γ rays, cosmic rays, and neutrinos
High Energy Radiation from Black Holes: γ rays, cosmic rays, and neutrinos Charles Dermer Naval Research Laboratory &
Govind Menon Troy University • Book on astrophysical radiation processes and general relativity • In review by Princeton University Press • Graduate level text/monograph • Basic tools for modeling black hole radiations • Anticipation of new generation of experiments
Outline Preliminaries 1. 2. 3. 4. 5.
Introduction Relativistic Kinematics Geometry of Spacetime Physical Cosmology Radiation Physics of Relativistic Flows
10. 11. 12. 13. 14. 15.
Processes 6. 7. 8. 9.
Compton Scattering Synchrotron Radiation Binary Particle Collision Processes Photohadronic Processes
γ-γ Pair Production Blastwave Physics Introduction to Fermi Acceleration Second-Order Fermi Acceleration First-Order Fermi Acceleration Black-Hole Electrodynamics
Systems 16. 17. 18. 19.
Black Holes in Nature Blazars GRBs Cosmic Rays
Appendix: Primer on General Relativity
Science Missions and Drivers 1. Compton Gamma-Ray Observatory: Pioneering γ-ray space observatory (1991-2000)
2. Swift Gamma-ray Burst Explorer (NASA 2004 Midex) 3. HESS (High Energy Stereoscopic System): Ground-based γray air Cherenkov telescope in Namibia since 2005
4. MAGIC/MILAGRO ground-based γ-ray telescopes 5. Very Energetic Radiation Imaging Telescope Array System (VERITAS): First light April 2007 6. AGILE: Launched April 23, 2007 7. Gamma-ray Large Area Space Telescope (GLAST): 8.
Scheduled for launch in December 2007 IceCube: NSF’s South Pole km-scale neutrino telescope. km3-yr exposure in 2009, km3-yr exposure every year in 2012
9. Auger cosmic ray experiment 10. LWA, LIGO, … 2005 – 2015: Decade of Discovery
GLAST Large Area Telescope (LAT)
GLAST Burst Monitor
(GBM)
Black Holes in Nature Primordial Mini-Black Holes (4x1018 eV)
Size Scales of Black Hole Schwarzschild radius of a black hole of mass M:
VLBI imaging capability: ≈10 µarcsec at GHz frequencies Galactic Center Black Hole Mass: ≈ 4×106 Mo At 42 GHz, ≈200 µarcsec ⇒ 24(±2) RS Not technically feasible for other black holes
SEDs; Timing
Energy Fluxes For unresolved sources, measure spectral photon flux φ(ε): photons cm-2 s-1 ε-1 Energy flux (ergs cm-2 s-1) defined in terms of luminosity L*:
Define νFν flux: ∴
ε* = (1+z)ε
Spectral Energy Distributions
Milky Way
Infrared-Luminous Galaxies
Spectral Energy Distributions
Quasars
Galaxies of Various Types
3C 279
Sub-day scale variability, well-defined flaring emissions ⇒ γ-ray emission mainly
z = 0.538
from a single zone Eddington luminosity:
L ~5x1048 x (f/10-9 ergs cm-2 s-1) ergs s-1
Mrk 421
BL Lac, z = 0.031
L ~1045 x (f/10-10 ergs cm-2 s-1) ergs s-1
Macomb et al. 1995
Blazar Main Sequence FSRQ
BL Lac Evolution from FSRQ to BL Lac Objects in terms of a reduction of fuel from surrounding gas and dust Sambruna et al. (1996); Fossati et al. (1998)
Böttcher and Dermer (2000) Cavaliere and d’Elia (2000)
Improved modeling given specific or statistical mean values of B and δD for various classes
Telescope Sensitivities
Timing Studies and Black Hole Mass Estimates Naively
Rg =
GM c∆t < c2 (1 + z )
Γ
d
1/Γ
2Γ 2ctvar d≈ (1 + z ) Variability timescale implies maximum emission region size scale, maximum engine size scale, but not emission location
M87
Rapid variability by energizing regions within the Doppler cone (e.g., external shocks)
Black Hole Statistical Studies and Size Distributions Detector threshold flux φthr
Size Distribution
statistic
Fluence distribution of 477 short and 1496 long BATSE GRBs 〈V/Vmax〉 > 0.5 (many faint sources)—more sources or brighter sources at large distances
Open Questions in Black Hole Research Origin of high energy cosmic rays Origin of γ rays from black hole jets Origin of diffuse γ-rays and neutrinos Differences between radio-loud and radio-quiet AGNs Does the Blandford-Znajek process make jets? γ rays as probes of background radiation fields (intrinsic spectrum?) Relationship of variability and black hole mass Composition and speed of black hole jets Explanation of blazar sequence
Govind Menon Troy University • Book on astrophysical radiation processes and general relativity • In review by Princeton University Press • Graduate level text/monograph • Basic tools for modeling black hole radiations • Anticipation of new generation of experiments
Outline Preliminaries 1. 2. 3. 4. 5.
Introduction Relativistic Kinematics Geometry of Spacetime Physical Cosmology Radiation Physics of Relativistic Flows
10. 11. 12. 13. 14. 15.
Processes 6. 7. 8. 9.
Compton Scattering Synchrotron Radiation Binary Particle Collision Processes Photohadronic Processes
γ-γ Pair Production Blastwave Physics Introduction to Fermi Acceleration Second-Order Fermi Acceleration First-Order Fermi Acceleration Black-Hole Electrodynamics
Systems 16. 17. 18. 19.
Black Holes in Nature Blazars GRBs Cosmic Rays
Appendix: Primer on General Relativity
Science Missions and Drivers 1. Compton Gamma-Ray Observatory: Pioneering γ-ray space observatory (1991-2000)
2. Swift Gamma-ray Burst Explorer (NASA 2004 Midex) 3. HESS (High Energy Stereoscopic System): Ground-based γray air Cherenkov telescope in Namibia since 2005
4. MAGIC/MILAGRO ground-based γ-ray telescopes 5. Very Energetic Radiation Imaging Telescope Array System (VERITAS): First light April 2007 6. AGILE: Launched April 23, 2007 7. Gamma-ray Large Area Space Telescope (GLAST): 8.
Scheduled for launch in December 2007 IceCube: NSF’s South Pole km-scale neutrino telescope. km3-yr exposure in 2009, km3-yr exposure every year in 2012
9. Auger cosmic ray experiment 10. LWA, LIGO, … 2005 – 2015: Decade of Discovery
GLAST Large Area Telescope (LAT)
GLAST Burst Monitor
(GBM)
Black Holes in Nature Primordial Mini-Black Holes (4x1018 eV)
Size Scales of Black Hole Schwarzschild radius of a black hole of mass M:
VLBI imaging capability: ≈10 µarcsec at GHz frequencies Galactic Center Black Hole Mass: ≈ 4×106 Mo At 42 GHz, ≈200 µarcsec ⇒ 24(±2) RS Not technically feasible for other black holes
SEDs; Timing
Energy Fluxes For unresolved sources, measure spectral photon flux φ(ε): photons cm-2 s-1 ε-1 Energy flux (ergs cm-2 s-1) defined in terms of luminosity L*:
Define νFν flux: ∴
ε* = (1+z)ε
Spectral Energy Distributions
Milky Way
Infrared-Luminous Galaxies
Spectral Energy Distributions
Quasars
Galaxies of Various Types
3C 279
Sub-day scale variability, well-defined flaring emissions ⇒ γ-ray emission mainly
z = 0.538
from a single zone Eddington luminosity:
L ~5x1048 x (f/10-9 ergs cm-2 s-1) ergs s-1
Mrk 421
BL Lac, z = 0.031
L ~1045 x (f/10-10 ergs cm-2 s-1) ergs s-1
Macomb et al. 1995
Blazar Main Sequence FSRQ
BL Lac Evolution from FSRQ to BL Lac Objects in terms of a reduction of fuel from surrounding gas and dust Sambruna et al. (1996); Fossati et al. (1998)
Böttcher and Dermer (2000) Cavaliere and d’Elia (2000)
Improved modeling given specific or statistical mean values of B and δD for various classes
Telescope Sensitivities
Timing Studies and Black Hole Mass Estimates Naively
Rg =
GM c∆t < c2 (1 + z )
Γ
d
1/Γ
2Γ 2ctvar d≈ (1 + z ) Variability timescale implies maximum emission region size scale, maximum engine size scale, but not emission location
M87
Rapid variability by energizing regions within the Doppler cone (e.g., external shocks)
Black Hole Statistical Studies and Size Distributions Detector threshold flux φthr
Size Distribution
statistic
Fluence distribution of 477 short and 1496 long BATSE GRBs 〈V/Vmax〉 > 0.5 (many faint sources)—more sources or brighter sources at large distances
Open Questions in Black Hole Research Origin of high energy cosmic rays Origin of γ rays from black hole jets Origin of diffuse γ-rays and neutrinos Differences between radio-loud and radio-quiet AGNs Does the Blandford-Znajek process make jets? γ rays as probes of background radiation fields (intrinsic spectrum?) Relationship of variability and black hole mass Composition and speed of black hole jets Explanation of blazar sequence
