rays, cosmic rays and s s from from rays, cosmic rays and - - PowerPoint PPT Presentation
rays, cosmic rays and s s from from rays, cosmic rays and Astrophysical Sources ( Sources (GRBs GRBs) ) Astrophysical Soebur Razzaque Soebur Razzaque U.S. Naval Research Laboratory, Washington, D.C. U.S. Naval
CRIS 2010, September 13-17, CRIS 2010, September 13-17, Catania Catania, Italy , Italy
Large Area Telescope (LAT)
Pair conversion detector Energy Range: 20 MeV to >300 GeV
[20 MeV to 30 GeV for EGRET]
Effective Area: 9000 cm2
[1500 cm2 for EGRET]
Field of View: 2 sr [0.5 sr for EGRET] Angular resolution: <3.5o at >100 MeV
[5.8o at 100 MeV for EGRET] Gamma-ray Burst Monitor (GBM)
12 NaI detectors (8 keV - 1 MeV) 2 BGO detectors (150 keV - 30 MeV) Field of view: 8 sr
Survey mode (3.5 hr full sky) Pointing mode Automatic pointing mode for GRBs
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Delayed onset of LAT ≥ ≥ 100 100 MeV MeV emission compared to emission compared to keV-MeV keV-MeV
Hard additional power-law component dominant in the dominant in the ≥ ≥ 100 100 MeV MeV and in some cases in the <100 and in some cases in the <100 keV keV ranges ranges
Extended ≥ ≥ 100 100 MeV MeV emission in LAT well after emission in LAT well after keV-MeV keV-MeV emission emission falls below GBM detection threshold falls below GBM detection threshold
Jet velocity (bulk Lorentz Lorentz factor) factor)
Prompt emission (internal shocks?), afterglow emission
Emission mechanism: synchrotron, Compton, hadronic
Limits on quantum gravity models: M MQG
QG
≥ ≥ 1.2 1.2 M MPl
Pl
[GRB 090510] [GRB 090510]
Constraints on the extragalactic background light (EBL) models by Stecker Stecker et al. (2006) [GRB 080916C, GRB 090902B] et al. (2006) [GRB 080916C, GRB 090902B]
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8 – 250 keV 0.26 – 5 MeV > 100 MeV > 1 GeV All LAT events
No significant emission No significant emission in the LAT energy in the LAT energy range for the first range for the first ~4 s ~4 s 1st >100 1st >100 MeV MeV at ~4s at ~4s 1st >1 GeV at ~6s. 1st >1 GeV at ~6s. Delayed >100 Delayed >100 MeV MeV emission is common in emission is common in most other bright LAT most other bright LAT GRBs GRBs as well as well
GBM LAT
Abdo et al. Science, 2009
090510 090926A 090902B
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Time-integrated and time-resolved spectroscopy of 2 bright LAT Time-integrated and time-resolved spectroscopy of 2 bright LAT GRBs GRBs
Phenomenological Band function (2 smoothly connected power laws, 4 parameters)
fit ~100 keV - few MeV data well
Extra power-law component (2 parameters) is required to fit >100 MeV LAT
emission and below ~100 keV in some cases Band Power-law 090902B 090902B
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α+2 β+2 090510 090510
Bright LAT Bright LAT GRBs GRBs show significant show significant high energy emission extending after high energy emission extending after the the low energy emission low energy emission disappear disappear below below detectability detectability t -1.38+/-0.07
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090510 090510 080916C 080916C
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Very high jet bulk Very high jet bulk Lorentz Lorentz factor factor
Calculated from Calculated from γγ γγ → → e e+
+e
e-
pair production opacity argument ( production opacity argument (τ τγγ
γγ
= 1) = 1) for for ≥ ≥10 GeV source photons (co-spatial 10 GeV source photons (co-spatial with with keV-MeV keV-MeV photons) from photons) from GRBs GRBs detected with Fermi LAT detected with Fermi LAT Minimum jet bulk Minimum jet bulk Lorentz Lorentz factors factors
GRBs Some caveats Some caveats
The PL component may Originate from physically Originate from physically Separate region Separate region
Radiation transport effect Both lead to lower Both lead to lower Γ Γ by a factor ~2 by a factor ~2 Preliminary studies show that non- Preliminary studies show that non- LAT but bright GBM bursts has LAT but bright GBM bursts has systematically lower systematically lower Γ Γ Calculation of Calculation of Γ Γ from onset of from onset of afterglow also results in high values afterglow also results in high values
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Rees, Meszaros, Piran and others … “standard GRB model”
Synchrotron emission by shocked electrons for prompt and afterglow emission
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Synchrotron self Compton (
(Abdo Abdo et al. 2010; et al. 2010; Toma Toma, Wu & , Wu & Meszaros Meszaros 2010) 2010)
Photopion and cascade radiation and cascade radiation (Asano,
(Asano, Guiriec Guiriec & & Meszaros Meszaros 2009) 2009)
Proton synchrotron and cascade radiation (Razzaque,
(Razzaque, Dermer Dermer & Finke 2010) & Finke 2010)
Synchrotron radiation from a highly radiative radiative blast wave blast wave (
(Ghirlanda Ghirlanda et al. 2009; et al. 2009; Ghisellini Ghisellini et al. 2009) et al. 2009)
Synchrotron radiation from an adiabatic blast wave (Kumar &
(Kumar & Barniol-Duran Barniol-Duran 2009; 2009; Gao Gao et al. 2009) et al. 2009)
Synchrotron radiation from two component jet (
(Corsi Corsi, , Guetta Guetta & & Piro Piro 2009) 2009)
Proton synchrotron radiation from an adiabatic blast wave from an adiabatic blast wave (Razzaque 2010)
(Razzaque 2010)
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Can not produce delay longer than the pulse width, the pulse width, ~ 0.01 s - 0.1 s ~ 0.01 s - 0.1 s
Can not produce excess emission at <100 at <100 keV keV
Energetically efficient
( (Abdo Abdo et al., et al., ApJ ApJ, 2010) , 2010)
20
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Acceleration to 10 Acceleration to 1020
20
eV eV requires large magnetic field - requires large magnetic field - Fermi mechanism Fermi mechanism
Collision between two plasma Collision between two plasma “ “shells shells” ” ejected by a black hole ejected by a black hole “ “central engine central engine” ”
Relativistic forward & reverse shockwaves plough through the Relativistic forward & reverse shockwaves plough through the “ “shells shells” ”
Plasma instabilities, turbulent motion generate magnetic field Plasma instabilities, turbulent motion generate magnetic field
Charged particles (
Charged particles (test particle test particle) are accelerated in the induced electric field ) are accelerated in the induced electric field
n’a n’b ΓFS ΓRS Γ up = e
1L
4R22c B2 8 = Bup
Emax = Q B r = Ze
ec 21020 Z
e L 1046ergs s1 eV
Γb Γa Γ
UHECR Gamma ray Neutrino Black hole Plasma “shells” Colliding “shells” Particle energy density in the shocked fluid Non-thermal γ-ray luminosity
Collision hydrodynamics
Power requirement to Produce 1020 eV CRs Maximum CR energy Maximum CR energy
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acceleration synchrotron B’ = 100 kG Γ = 1000 tv = 0.1 s dynamic photopion Esat,p~2x1020 eV tsat=0.01s
UHECR acceleration in magnetic field and interactions UHECR acceleration in magnetic field and interactions may may provide provide γ γ ray signature from ray signature from GRBs GRBs, specially in , specially in Fermi Fermi LAT LAT
Synchrotron radiation and associated e e+
+e
e-
cascade radiation
Photohadronic interactions with observed interactions with observed keV keV -
MeV γ γ rays and cascade emission rays and cascade emission
Razzaque, Dermer, Finke & Atoyan, arXiv:0811.1160
Very high jet bulk Lorentz Lorentz factor reduces factor reduces photohadronic photohadronic cooling cooling
Could work in other bright GBM bursts bright GBM bursts
A γγ γγ cutoff in HE cutoff in HE spectrum would spectrum would be an be an indication indication
Synchrotron cooling is dominant in high dominant in high B B field field
GRB 080916C
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Particle acceleration in the forward shock Particle acceleration in the forward shock B B field field
Cooling is dominated by synchrotron radiation in the same Cooling is dominated by synchrotron radiation in the same B B field field
Minimum LF Minimum LF Cooling LF Cooling LF t tsyn
syn
= = t tdyn
dyn
Saturation LF Saturation LF t tsyn
syn
= = t tacc
acc
Injection Injection spectrum spectrum Cooled spectrum Cooled spectrum
Synchrotron spectrum Synchrotron spectrum
Fast cooling Fast cooling γ γm
m >
> γ γc
c or
νm
m >
> ν νc
c
All break frequencies evolve with time as the
All break frequencies evolve with time as the B B field (and field (and Γ Γ) does ) does
dN d
p sat m p1 t (fast cooling) (fast cooling)
F
sat m p / 2 1/ 2 1/ 3 t t
(slow cooling) (slow cooling) ( p1)/ 2
F
sat c p / 2 1/ 3 t t
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Particle acceleration in the forward shock Particle acceleration in the forward shock B B field field
Cooling is dominated by synchrotron radiation in the same Cooling is dominated by synchrotron radiation in the same B B field field
Minimum LF Minimum LF Cooling LF Cooling LF t tsyn
syn
= = t tdyn
dyn
Saturation LF Saturation LF t tsyn
syn
= = t tacc
acc
Injection Injection spectrum spectrum Cooled spectrum Cooled spectrum
Synchrotron spectrum Synchrotron spectrum
Fast cooling Fast cooling γ γm
m >
> γ γc
c or
νm
m >
> ν νc
c ;
; Slow cooling Slow cooling γ γm
m <
< γ γc
c or
νm
m <
< ν νc
c
All break frequencies evolve with time as the
All break frequencies evolve with time as the B B field (and field (and Γ Γ) does ) does
dN d
p sat m p1 t
Fermi Fermi LAT LAT
emission (>100
emission (>100 MeV MeV) ) modeled by proton-synchrotron modeled by proton-synchrotron radiation radiation from a coasting from a coasting (constant bulk (constant bulk Lorentz Lorentz factor) factor) GRB fireball GRB fireball
Synchrotron radiation by proton and associated associated e e+
+e
e-
cascade from from γγ γγ
Accumulation of protons cooling in time cooling in time build-up flux in LAT build-up flux in LAT Can explain delayed Can explain delayed emission in LAT emission in LAT
Requires large (~10 ~102
2 ×
× γ γ rays rays) ) energy budget energy budget
Narrow (1/Γ Γ) jet opening angle can help ) jet opening angle can help by reducing actual energy release by reducing actual energy release
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Razzaque, Dermer & Finke, arXiv:0908.0513
GRB 080916C GRB 080916C
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tdec 1.9(1+ z)(E55/n)1/33
8/3 s
Energy injection rate in the forward shock: forward shock:
Deceleration time:
Bulk Lorentz Lorentz factor: factor:
Total KE in Total KE in blast wave = blast wave = swept-up material swept-up material
Blandford Blandford & McKee 1976 & McKee 1976
Blast wave radius:
Magnetic field in the FS:
1/2 (E55n3)1/8ts 3/8 G
Relationship between t t, , Γ Γ and and R R : :
R = 22act(1+ z)1 a a = 1 = 1 for coasting for coasting a a = 4 = 4 after after decel decel. .
763(1+ z)3/8 (E55/n)1/8ts
3/8
R 1.4 1017(1+ z)1/4 (E55/n)1/4 ts
1/4 cm
eshock = 4nmpc 22
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Sari, Sari, Piran Piran & & Narayan Narayan 1998 1998
Fast cooling : Fast cooling : ν νm
m >
> ν νc
c
Slow cooling : Slow cooling : ν νc
c >
> ν νm
m
c < < m : F
1/ 2t1/ 4
>m > c : F
p / 2t(3/ 4)( p2/ 3)
m < < c : F
( p1)/ 2t(3/ 4)( p1)
>c > m : F
p / 2t(3/ 4)( p2/ 3)
Fν ∝ ν−β t−α closure relations closure relations Fν ∝ ν−β t−α closure relations closure relations
p-particle particle spectral index : spectral index : dN
dE Ep
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t -1.38±0.07
Earth occultation
Afterglow
Multi wavelength light curve in Multi wavelength light curve in γ γ ray, x ray and UV ray, x ray and UV fitted with fitted with p- p- and and e- e- synchrotron radiation from afterglow synchrotron radiation from afterglow
Smooth power-law Smooth power-law evolution of the fluxes evolution of the fluxes indicate their origin indicate their origin from afterglow from afterglow p- p-synchrotron synchrotron radiation radiation (solid) produces >100 (solid) produces >100 MeV MeV LAT data LAT data e- e-synchrotron synchrotron radiation radiation (dashed) produces XRT (dashed) produces XRT and UVOT data and UVOT data Requires ~100 times Requires ~100 times more energy in the jet more energy in the jet than in observed g rays than in observed g rays
Razzaque, arXiv:1004.3330
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Both electrons and ions are accelerated in the Forward shock Both electrons and ions are accelerated in the Forward shock
Total isotropic-equivalent jet energy : Ek,iso > Eγ,iso ≅ 1053 ergg
Constant density surrounding medium : nISM ≅ 1 cm-3
Jet deceleration time scale : tdec ≤ 1 s and Γ0 ≥ 1000
≥ Γmin (from γγ Opacity calculation)
dN d
A
k2
k1
Ion spectrum Ion spectrum Electron spectrum Electron spectrum
dN d
e
m p me
k
Crucial parameters: εB; ηA, ηe, k and k2 are fitted from data
Fraction of jet energy: εA and εe are calculated from required spectra are calculated from required spectra
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XRT light curve: XRT light curve: t t
in between ~100 s ~100 s and and 1.4 1.4 ks ks
Model with Model with e e-
synchrotron in the fast-cooling and for in the fast-cooling and for ν νXRT
XRT >
> ν νm,e
m,e >
> ν νc,e
c,e
k k = (4/3) = (4/3)α αXRT
XRT + 2/3 = 1.65 ± 0.04 ;
+ 2/3 = 1.65 ± 0.04 ; β βXRT
XRT =
= k k/2 = 0.83 /2 = 0.83 ± 0.02 ± 0.02
LAT light curve: LAT light curve: t t
in between ~0.3 s ~0.3 s and and 100 s 100 s
Model with Model with p p-
synchrotron in the slow-cooling and for in the slow-cooling and for ν νm,p
m,p
< < ν νLAT
LAT
< < ν νc,p
c,p
k
k2
2 = (4/3)
= (4/3)α αγ
γ +
+ 1 = 2.84 ± 0.09 ; 1 = 2.84 ± 0.09 ; β βγ
γ = (
= (k k2
2 - 1)/2 = 0.92 ± 0.05
β βγ
γ
needs to be compatible with measured LAT needs to be compatible with measured LAT photon index photon index (and it is) (and it is)
Parameters such as Parameters such as n nISM
ISM
and and Γ Γ0 are mainly constrained by are mainly constrained by t tdec
dec
≤ ≤ 0.3 s 0.3 s
Parameters such as Parameters such as E Ek
k, ,iso iso ,
,ε εB
B ,
,
η
ηe
e ,
,
η
ηp
p
are are set to produce required fluxes set to produce required fluxes
Parameters Parameters ε εe
e ,
,
ε
εp
p are calculated from other parameters and constrained
are calculated from other parameters and constrained <1 <1
UVOT light curve is constrained by XRT UVOT light curve is constrained by XRT ( (e e-synchrotron
)
BAT light curve can not be fitted BAT light curve can not be fitted continued central engine activity continued central engine activity
Use closure relations Use closure relations Fν ∝ ν−β t−α to determine to determine β β and and k k
k k2
2
Note: Note: e e-synchrotron
model alone cannot satisfy the closure relations
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Opacities for Opacities for γγ γγ pair production and pair production and photopion photopion production for maximum energy particles production for maximum energy particles
synchrotron photons synchrotron photons are targets for are targets for γγ γγ and and p pγ γ
maximum maximum e e-sync
. photon photon ~100 GeV ~100 GeV
maximum maximum p- p-sync sync. . photon photon >1 >1 TeV TeV
γγ
γγ pair pair production
production can only be marginally can only be marginally important important
Ground-based Ground-based detectors can probe detectors can probe p- p-synchrotron synchrotron model model
Extragalactic Background Light (EBL) limits distance of the source Extragalactic Background Light (EBL) limits distance of the source GRBs GRBs up to up to z ~ 0.5 z ~ 0.5 can be detected at can be detected at ≤ ≤ 200 GeV 200 GeV
Note that Note that Stecker Stecker et et
now disfavoured by now disfavoured by Fermi LAT data Fermi LAT data
Finke, Razzaque & Dermer 2010
Finke et al. (2010)
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The energy spectrum measured by The energy spectrum measured by Auger and Auger and HiRes HiRes
Phenomenological fits Phenomenological fits Confirm spectral cutoff Confirm spectral cutoff GZK or GZK or source feature? source feature? Nature of Primaries Nature of Primaries Debated, p or Fe? Debated, p or Fe? Galactic/extragalactic Galactic/extragalactic Where is the transition? Where is the transition? Local power output Local power output by by extragalactic sources extragalactic sources Depends on threshold Depends on threshold
ankle Auger Collaboration 2010
f ×1044 erg Mpc-3 yr-1 ; f ~1
Total non-thermal power output may be smaller if most keV - MeV emission is
thermal, and Fermi LAT is dominated by non-thermal emission
Time delay due to scattering by intergalactic magnetic field
Effectively increases the GRB rate within GZK volume by (0.2)3ΔtCR
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Back of the envelope calculation Back of the envelope calculation
Total electromagnetic energy release per GRB: 1051E51 erg Observed GRB rate ~ 2 Gpc-3 yr-1 at z ~ 1-2 ~ 0.2 Gpc-3 yr-1 at z ~ 0
beaming corrected rate ~ 100 fb times higher
γ ray power output ~ 1051E51 erg × 100 fb × 0.2 Gpc-3 yr-1 ~ 2×1043E51 fb erg Mpc-3 yr-1 Detail calculation using luminosity density function gives ~1-10 times this number
tCR 2 105Z 2BnG
2 E40EeV 2
d200Mpc
3/2
1Mpc
3/2 year
Cumulative power (> 10 Cumulative power (> 10 keV keV) output ) output from Gamma Ray Bursts from Gamma Ray Bursts
A few caveats A few caveats
Dermer & Razzaque, arXiv:1004.4249
Large baryon loading, 10-1000, seems required for GRBs to be UHECR sources
Eichler, Guetta & Pohl, arXiv:1004.4249
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Non-thermal Non-thermal (>100 (>100 MeV MeV) power output ) power output measured by Fermi LAT measured by Fermi LAT
Starburst Galaxies Starburst Galaxies Within GZK Within GZK FR I Radio Galaxies FR I Radio Galaxies Mostly within GZK Mostly within GZK FR II Radio Galaxies FR II Radio Galaxies Outside GZK Outside GZK BL BL Lacs Lacs Barely within GZK Barely within GZK Flat Spectrum Radio Flat Spectrum Radio Quasars Quasars Outside GZK Outside GZK
Dermer & Razzaque, arXiv:1004.4249
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Radio galaxies, Radio galaxies, blazars blazars
LAT HESS Swift & Suzku TANAMI
Broadband SED model of Broadband SED model of Cen Cen A A Nearest (3.7 Mpc) radio galaxy Nearest (3.7 Mpc) radio galaxy
Abdo et al. 2010, ApJ
One-zone SSC model of the SED One-zone SSC model of the SED Extract model parameters Extract model parameters Jet Doppler factor, bulk Jet Doppler factor, bulk Lorentz Lorentz factor factor Magnetic field Magnetic field, , jet power jet power Use these parameters to calculate Use these parameters to calculate maximum maximum cosmic ray energy cosmic ray energy
Emax 61020 Z
Z
B 6.2G
j 7.0
Emax 4 1019 Z
6.2G
105 s
j 7.0
Acceleration time Acceleration time = = synchrotron cooling time synchrotron cooling time Acceleration time Acceleration time = variability (dynamic) time = variability (dynamic) time
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GRBs can most easily accelerate can most easily accelerate protons protons and/or Iron and/or Iron
Powerful blazars blazars can easily can easily accelerate Iron, and proton accelerate Iron, and proton in some in some cases cases
Radio Galaxies may only accelerate Irons Irons Available (dynamic) time and/or energy losses Available (dynamic) time and/or energy losses limit acceleration limit acceleration
Dermer & Razzaque, arXiv:1004.4249
Identification of primary Identification of primary composition will help composition will help identifying sources identifying sources
He/CO star H envelope
ν ν
Buried shocks No γ-ray emission
Razzaque, Meszaros & Waxman 2003
Precursor ν’s ν ν
Internal shocks Prompt γ-ray (GRB)
Waxman & Bahcall 1997 Dermer & Atoyan 2003 Lipari et al. 2008
Burst ν’s
External shocks Afterglow X,UV,O
Waxman & Bahcall 2000 Dai & Lu 2000
Afterglow ν’s γ
CR
ν ν’s
Supernova shell GRB after SN
Razzaque, Meszaros & Waxman 2003
Supranova ν e,p γ n γ n p e
During fireball expansion No shock, n-p interact
Decoupling ν’s
Derishev et al. 1999 Bahcall & Meszaros 2000 Razzaque & Meszaros 2006
CR CR
γ γ Massive stellar core collapse scenario
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Nearby (z<0.5) bright GRBs with high variability (~1 ms) are the best bet candidates for neutrino telescopes
Razzaque, Meszaros & Waxman 2004
Neutrino flux models: Dai & Lu 2000 (afterglow wind) Razzaque, Meszaros & Waxman, PRL 2003 (supranova) Razzaque, Meszaros & Waxman, PRD 2003 (precursor) Waxman & Bahcall 2000 (afterglow ISM) Waxman & Bahcall 1997 (burst/prompt)
Projected ν events for IceCube Flux model νµ νe+ντ Precursor II (H) 4.1 1.1 Burst/prompt 3.2 0.3 Afterglow (ISM)
0.1
13 2.4
GRB 030329/SN 2003dh
Typical long duration GRB with bright SN ~1051 ergs/s luminosity at redshift z = 0.17
Neutrinos are very weakly
interacting only 10-6 probability at ~TeV energy
UHECRs need to interact
with soft photons in the GRB to make ν’s high opacity
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Fermi Fermi LAT found the nova in routine LAT found the nova in routine LAT processing for transients LAT processing for transients
Initially, counterpart was unknown Initially, counterpart was unknown
Later developments established: Later developments established:
First
First γ γ-ray detection of any nova
First clear
First clear γ γ-ray detection of
any source associated with a white source associated with a white dwarf dwarf (in binary system) (in binary system) Cheung Cheung et al et al, ATEL 2487 , ATEL 2487 Fermi Fermi LAT publication: LAT publication: Science, Science, 329 329, 817 (2010) , 817 (2010)
Nova 2010 V407 Cygni PSR J2021+4026 1FGL J2111.3+4607
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Optical nova was detected Optical nova was detected
γ γ ray emission ray emission detected later detected later in the day of optical in the day of optical detection (March 10). detection (March 10).
Lasts for 15 days
Lasts for 15 days
Peaks around day 2/3
Peaks around day 2/3
X-ray peaks ~30 d after X-ray peaks ~30 d after
γ-ray
emission.
Multiwavelength Multiwavelength emission can be emission can be understood broadly from understood broadly from the system geometry the system geometry
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θ
White Dwarf White Dwarf Red Giant Red Giant
R
Red Giant wind density from WD Red Giant wind density from WD Nova shell Nova shell
θ = 0° 30° 30° 60° 60° 90° 90° 180° 180°
1014 cm
Mwind ~ 3×10-7 Msun yr-1 vwind = 10 km s-1 Mejecta ~ 10-6 Msun vnova = 3000 km s-1
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π π±
± are also produced in
are also produced in pp pp interactions interactions
Neutrinos are produced Neutrinos are produced through decays through decays π π → →
ν + µ
ν + µ → → e e + ν + ν + ν + ν
Expected Expected ν ν fluxes of different fluxes of different flavors can be calculated flavors can be calculated using observed using observed γ γ-ray flux
10 GeV 10 GeV ν ν fluence fluence over the
transient lifetime transient lifetime ~10 ~10-4
erg ≥ ≥100 100 MeV MeV γ γ ray ray fluence fluence ~3 ~3× ×10 10-3
erg cm-2
Adopt the Adopt the π π0
0 model for
model for γ γ rays rays
γ γ ray and ray and ν ν spectra (15 day average) spectra (15 day average)
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Razzaque, Jean & Mena, arXiv:1008.5193
3500 km
L
6 3 7 1 k m
θz
Earth Earthʼ ʼs s density density profile profile
neutrino detector
ν νʼ ʼs s are created with definite flavors are created with definite flavors α α = = e, e, µ µ, , τ τ
ν νʼ ʼs s propagate with definite mass states propagate with definite mass states i i = 1, 2, 3 = 1, 2, 3
α α and and i i states are mixed while states are mixed while propagation in vacuum and in matter propagation in vacuum and in matter ( (Mikheyev-Smirnov-Wolfenstein
Mikheyev-Smirnov-Wolfenstein effect effect)
)
neutrinos are mostly affected by matter neutrinos are mostly affected by matter for normal mass hierarchy for normal mass hierarchy m m1
1/
/m m2
2 <
< m m3
3
antineutrinos are mostly affected by
antineutrinos are mostly affected by matter for inverted mass hierarchy matter for inverted mass hierarchy m m1
1/
/m m2
2
> > m m3
3
Creation and detection of Creation and detection of ν νʼ ʼs s at at separate places allow them to separate places allow them to change change their their “ “flavors flavors” ” from from creation to detection creation to detection
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ν ν flavor conversion probability flavor conversion probability in vacuum and inside the Earth in vacuum and inside the Earth Numerical calculation Numerical calculation ν ν flux at flux at a detector a detector at the at the South Pole looking South Pole looking “ “down down” ” Detail calculation depends on Detail calculation depends on
V407 Cygni Cygni direction ( direction (DEC DEC = 45.7 = 45.7o
)
ν oscillation parameters
Earthʼ ʼs density profile model s density profile model
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e.g., Razzaque & Smirnov 2010
≥ ≥10 GeV 10 GeV ν ν Detector Detector at the South Pole at the South Pole
13 13 “ “strings strings” ” at the core at the core
IceCube array array
6 strings with closely 6 strings with closely spaced (7-10 m) HQE spaced (7-10 m) HQE digital optical digital optical modules modules
allow detection of
allow detection of ν νʼ ʼs s down to ~10 GeV down to ~10 GeV
Detection volume ~10 Mt Detection volume ~10 Mt
Fully operational and Fully operational and taking data since taking data since ~31st March, 2010 ~31st March, 2010
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Hulth at ν workshop, Penn State U. 2010
Atmospheric background in ~15 days Atmospheric background in ~15 days N(νµ) + N(νµ) ~ 60 (Δθ ~ 10o) ~160 (Δθ ~ 30o)
Depends on angular resolution
Can be smaller if most ν νʼ ʼs s come w come within ithin <15 days <15 days
Neutrino-nucleon interactions Neutrino-nucleon interactions in the detector volume produce in the detector volume produce a detectable a detectable muon muon (electron and (electron and tau tau as well) as well)
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Wait for a brighter Wait for a brighter γ γ-ray nova in future!
Fermi has been producing exciting results from Fermi has been producing exciting results from GRBs GRBs
Delyaed
Delyaed onset of >100
MeV emission emission
LAT bursts are endowed with very high bulk LAT bursts are endowed with very high bulk Lorentz Lorentz factor factor
>100 >100 MeV MeV emission extends beyond emission extends beyond keV-MeV keV-MeV emission emission
We explored We explored γ γ ray emission from ray emission from UHECRs UHECRs from from GRBs GRBs
May explain >100
May explain >100 MeV MeV radiation detected with Fermi LAT radiation detected with Fermi LAT
Requires large (10-1000) baryon loading Requires large (10-1000) baryon loading
We also explored We also explored
UHECRs
Non-thermal, >100
Non-thermal, >100 MeV MeV, , γ γ-ray power output within GZK volume
from from Radio galaxies, Radio galaxies, BL BL Lacs Lacs and Starburst galaxies and Starburst galaxies exceeds exceeds total power total power
UHECRs above ankle above ankle
Total power per source
Total power per source for acceleration up to 10 for acceleration up to 1020
20
eV eV
Gamma Ray Bursts easily accelerates p and Fe Gamma Ray Bursts easily accelerates p and Fe
Most
Most blazars blazars can accelerate can accelerate p and Fe p and Fe
Radio galaxies may only accelerate Fe
Radio galaxies may only accelerate Fe
High-energy neutrinos High-energy neutrinos
May be detectable from nearby
May be detectable from nearby GRBs GRBs
Surprising sources Surprising sources such as such as γ γ-ray
Nova 2010 in V407 Cygni Cygni
CRIS 2010, CRIS 2010, Catania Catania
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