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Transcript of Gamma-rays, neutrinos and cosmic rays from microquasars Gustavo E. Romero (IAR – CONICET & La...
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Gamma-rays, neutrinos and cosmic rays Gamma-rays, neutrinos and cosmic rays from microquasarsfrom microquasars
Gustavo E. RomeroGustavo E. Romero(IAR – CONICET & La Plata University, Argentina)(IAR – CONICET & La Plata University, Argentina)
Email: [email protected]: [email protected]
Grupo de Astrofísica Relativista y Radioastronomía (GARRA)
Trondheim, June 2009
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Microquasars
Microquasars (MQs) are accreting binaries formed by a compact object and a donor star. The compact object can be a neutron star (e.g. as in Sco X-1) or a black hole (e.g. Cygnus X-1). The donor star can be of an early type or a low-mass star.
MQs present non-thermal jets. This means that there are relativistic particles in the jets.
In the environment of a MQ the presence of relativistic particles can result in the production of detectable gamma-rays and neutrinos (e.g. Levinson & Blandford 1996, Romero et al. 2003).
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› Compact object
› Donor star
› Accretion disk
› Hot corona
› Relativistic jets
Main components of a microquasar
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Low-hardLow-hard
•
•
•
keV
keV
keV
keV
High-soft
›
›
›
Spectral states
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MQs display different X-ray spectral states:- Low/hard state (a.k.a. power-law state). Compact radio jet.- High/soft state (a.k.a. thermal-dominant state). No radio emission.- Intermediate and very high states transitions. Transient radio emission.
(Fender 2001)
MQs states and types of jets
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SS433: a precessing microquasar with heavy jetsSS433: a precessing microquasar with heavy jets
Jets with high kinetic power: Jets with high kinetic power: LLkk=10=103939erg/serg/s
Fe lines from detected from jets Fe lines from detected from jets (Migliari et al. 2002)(Migliari et al. 2002)
Jets and extended disk wind in Jets and extended disk wind in precession (precession (PPprecprec=162 d)=162 d)
Potential neutrino source (Eichler Potential neutrino source (Eichler 1980, Reynoso et al. 2008)1980, Reynoso et al. 2008)
VLBA
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Evidence for relativistic hadrons in MQ jetsEvidence for relativistic hadrons in MQ jets
Migliari et al. 2002; Kotani 1994, 1996
Migliari et al. 2002
SS433
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a cartoon…a cartoon…
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Relativistic particles in the jetsRelativistic particles in the jets
Local magnetic fieldLocal magnetic field::
Shock acceleration of electrons and protonsShock acceleration of electrons and protons
Rate:Rate:
Power in relativistic particles:Power in relativistic particles:
One-zone approximation (e.g. Khangulyan et al. 2007)One-zone approximation (e.g. Khangulyan et al. 2007)
Acceleration zoneAcceleration zone
zz00
JetJet
BHBH
andand
Injection function:Injection function: ((GeVGeV-1-1 cm cm-3-3 s s-1-1 sr sr-1-1))
LLrelrel is a fraction is a fraction qqrel rel of kinetic powerof kinetic power
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Content of relativistic particles Initial magnetic field
Simple model
Compact acceleration/emission region located where the field falls below equipartition
Mildly relativistic outflow, =1.5
Conical jet, perpendicular to binary orbit
Viewing angle =30º, moderate
Falcke & Biermann (1995)
Körding et al. (2006)
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Particle distributions “one-zone” approximation
diffusive shock acceleration
~ 2.2
(Khangulyan et al. 2007)
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Interaction of
relativistic p and e- with
magnetic field
radiation fields
in the jet
, , p e B p e
e e
( ) op p a b 2o
p p e e
• Synchrotron radiation
• Inverse Compton (IC)
• Photohadronic interactions (p)
v e ee
e B e
( ) op n a b
• Proton-proton inelastic collisions p + p p + p + a 0+ b(+ +-)
The proton microquasr jet modelThe proton microquasr jet model (Romero & Vila, A&A (Romero & Vila, A&A 485, 623 (2008), also Romero & Vila, A&A, 485, 623 (2008), also Romero & Vila, A&A, 494, L33 (2009) ) )
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Particle lossesParticle losses
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Proton escapeProton escape
Protons with energies beyond 1PeV can Protons with energies beyond 1PeV can be produced.be produced.
Main losses for protons are synchrotron Main losses for protons are synchrotron but locally produced energetic neutrons but locally produced energetic neutrons can escape:can escape:
Then, the neutrons decay outside the Then, the neutrons decay outside the region of high magnetic field injecting region of high magnetic field injecting protons, electrons and anti-neutrinosprotons, electrons and anti-neutrinos
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Case of SS 433Case of SS 433
Reynoso, Romero & Christiansen, MNRAS 387, 1747, 2008
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Romero & Vila, A&A, 494, L33 (2009)
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Magnetic field effects on neutrino productionMagnetic field effects on neutrino production
Reynoso & Romero A&A, 493, 1 (2009)
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Charged pions and muon distributionsCharged pions and muon distributions
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Magnetic field effects on neutrino productionMagnetic field effects on neutrino production
Reynoso & Romero A&A, 493, 1 (2009)
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SS 433: Differential Neutrino flux at EarthSS 433: Differential Neutrino flux at Earth
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SS 433: Integrated neutrino fluxSS 433: Integrated neutrino flux
Here, qrel= 10-3
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Gamma-ray absorption in MQsGamma-ray absorption in MQs
γγ-rays can be absorbed by:-rays can be absorbed by:
Optical depthOptical depth
Differential optical depth
Reynoso et al. APh, 28, 565 (2008)
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Gamma-ray absorption in SS433:
Absorption due to Absorption due to γγγγ interactions interactions
Target photons from the starTarget photons from the star::
Differential optical depthDifferential optical depth (Gould & Schreder 1967)(Gould & Schreder 1967)
with with TT✹✹=8500 K for SS433=8500 K for SS433 Target photons from the extended diskTarget photons from the extended disk
UV emission: Black body with UV emission: Black body with TT= 21000 K, (10= 21000 K, (103 3 Å < Å < λλ <10 <104 4 Å)Å)
RRUV UV = 33 R= 33 R ✹ ✹ (Gies et al. 2002)(Gies et al. 2002)
IR emission: , IR emission: , (2µm < (2µm < λλ <12 <12 µm)µm)
RRIRIR= 50 = 50 RR ✹ ✹ (Fuchs et al. 2005) (Fuchs et al. 2005)
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γγγγ absorptionabsorption Starlight contribution
Gamma-ray absorption in SS433:
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γγγγ absorptionabsorptionContribution due to IR emission Contribution due to IR emission Contribution due to UV emissionContribution due to UV emission
Gamma-ray absorption in SS433:
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Absorption due to Absorption due to γγN N interactionsinteractions
Optical depthOptical depth
Cross sectionCross section
Density of the star:
Density of the extended disk:
Gamma-ray absorptionabsorption in SS433:
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γN optical depthGamma-ray absorption in SS433:
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Total optical depthTotal optical depth
For For γγ-rays originated at jet base-rays originated at jet base
Gamma-ray absorption in SS433:Gamma-ray absorption in SS433:
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Effects on a gamma signalEffects on a gamma signal Gamma-ray absorption in SS433: Gamma-ray absorption in SS433:
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Integrated gamma-ray fluxes for SS 433Integrated gamma-ray fluxes for SS 433
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Positrons are copiously produced by internal Positrons are copiously produced by internal absorption and charged muon decaysabsorption and charged muon decays
INTEGRAL results (Weidenspointener et al., Nature 451, 159 (2008)
Annihilation line distribution
LMXRBs distribution
Models with a=100 produces around 1042 positrons/s
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Lepto/hadronic models for LMXRB Lepto/hadronic models for LMXRB (Vila & Romero, in preparation)(Vila & Romero, in preparation)
GX 339-4
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PAMELA positron fractionPAMELA positron fraction
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Final commentsFinal comments The consistency of the models presented can be tested with present The consistency of the models presented can be tested with present
and future neutrino and gamma-ray observations.and future neutrino and gamma-ray observations.
MQs can be sources of comic rays up to energies of the order of the MQs can be sources of comic rays up to energies of the order of the knee.knee.
MQs can also be an important source of positrons in the Galaxy MQs can also be an important source of positrons in the Galaxy A more realistic treatment is necessary to refine predictions: e.g. go A more realistic treatment is necessary to refine predictions: e.g. go
beyond the one-zone approximation.beyond the one-zone approximation.
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Thank you!Thank you!
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Parameters of the model for SS433Parameters of the model for SS433