Acceleration of highest energy cosmic rays in jets of powerful AGNs
High-Energy Cosmic Particles by Black-hole Jets in Galaxy ...crphys2020/slide/S6_Fang.pdf · with...
Transcript of High-Energy Cosmic Particles by Black-hole Jets in Galaxy ...crphys2020/slide/S6_Fang.pdf · with...
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High-Energy Cosmic Particles by Black-hole Jets in Galaxy Clusters
Ke Fang Einstein Fellow, Stanford University
YITP Workshop, Kyoto, Japan (virtual attendance) Dec 10, 2020
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• A “common origin” of cosmic particles?
• Cosmic-ray acceleration and confinement
• Astroparticles from galaxy clusters
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• A “common origin” of cosmic particles?
• Cosmic-ray acceleration and confinement
• Astroparticles from galaxy clusters
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UHECRs, High-energy Neutrinos & Gamma Rays
Ultrahigh Energy Cosmic Ray (UHECR)
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Ultrahigh Energy Cosmic Ray (UHECR)
Telescope Array, ICRC (2015)
UHECRs, High-energy Neutrinos & Gamma Rays
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Light component in the transition
regimeKASCADE, LOFAR,
IceTop
KASCADE-Grande (ICRC 2017)
UHECRs, High-energy Neutrinos & Gamma Rays
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TeV - PeV: Detected by IceCube since 2013
UHECRs, High-energy Neutrinos & Gamma Rays
1010 1012 1014 1016 1018 1020
Emax [eV]
1042
1043
1044
1045
1046
1047
E opt[e
rgM
pc°
3yr
°1 ]
novae
SLSNe-I
SLSNe-II
SN-IIn
CCSNeTDE
FBOT
Luminous FBOTIa-CSM
≤rel <1%
≤rel <100%
E∫ > 100 TeV
IceCube DiÆuse Neutrinos
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Neutrino Sources are Powerful and Abundant!
KF, Metzger, Vurm, Aydi, Chomiuk (2020)
Transients powered by non-relativistic shocks can barely explain the IceCube diffuse neutrinos.
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~14% of the Fermi extragalactic gamma-ray background is contributed by unknown sources. Fermi Collabora,on (2016)
Lisan, et al (2016)
UHECRs, High-energy Neutrino & Gamma Rays
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When putting them together..
Despite ten orders of magnitudes difference in energy, UHECRs, IceCube neutrinos, Fermi non-blazar EGB share similar energy injection rate.
Murase, Ahlers & Lacki (2013), Waxman 1312.0558, Giacin, et al (2015), Murase & Waxman (2016), Wang & Loeb (2017) …
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A common origin is nontrivialThe sources need to provide the right
interaction probability
Truncation / hard spectrum below ~TeV
[e.g., Murase, Guetta & Ahlers, (2016), Bechtol+ (2017)] Neutrinos above 10 PeV?
[IceCube Coll. (2018)]
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• A “common origin” of cosmic particles?
• Cosmic-ray acceleration and confinement
• Astroparticles from galaxy clusters
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• “Mini AGN” in our own galaxy with extended X-ray jets
Black Hole Jets as Cosmic Accelerators Microquasar SS 433
ROSAT 0.2 keVHAWC ~20 TeV
• TeV gamma-rays in both lobes detected by HAWC
HAWC Collaboration, Nature (2018)KF as a main author
• GeV counterparts identified in Fermi-LAT data
KF, Charles, Blandford, ApJL (2020)
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HAWC Collaboration, Nature (2018)KF as a main author
KF, Charles, Blandford, ApJL (2020)
ROSAT 0.2 keVHAWC ~20 TeV
• Electrons above 20 TeV were accelerated
• Particle acceleration sites ~30 pc away from hole
E ⇠ Z 1019✓
B
1µG
◆✓R
10 kpc
◆eV
Scaling to jets of supermassive black holes:
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Confinement of Cosmic Rays in Local Environment Cygnus Cocoon
GeV to100 TeV gamma-rays trace infrared emission
HAWC Collaboration, under reviewKF as a main author
Fermi-LAT Coll., Science (2011)
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• A “common origin” of cosmic particles?
• Cosmic-ray acceleration and confinement
• Astroparticles from galaxy clusters
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nICM(r) = nICM,0
"1 +
✓r
rc
◆2#�3�/2ICM gas
Radiation backgrounds: Infrared background from galaxies, CMB, Extragalactic background lights
Magnetic field following Kolmogorov turbulence
The Intracluster Medium Environment for Interactions
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KF & Olinto (2017)KF & Murase Nature Physics (2018)
Strength of magnetic field in the core of a galaxy cluster
CRPropa3 + SOPHIA for turbulent field & [Ba,sta+ JCAP (2016)]
EPOS for [KF, Kotera & Olinto ApJ (2012)]
Diffuse propaga@on [Kotera & Lemoine PRD (2007), KF & Olinto ApJ (2016)]
N�
Np
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Dtotal = 46Mpc
Bc = 10µG,M = 1015 M�
Particle Larmor RadiusrL = 10E19 B
�1�6 Z
�1 kpc
Field Correlation Length
l0 ⇠ 20 kpc
Particle Trajectory in the Intracluster Medium - 10 EeV
KF & Murase Nature Physics (2018)
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Bc = 10µG,M = 1015 M�
Particle Larmor Radius
rL = 0.1E17 B�1�6 Z
�1 kpc<latexit sha1_base64="1IkbeNwFzqpHyLOWl7Av/sV7vi0=">AAACGXicbVDLSgMxFM34rPU16tJNsAgu2jIRsW6EqgguXFSwD+yMQyZN29DMgyQjlGF+w42/4saFIi515d+YtrPQ1gMhJ+fcy809XsSZVJb1bczNLywuLedW8qtr6xub5tZ2Q4axILROQh6Klocl5SygdcUUp61IUOx7nDa9wcXIbz5QIVkY3KphRB0f9wLWZQQrLbmmJdxreAqtMoJ28dJNUCW1i+duUjpO75MS0o+77LaFDwcRcc2CVbbGgLMEZaQAMtRc89PuhCT2aaAIx1K2kRUpJ8FCMcJpmrdjSSNMBrhH25oG2KfSScabpXBfKx3YDYU+gYJj9XdHgn0ph76nK32s+nLaG4n/ee1YdU+chAVRrGhAJoO6MYcqhKOYYIcJShQfaoKJYPqvkPSxwETpMPM6BDS98ixpHJaRDvbmqFA9y+LIgV2wBw4AAhVQBVegBuqAgEfwDF7Bm/FkvBjvxsekdM7IenbAHxhfPyEfnU4=</latexit><latexit sha1_base64="1IkbeNwFzqpHyLOWl7Av/sV7vi0=">AAACGXicbVDLSgMxFM34rPU16tJNsAgu2jIRsW6EqgguXFSwD+yMQyZN29DMgyQjlGF+w42/4saFIi515d+YtrPQ1gMhJ+fcy809XsSZVJb1bczNLywuLedW8qtr6xub5tZ2Q4axILROQh6Klocl5SygdcUUp61IUOx7nDa9wcXIbz5QIVkY3KphRB0f9wLWZQQrLbmmJdxreAqtMoJ28dJNUCW1i+duUjpO75MS0o+77LaFDwcRcc2CVbbGgLMEZaQAMtRc89PuhCT2aaAIx1K2kRUpJ8FCMcJpmrdjSSNMBrhH25oG2KfSScabpXBfKx3YDYU+gYJj9XdHgn0ph76nK32s+nLaG4n/ee1YdU+chAVRrGhAJoO6MYcqhKOYYIcJShQfaoKJYPqvkPSxwETpMPM6BDS98ixpHJaRDvbmqFA9y+LIgV2wBw4AAhVQBVegBuqAgEfwDF7Bm/FkvBjvxsekdM7IenbAHxhfPyEfnU4=</latexit><latexit sha1_base64="1IkbeNwFzqpHyLOWl7Av/sV7vi0=">AAACGXicbVDLSgMxFM34rPU16tJNsAgu2jIRsW6EqgguXFSwD+yMQyZN29DMgyQjlGF+w42/4saFIi515d+YtrPQ1gMhJ+fcy809XsSZVJb1bczNLywuLedW8qtr6xub5tZ2Q4axILROQh6Klocl5SygdcUUp61IUOx7nDa9wcXIbz5QIVkY3KphRB0f9wLWZQQrLbmmJdxreAqtMoJ28dJNUCW1i+duUjpO75MS0o+77LaFDwcRcc2CVbbGgLMEZaQAMtRc89PuhCT2aaAIx1K2kRUpJ8FCMcJpmrdjSSNMBrhH25oG2KfSScabpXBfKx3YDYU+gYJj9XdHgn0ph76nK32s+nLaG4n/ee1YdU+chAVRrGhAJoO6MYcqhKOYYIcJShQfaoKJYPqvkPSxwETpMPM6BDS98ixpHJaRDvbmqFA9y+LIgV2wBw4AAhVQBVegBuqAgEfwDF7Bm/FkvBjvxsekdM7IenbAHxhfPyEfnU4=</latexit><latexit sha1_base64="1IkbeNwFzqpHyLOWl7Av/sV7vi0=">AAACGXicbVDLSgMxFM34rPU16tJNsAgu2jIRsW6EqgguXFSwD+yMQyZN29DMgyQjlGF+w42/4saFIi515d+YtrPQ1gMhJ+fcy809XsSZVJb1bczNLywuLedW8qtr6xub5tZ2Q4axILROQh6Klocl5SygdcUUp61IUOx7nDa9wcXIbz5QIVkY3KphRB0f9wLWZQQrLbmmJdxreAqtMoJ28dJNUCW1i+duUjpO75MS0o+77LaFDwcRcc2CVbbGgLMEZaQAMtRc89PuhCT2aaAIx1K2kRUpJ8FCMcJpmrdjSSNMBrhH25oG2KfSScabpXBfKx3YDYU+gYJj9XdHgn0ph76nK32s+nLaG4n/ee1YdU+chAVRrGhAJoO6MYcqhKOYYIcJShQfaoKJYPqvkPSxwETpMPM6BDS98ixpHJaRDvbmqFA9y+LIgV2wBw4AAhVQBVegBuqAgEfwDF7Bm/FkvBjvxsekdM7IenbAHxhfPyEfnU4=</latexit>
Field Correlation Length
l0 ⇠ 20 kpc
KF & Murase Nature Physics (2018)Dtotal ⇠ tcluster
Particle Trajectory in the Intracluster Medium - 0.1 EeV
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Bddvnvmbujpo!bu!mpx!F
Tpgufs!tqfdusvn!evf!up!DS!ftdbqf
Bc = 10µG,M = 1015 M�
Neutrino Spectrum from One Cluster
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Injection Composition = Galactic CR abundance
IceCube (>100 TeV)
UHECRs
Non-blazar Extragalactic Gamma-ray Background
Cosmic Particles from Black Hole Jets in Galaxy ClustersKF & Murase Nature Physics (2018)
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Fits to UHECR data
KF & Murase (2018)
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Accretion Shocks around Galaxy Cluster
Due to low baryon density at the outskirts of clusters, particle interaction near accretion shocks is too weak to explain observed high-energy neutrinos.
KF & Olinto (2017)
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• Sources of high-energy neutrinos and ultrahigh energy cosmic rays are abundant and powerful
• Cosmic-ray acceleration and confinement commonly exist in astrophysical environments
• A “common origin” of cosmic particles may be explained by black hole jets in galaxy clusters
Conclusion
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• What’s your targeted physics in next decade? Sources of high-energy neutrinos High-energy messengers (gamma rays and neutrinos) from transients such as TDEs, binary mergers
• What we need to accomplish? Design and planning of next-generation astroparticle experiments Data analysis infrastructures that enable collaboration of different experiments
Conclusion
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Cosmic Ray Production by the Jet
Cosmic rays that are confined by the radio lobes cool adiabatically
*taking a typical lobe size 10 kpc, coherence length 0.3 kpc, magnetic field strength 5 muG, and expansion velocity 2000 km/s.
Only particles above ~PeV leave the source
*tlobedi↵ ⇠ 6.1
✓E/Z
1PeV
◆�1/3
Myr
tcool ⇠ 5Myr
E ⇠ Z 1019✓
B
1µG
◆✓R
10 kpc
◆eV
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Neutrino Sources are Powerful and Abundant!
KF, Metzger, Vurm, Aydi, Chomiuk (2020)
Transients powered by non-relativistic shocks can barely explain the IceCube diffuse neutrinos.
106 107 108 109 1010
vsh [cm s°1]
104
105
106
107
A/A
§
Lsh = 1036 1040 1044
tpk = 3
tpk = 30
tpk = 300
Emax = 1012 1014 1016
radiative adiabatic
tcool = tpk tpp = tpk
novae
LRN
SLSNe-ISLSNe-II
SN-IIn
CCSNe
TDE
FBOT
Luminous FBOT
Ia-CSM
1010 1012 1014 1016 1018 1020
Emax [eV]
1042
1043
1044
1045
1046
1047
E opt[e
rgM
pc°
3yr
°1 ]
novae
SLSNe-I
SLSNe-II
SN-IIn
CCSNeTDE
FBOT
Luminous FBOTIa-CSM
≤rel <1%
≤rel <100%
E∫ > 100 TeV