radiation

  • Total energy put into CRs (swept-up mass is <

Mej) from day 1 to 3100.

  • With a dense target gamma-rays are expected but

absorbed due to electron-positron pair production.

γ (gamma)γ(UV-optical)→e+/e-

ECR=∫dt4πRsh

2εNTFNT=7.9x1049 ergs

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Soft photons

SN photosphere => Black body, UV dominates the first week and hence T~7000 K after day 120.

Lewis+94 Aharonian+08 Bolometric luminosity

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At the level of F(>1TeV)~2 10-12cm-2 s-1 (Tatischeff’09, Kirk+95) Fermi HESS

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HESS Fermi

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Perspectives: Cerenkov Telescope Array

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But likely an underestimation Fermi CTA

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Anisotropic pair production

Rphot Rsh

Opacity ↑ Opacity ↓ As most gamma-ray photons are produced forward anisotropic pair production gives smaller opacities. Rear-on Head-on

Renaud, A.M.+ in prep

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Neutrinos

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Secondary leptons

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Perspectives: SN

  • If a Wolf-Rayet phase occurs after RSG phase then

the peak of gamma-ray emission is shifted in time.

  • majority of type II SN; i.e. IIP may enter in a simple

sequence MS(8-16 solar masses)=>RSG=>SNIIP

Meynet+11

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Mauron & Josselin’11

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SN IIP

  • Less luminous

=> decreases opacity to pair production => P=Plateau: mean luminosity higher with time wrt iib and IIL => extend the effect of pair production.

  • Remains to be tested.
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Conclusions

  • SNR associated with RSG phase are interesting
  • bjects:

– If medium fully ionized the Bell instability may grow fastly (within days timescale) – Maximum CR energies may reach PeV also rapidly (within days timescale)

  • SN 1993J is one of the most observed SN IIb at all

wavelengths

– Shock velocity ~ 0.2c, high magnetic field that may be interpreted as generated by CRs – High energy CRs may be produced within day timescales uploading a few % of SN explosion – Translated into gamma-rays signal modulo pair production can lead to a detection by CTA @ 5.6sigma within 50 days

  • Other targets to be tested e.g. SN IIP