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Rays from Black Holes in X-Ray Binaries and Microquasars

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Rays from Black Holes in X-Ray Binaries and Microquasars Black Holes in the Galaxy from a high-energy astrophysics theory perspective Chuck Dermer, NRL http://heseweb.nrl.navy.mil/gamma/~dermer/default.htm Workshop on High Energy Galactic Physics 329 Pupin Hall, Columbia University May 28-29, 2010 Outline Energy from black holes γ-rays from black holes in X-ray binaries and microquasars – Leptonic jet model – Hadronic model – Colliding winds model – Synchrotron/γ-ray models Acknowledgement: γ rays from isolated black holes J. M. Paredes Galactic Center Black Hole [Ultraluminous X-ray Sources] Dermer VERITAS_NYC 28-29 May 2010 1 Cygnus Region Cyg X-1, 5.6 d Cyg X-3, 4.8 hr 11/04/2008 2 Credit: B. Cerutti Black Holes Radio loud vs. radio quiet Energy source: 2 kBT = hc / λ, λ → RS = 2GM / c 3 1. Evaporation ∴TH = hc /8πGM ∝1/ M Hawking radiation 2 4 −2 dT / dt ~ σ SB R T ∝ M 2. Accretion—Schwarzschild (1/12) vs. Kerr Low efficiency outflows, ADAFs X-ray and radio correlations for LMXBs Magnetic field prescription: B2~L/R2c Jet sources: something special? B(MG) ~ 200 l Edd / M1 /(R / Rg ) 47 2 P(erg / s) ~ 10 l Edd M 9 /(R / Rg ) 3. Rotation: Kerr Black holes, large a 2 BZ power: dE πB0 a a Blandford’s = [arctan( ) − ] conjecture (1990) dt ar+ r+ 2M Dermer & Menon (2009) 2 2 r±: ergosphere boundaries r± = M ± M − a Dermer VERITAS_NYC 28-29 May 2010 3 γ-rays from black holes in X-ray binaries and microquasars (Young) High-mass X-ray binaries (HMXBs) and (Old) Low-mass X-ray binaries (LMXBs): High and low mass refers to companion star, not compact object Accretion primarily through stellar wind (HMXB) and Roche-lobe overflow (LMXB) X-ray variability due to orbital timescale (pulsed emission rarely) Be X-ray binaries Microquasars: X-ray Binaries with Jets HMXBs thought to be γ-ray sources since COS-B and EGRET days Dermer VERITAS_NYC 28-29 May 2010 4 Observer Black Hole Jet Physics: microquasars θ Synchrotron/Compton BLR clouds Leptonic Jet Model Γ Relativistically Collimated Target photons for scattering Plasma Jet Accretion regime Accretion Ω High mass Disk Energy Sources: star BH 1. Accretion: wind, disk 2. Rotation Power Stellar Photons and Wind Γ Ambient Identifying hadronic emissions Radiation Fields Dermer VERITAS_NYC 28-29 May 2010 5 γ-ray Binaries and Candidates 3 confirmed γ-ray binaries from TeV data: – LSI +61 303. Pulsar/binary or black-hole binary/microquasar? (GeV source) – LS 5039. Pulsar/binary or black-hole binary? (GeV source) – PSR B1259-63. Pulsar/binary system. (GeV source?) Other (mostly high-mass) binaries are candidate GeV/TeV γ-ray binaries, but evidence is weaker: –Cyg X-3 (GeV source), Cyg X-1 (MAGIC source), Cen X-3, Her X-1, SS 433, A 0535+26, HESS J0632+057 A total of 280 X-ray binaries (circa 2006), including HMXBs: (131) Optical companion with spectral type O or B. Mass transfer via Be stars or via strong wind or Roche-lobe overflow. LMXBs: (149) Optical companion with spectral type later than B. Mass transfer via Roche-lobe overflow. 8 HMXBs 280 X-ray Binaries At least 15 micro- including 43 (15%) Radio 35 LMXBs quasars emitting Dermer XRBs VERITAS_NYC 28-29 May 2010 6 High Mass Microquasars Paredes (2005) P = 4.8 hr GeV/TeV Emitter LS 5039: 26 Mo O6.5V, 39000 K, 7e38 erg/s Cyg X-3: Wolf-Rayet star V1521 Cyg Cyg X-1: Blue supergiant, 31000 K, ~20-40 Mo, >40 Mo PSR 1259-63 47 ms Be X-ray binary 47 ms Be X-ray binary Porb=3.5 yr (not a microquasar) Dermer VERITAS_NYC 28-29 May 2010 7 Low Mass Microquasars Paredes (2005) Dermer VERITAS_NYC 28-29 May 2010 8 Three eccentric binaries MBH < 4 M~ or NS age < 2-3 Myr LS 5039 (HESS) LSI +61°303 (MAGIC) spectral brightening with flux 3.903 d et al. ’05 Albert et al. ‘06 Aharonian Dermer VERITAS_NYC 28-29 May 2010 9 Models for high energy γ rays from γ-ray binaries MICROQUASAR JET MODELS: Powered by accretion onto compact objet Blazar-microblazar analogy High mass stars provide wind (accretion energy) + photons (targets) Leptonic microquasar model: electrons in the jets are accelerated up to TeV energies Hadronic microquasar models Mildly relativistic outflows Confirming evidence: VHE emission from definite BHs (e.g Cyg X-1, V 4641, GRS 1915) PULSAR WIND MODEL: Powered by rotational energy of neutron star PSR B1259-63, LS 5039 & LSI +61 303 have compact objects with M < 4 Mo Time variability & X-ray spectrum of LSI +61 303 resemble those of young pulsars LS 5039, LSI have similar spectral cutoffs to pulsars LSI +61 303 is a Be star like PSR B1259-63 & all known Be/X-ray binary are NSs But does not satisfactorily fit the GeV & radio wavelength fluxes in LSI & LS 5039 Confirming evidence: Detection of pulsations in LS 5039 & LSI +61 303 ROTATING BLACK-HOLE WIND MODEL Dermer VERITAS_NYC 28-29 May 2010 10 Leptonic Microquasar Model for LS 5039 RXTE XMM Aharonian et al. (2005) Companion O7 Star (L ≅ 7×1038 ergs s-1) Optical stellar radiation strongly absorbs Leptonic Jet Model (as in blazars) TeV photons and provides a target for jet Synchrotron radio/optical/X-ray emission and electrons to be scattered to GeV energies thermal/nonthermal accretion disk and thermal Radio emission from jets reaches 10 AU stellar radiation) Compton-scattered origin of γ rays: Target photons from accretion disk and stellar radiation field Dermer VERITAS_NYC 28-29 May 2010 11 Bosch-Ramon jet model fit to LS5039 pre-Fermi Dermer VERITAS_NYC 28-29 May 2010 12 Spectral Energy Distribution + Components…(Paredes et al. 2006, A&A 451, 259). Dermer VERITAS_NYC 28-29 May 2010 13 External Compton Scattering ECS with a dominant contribution from the companion star field X-ray emitting jets (by Compton, not synchrotron): ➢ Cylindrical jet populated by relativistic particles emitting by IC processes. ➢ Injected 100 MeV e- interact via Thomson with stellar and disk photons. ➢ Applied to Cygnus X-1 and XTE J1118+480 ECS emission due to the (Georganopoulos, Aharonian & Kirk 2002, A&A 388, L25). companion star ECS emission due to the accretion disc ECS emission due to Cygnus X-1 XTE J1118+480 the accretion disc Dermer VERITAS_NYC 28-29 May 2010 14 γ Rays from Microquasars: Production and Attenuation Phase φ = 0 (High mass star Compton Scattering in KN regime for TeV γ rays closest to observer): superior – Companion Star Temperature = 39000 K = 3.4 eV conjunction Orbital Modulation of Compton Scattered radiation d – Anisotropic stellar radiation field Böttcher and Dermer (2005) γγ Attenuation (inf conj) φ = π φ = 0 (sup conj) Dermer VERITAS_NYC 28-29 May 2010 15 Spectral changes induced by γγ opacity HESS data Aharonian et al. 2006 Dubus et al. (2008) M. Böttcher (2007) Dermer VERITAS_NYC 28-29 May 2010 16 Anisotropic Compton Scattering Calculations Parameter study using broken power law electron distribution How to make GeV spectrum with break at a few GeV? Composite pulsar + shocked wind spectrum (Torres et al. 2010) Scattering effects Combined scattering and γγ + cascade calcultion Dermer VERITAS_NYC 28-29 May 2010 17 Model Fit to the Multiwavelength Spectrum of LS 5039 Microquasar jet model Fit assuming EGRET and HESS data are simultaneously measured SED EGRET emission: high- energy extension of synchrotron spectrum Combination of Compton Scattered Stellar Radiation and SSC for TeV Dermer & Böttcher 2006 Dermer VERITAS_NYC 28-29 May 2010 18 Model Fit to the Multiwavelength Spectrum of LS 5039 Fit assuming that EGRET and HESS data are different between two epochs of measurement In accord with variability expected from leptonic model Predict orbital modulation of TeV γ-rays for inner jet model Orbital modulation of GeV γ-rays for inner or extended jet model Dermer VERITAS_NYC 28-29 May 2010 19 Flow evolution calculations Scattering Calculations Dubus, Cerutti, & Henri (2008) KN Hardening effect: Dermer & Atoyan (2002) Moderski et al. (2006) Dermer VERITAS_NYC 28-29 May 2010 20 Propagation of very high energy γ-rays inside massive binaries LS 5039 and LSI +61 303 Bednarek (2006) Bednarek and Giovanelli (2007) Primary electrons and/or gamma-rays, injected at the distance z from the base of the jet, initiate an anisotropic IC e± pair cascade in the radiation field of the massive star. A part of the primary γ-rays and secondary cascade γ-rays escape from the binary system toward the observer. The cascade processes occurring inside these binary systems significantly reduce the γ-ray opacity obtained in other works by simple calculations of the escape of γ-rays The maximum in TeV γ-ray light curve predicted from the radiation fields of the massive stars by the propagation effects in LSI +61 303 should occur after periastron passage (as has been observed). Dermer VERITAS_NYC 28-29 May 2010 21 Hadronic jet models for microquasars Hadronic models (only) for gamma γ-ray emission: ➢ Conical jet 1014 eV protons interacting with strong stellar wind protons, assuming efficient wind proton diffusion inside the jet. ➢ Protons are injected in the base of the jet and evolve adiabaticaly. ➢ Applied to explain gamma-ray emission from high mass microquasars (Romero et al. 2003, A&A 410, L1). ¾ The γ-ray emission arises from the decay of neutral pions created in the inelastic collisions between relativistic protons ejected by the compact object and the ions in the stellar wind. Dermer VERITAS_NYC 28-29 May 2010 22 Model for windy high-mass stellar companion and multi-TeV protons in the jet. Spherically symmetric wind and circular orbit Romero,Torres, Kaufman, Mirabel 2003, A&A 410, L1 Secondary nuclear production (Aharonian & Atoyan 1996, Space Sci.
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