Active Galactic Nuclei Active Galactic Nuclei AGN Nuclei
![Active Galactic Nuclei Active Galactic Nuclei](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-1.jpg)
![Active Galactic Nuclei (AGN) Nuclei of galaxies with peculiar properties: • Extremely bright nuclei Active Galactic Nuclei (AGN) Nuclei of galaxies with peculiar properties: • Extremely bright nuclei](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-2.jpg)
![AGN Variability ZW 229 -015 Variability time scales tvar of a few days. Causality AGN Variability ZW 229 -015 Variability time scales tvar of a few days. Causality](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-3.jpg)
![Emission Line Spectra ZW 229 -015 Ha Width of emission lines Dl indicates fast Emission Line Spectra ZW 229 -015 Ha Width of emission lines Dl indicates fast](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-4.jpg)
![Reverberation Mapping ZW 229 -015 (Barth et al. 2011) Reverberation Mapping ZW 229 -015 (Barth et al. 2011)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-5.jpg)
![Measuring Black Hole Masses Reverberation Mapping: To observer Dtline = (RBLR/c) (1 – cosq) Measuring Black Hole Masses Reverberation Mapping: To observer Dtline = (RBLR/c) (1 – cosq)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-6.jpg)
![Measuring Black Hole Masses The M-s Relation The stellar velocity disperion s in the Measuring Black Hole Masses The M-s Relation The stellar velocity disperion s in the](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-7.jpg)
![Cosmic Jets and Radio Lobes Gamma-Rays (Fermi) + Optical Many active galaxies show powerful Cosmic Jets and Radio Lobes Gamma-Rays (Fermi) + Optical Many active galaxies show powerful](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-8.jpg)
![Jets at all Wavelengths M 87 X-rays + Optical X-rays Optical Radio Jets at all Wavelengths M 87 X-rays + Optical X-rays Optical Radio](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-9.jpg)
![Evidence for Relativistic Beaming • Fast variability (tvar < 1 d) • High-luminosity (L Evidence for Relativistic Beaming • Fast variability (tvar < 1 d) • High-luminosity (L](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-10.jpg)
![Relativistic Beaming / Boosting In the co-moving frame of the emission region: In the Relativistic Beaming / Boosting In the co-moving frame of the emission region: In the](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-11.jpg)
![Relativistic Beaming / Boosting n. Fn Fn d d 3 n-a d 4 d Relativistic Beaming / Boosting n. Fn Fn d d 3 n-a d 4 d](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-12.jpg)
![The AGN Zoo Ellipticals Spirals Radio quiet Radio loud Seyferts Radio quiet quasars Radio The AGN Zoo Ellipticals Spirals Radio quiet Radio loud Seyferts Radio quiet quasars Radio](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-13.jpg)
![AGN Unification Seyfert 1 / Quasar Strong broad emission lines; UV/X-ray excess Seyfert 2 AGN Unification Seyfert 1 / Quasar Strong broad emission lines; UV/X-ray excess Seyfert 2](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-14.jpg)
![Types of radio-loud AGN and AGN Unification n tio c e r i d Types of radio-loud AGN and AGN Unification n tio c e r i d](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-15.jpg)
![Types of radio-loud AGN and AGN Unification Flat-Spectrum Radio Quasar or BL Lac object Types of radio-loud AGN and AGN Unification Flat-Spectrum Radio Quasar or BL Lac object](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-16.jpg)
![Blazars • Class of AGN consisting of BL Lac objects and gamma-ray bright quasars Blazars • Class of AGN consisting of BL Lac objects and gamma-ray bright quasars](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-17.jpg)
![Blazar Spectral Energy Distributions (SEDs) 3 C 66 A Non-thermal spectra with two broad Blazar Spectral Energy Distributions (SEDs) 3 C 66 A Non-thermal spectra with two broad](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-18.jpg)
![Blazar Classification 3 C 66 A (Abdo et al. 2011) (Hartman et al. 2000) Blazar Classification 3 C 66 A (Abdo et al. 2011) (Hartman et al. 2000)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-19.jpg)
![Blazar Variability: Example: The Quasar 3 C 279 X-rays Optical Radio (Bӧttcher et al. Blazar Variability: Example: The Quasar 3 C 279 X-rays Optical Radio (Bӧttcher et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-20.jpg)
![Blazar Variability: Example: The BL Lac Object 3 C 66 A (Bӧttcher et al. Blazar Variability: Example: The BL Lac Object 3 C 66 A (Bӧttcher et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-21.jpg)
![Blazar Variability: Variability of PKS 2155 -304 VHE g-rays Optical X-rays (Aharonian et al. Blazar Variability: Variability of PKS 2155 -304 VHE g-rays Optical X-rays (Aharonian et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-22.jpg)
![Multiwavelength Variability 1 ES 1959+650 (2002) (Krawczynski et al. 2004) PKS 1510 -089 (2008 Multiwavelength Variability 1 ES 1959+650 (2002) (Krawczynski et al. 2004) PKS 1510 -089 (2008](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-23.jpg)
![Polarization Variability Radio – optical polarization => Synchrotron origin Theoretical maximum polarization: Pmax = Polarization Variability Radio – optical polarization => Synchrotron origin Theoretical maximum polarization: Pmax =](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-24.jpg)
![Blazar Models Synchrotron emission Qe (g, t) Injection, acceleration of ultrarelativistic electrons n. Fn Blazar Models Synchrotron emission Qe (g, t) Injection, acceleration of ultrarelativistic electrons n. Fn](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-25.jpg)
![Proton-induced radiation mechanisms: Relativistic jet outflow with G ≈ 10 n. Fn Qe, p Proton-induced radiation mechanisms: Relativistic jet outflow with G ≈ 10 n. Fn Qe, p](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-26.jpg)
![List of Model Parameters SSC: R: Radius of the emission region G: Bulk Lorentz List of Model Parameters SSC: R: Radius of the emission region G: Bulk Lorentz](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-27.jpg)
![Constraints from Observations 1) Variability time scale tvar → Causality => R ≤ c Constraints from Observations 1) Variability time scale tvar → Causality => R ≤ c](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-28.jpg)
![Constraints from Observations 2) Superluminal Motion The MOJAVE Project (Lister et al. ) Constraints from Observations 2) Superluminal Motion The MOJAVE Project (Lister et al. )](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-29.jpg)
![Superluminal Motion The MOJAVE Project (Lister et al. ) Superluminal Motion The MOJAVE Project (Lister et al. )](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-30.jpg)
![Constraints from Observations To observer 2) Superluminal Motion: Dtobs = Dt (1 – b Constraints from Observations To observer 2) Superluminal Motion: Dtobs = Dt (1 – b](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-31.jpg)
![Constraints from Observations 3) Spectral Variability: Constraints from Observations 3) Spectral Variability:](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-32.jpg)
![Spectral Variability Spectral Time Lags Spectral Hardness-Intensity Diagrams (Takahashi et al. 1996) Spectral Variability Spectral Time Lags Spectral Hardness-Intensity Diagrams (Takahashi et al. 1996)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-33.jpg)
![Constraints from Observations 3) Spectral Variability: If energy-dependent (spectral) time lags are related to Constraints from Observations 3) Spectral Variability: If energy-dependent (spectral) time lags are related to](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-34.jpg)
![Constraints from Observations Estimates from the SED: n. Fn (C) / n. Fn (sy) Constraints from Observations Estimates from the SED: n. Fn (C) / n. Fn (sy)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-35.jpg)
![Constraints from Observations Estimates from the SED (contd. ): From synchrotron spectral index a: Constraints from Observations Estimates from the SED (contd. ): From synchrotron spectral index a:](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-36.jpg)
- Slides: 36
![Active Galactic Nuclei Active Galactic Nuclei](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-1.jpg)
Active Galactic Nuclei
![Active Galactic Nuclei AGN Nuclei of galaxies with peculiar properties Extremely bright nuclei Active Galactic Nuclei (AGN) Nuclei of galaxies with peculiar properties: • Extremely bright nuclei](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-2.jpg)
Active Galactic Nuclei (AGN) Nuclei of galaxies with peculiar properties: • Extremely bright nuclei • Variability • High-Energy (X-/g-ray) emission • Emission lines • Polarization • Relativistic outflows (jets)
![AGN Variability ZW 229 015 Variability time scales tvar of a few days Causality AGN Variability ZW 229 -015 Variability time scales tvar of a few days. Causality](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-3.jpg)
AGN Variability ZW 229 -015 Variability time scales tvar of a few days. Causality => R < c tvar ~ 2. 6 x 1015 (tvar/d) cm Luminosity of L ~ 1046 erg/s > 100 Lgalaxy produced within a region the size of our Solar System! (Barth et al. 2011)
![Emission Line Spectra ZW 229 015 Ha Width of emission lines Dl indicates fast Emission Line Spectra ZW 229 -015 Ha Width of emission lines Dl indicates fast](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-4.jpg)
Emission Line Spectra ZW 229 -015 Ha Width of emission lines Dl indicates fast orbital motion of line-emitting gas: Hb Hd Hg 2 Dl (Barth et al. 2011) Emission lines indicate the presence of a bright source of ionizing radiation vr/c = Dl/l 0
![Reverberation Mapping ZW 229 015 Barth et al 2011 Reverberation Mapping ZW 229 -015 (Barth et al. 2011)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-5.jpg)
Reverberation Mapping ZW 229 -015 (Barth et al. 2011)
![Measuring Black Hole Masses Reverberation Mapping To observer Dtline RBLRc 1 cosq Measuring Black Hole Masses Reverberation Mapping: To observer Dtline = (RBLR/c) (1 – cosq)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-6.jpg)
Measuring Black Hole Masses Reverberation Mapping: To observer Dtline = (RBLR/c) (1 – cosq) ~ R/c v. BLR ~ (Dl/l 0) c v. BLR Kepler: MBH ~ v. BLR 2 RBLR / G RBLR q Reverberation Mapping is the most reliable method to measure black-hole masses
![Measuring Black Hole Masses The Ms Relation The stellar velocity disperion s in the Measuring Black Hole Masses The M-s Relation The stellar velocity disperion s in the](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-7.jpg)
Measuring Black Hole Masses The M-s Relation The stellar velocity disperion s in the bulge of the galaxy is correlated with the mass of the central black hole: log(M/M 0) ~ 4 log(s/200 km s-1) + 8 (Gueltekin et al. 2009)
![Cosmic Jets and Radio Lobes GammaRays Fermi Optical Many active galaxies show powerful Cosmic Jets and Radio Lobes Gamma-Rays (Fermi) + Optical Many active galaxies show powerful](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-8.jpg)
Cosmic Jets and Radio Lobes Gamma-Rays (Fermi) + Optical Many active galaxies show powerful relativistic jets + Radio Example: Cen A Optical X-rays (Chandra) Optical + Radio
![Jets at all Wavelengths M 87 Xrays Optical Xrays Optical Radio Jets at all Wavelengths M 87 X-rays + Optical X-rays Optical Radio](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-9.jpg)
Jets at all Wavelengths M 87 X-rays + Optical X-rays Optical Radio
![Evidence for Relativistic Beaming Fast variability tvar 1 d Highluminosity L Evidence for Relativistic Beaming • Fast variability (tvar < 1 d) • High-luminosity (L](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-10.jpg)
Evidence for Relativistic Beaming • Fast variability (tvar < 1 d) • High-luminosity (L > 1048 erg/s) Observed in many AGN (blazars) Assuming a stationary source: • Causality => R < c tvar ~ 2. 6*1015 tvar, d cm • R must be larger than the Schwarzschild radius of whatever produces the emission => M < R c 2/(2 G) ~ 8. 7*109 tvar, d M 0 • Luminosity must be smaller than Eddington Limit: => L < 1. 1*1048 tvar, d erg/s Elliot-Shapiro Relation
![Relativistic Beaming Boosting In the comoving frame of the emission region In the Relativistic Beaming / Boosting In the co-moving frame of the emission region: In the](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-11.jpg)
Relativistic Beaming / Boosting In the co-moving frame of the emission region: In the stationary (observer’s) frame: d = (G[1 – b. Gcosq])-1: Doppler boosting factor n’ Isotropic emission I’n’ at frequency n’ G = (1 -b. G 2)-1/2 Beamed emission: In = d 3 I’n’ n = d n’ For power-law Fn ~ n-a: Fn = d(3+a) F’n Time interval t’var Time interval tvar = t’var / d
![Relativistic Beaming Boosting n Fn Fn d d 3 na d 4 d Relativistic Beaming / Boosting n. Fn Fn d d 3 n-a d 4 d](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-12.jpg)
Relativistic Beaming / Boosting n. Fn Fn d d 3 n-a d 4 d d 3+a n. Fn pk L ______ ~ 4 p d. L 2 n n L ~ d 4 L’
![The AGN Zoo Ellipticals Spirals Radio quiet Radio loud Seyferts Radio quiet quasars Radio The AGN Zoo Ellipticals Spirals Radio quiet Radio loud Seyferts Radio quiet quasars Radio](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-13.jpg)
The AGN Zoo Ellipticals Spirals Radio quiet Radio loud Seyferts Radio quiet quasars Radio spectrum Emission lines Broad and narrow Narrow Seyfert 1 Flat Steep Seyfert 2 Blazars Radio galaxies Emission lines Weak/absent Strong BL Lac Objects Steep Spectrum Radio Quasars Flat Spectrum Radio Quasars FR II
![AGN Unification Seyfert 1 Quasar Strong broad emission lines UVXray excess Seyfert 2 AGN Unification Seyfert 1 / Quasar Strong broad emission lines; UV/X-ray excess Seyfert 2](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-14.jpg)
AGN Unification Seyfert 1 / Quasar Strong broad emission lines; UV/X-ray excess Seyfert 2 Narrow emission lines; UV/X-ray weak
![Types of radioloud AGN and AGN Unification n tio c e r i d Types of radio-loud AGN and AGN Unification n tio c e r i d](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-15.jpg)
Types of radio-loud AGN and AGN Unification n tio c e r i d g in rv e s Ob Cyg A (radio) Radio Galaxy: Powerful radio lobes at the end points of the jets, where kinetic jet power is dissipated.
![Types of radioloud AGN and AGN Unification FlatSpectrum Radio Quasar or BL Lac object Types of radio-loud AGN and AGN Unification Flat-Spectrum Radio Quasar or BL Lac object](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-16.jpg)
Types of radio-loud AGN and AGN Unification Flat-Spectrum Radio Quasar or BL Lac object Emission from the jet pointing towards us is Doppler boosted compared to the jet moving in the other direction (“counter jet”). in v er bs O g n io ct re di
![Blazars Class of AGN consisting of BL Lac objects and gammaray bright quasars Blazars • Class of AGN consisting of BL Lac objects and gamma-ray bright quasars](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-17.jpg)
Blazars • Class of AGN consisting of BL Lac objects and gamma-ray bright quasars • Rapidly (often intra-day) variable • Strong gamma-ray sources • Radio jets, often with superluminal motion • Radio and optical polarization
![Blazar Spectral Energy Distributions SEDs 3 C 66 A Nonthermal spectra with two broad Blazar Spectral Energy Distributions (SEDs) 3 C 66 A Non-thermal spectra with two broad](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-18.jpg)
Blazar Spectral Energy Distributions (SEDs) 3 C 66 A Non-thermal spectra with two broad bumps: • Low-energy (probably synchrotron): radio-IR-optical(-UV-X-rays) • High-energy (X-ray – g-rays)
![Blazar Classification 3 C 66 A Abdo et al 2011 Hartman et al 2000 Blazar Classification 3 C 66 A (Abdo et al. 2011) (Hartman et al. 2000)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-19.jpg)
Blazar Classification 3 C 66 A (Abdo et al. 2011) (Hartman et al. 2000) Quasars: Low-frequency component from radio to optical/UV, nsy ≤ 1014 Hz High-frequency component from X-rays to g-rays, often dominating total power Low-frequency peaked / Intermediate BL Lacs (LBLs/IBLs): (Acciari et al. 2009) High-frequency peaked BL Lacs (HBLs): Peak frequencies at IR/Optical and Ge. V gammarays, Low-frequency component from radio to UV/X-rays, 1014 Hz < nsy ≤ 1015 Hz often dominating the total power Intermediate overall luminosity Sometimes g-ray dominated nsy > 1015 Hz High-frequency component from hard X-rays to highenergy gamma-rays
![Blazar Variability Example The Quasar 3 C 279 Xrays Optical Radio Bӧttcher et al Blazar Variability: Example: The Quasar 3 C 279 X-rays Optical Radio (Bӧttcher et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-20.jpg)
Blazar Variability: Example: The Quasar 3 C 279 X-rays Optical Radio (Bӧttcher et al. 2007)
![Blazar Variability Example The BL Lac Object 3 C 66 A Bӧttcher et al Blazar Variability: Example: The BL Lac Object 3 C 66 A (Bӧttcher et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-21.jpg)
Blazar Variability: Example: The BL Lac Object 3 C 66 A (Bӧttcher et al. 2009) Optical Variability on timescales of a few hours.
![Blazar Variability Variability of PKS 2155 304 VHE grays Optical Xrays Aharonian et al Blazar Variability: Variability of PKS 2155 -304 VHE g-rays Optical X-rays (Aharonian et al.](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-22.jpg)
Blazar Variability: Variability of PKS 2155 -304 VHE g-rays Optical X-rays (Aharonian et al. 2007) (Costamante et al. 2008) VHE g-ray and X-ray variability often closely correlated VHE g-ray variability on time scales as short as a few minutes!
![Multiwavelength Variability 1 ES 1959650 2002 Krawczynski et al 2004 PKS 1510 089 2008 Multiwavelength Variability 1 ES 1959+650 (2002) (Krawczynski et al. 2004) PKS 1510 -089 (2008](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-23.jpg)
Multiwavelength Variability 1 ES 1959+650 (2002) (Krawczynski et al. 2004) PKS 1510 -089 (2008 - 2009) (Marscher al. 2010)
![Polarization Variability Radio optical polarization Synchrotron origin Theoretical maximum polarization Pmax Polarization Variability Radio – optical polarization => Synchrotron origin Theoretical maximum polarization: Pmax =](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-24.jpg)
Polarization Variability Radio – optical polarization => Synchrotron origin Theoretical maximum polarization: Pmax = (p + 1)/(p + 7/2) For typical electron index p ~ 3: Pmax ~ 75 % Observed polarization fractions Pobs <~ 10 % << Pmax => Not perfectly ordered magnetic fields! Both degree of polarization and polarization angles vary. Swings in polarization angle sometimes associated with high -energy flares! (Abdo et al. 2010)
![Blazar Models Synchrotron emission Qe g t Injection acceleration of ultrarelativistic electrons n Fn Blazar Models Synchrotron emission Qe (g, t) Injection, acceleration of ultrarelativistic electrons n. Fn](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-25.jpg)
Blazar Models Synchrotron emission Qe (g, t) Injection, acceleration of ultrarelativistic electrons n. Fn Relativistic jet outflow with G ≈ 10 n Compton emission g 1 g 2 g Injection over finite length near the base of the jet. Additional contribution from gg absorption along the jet Leptonic Models n. Fn g-q n Seed photons: Synchrotron (SSC), Accr. Disk + BLR (EC)
![Protoninduced radiation mechanisms Relativistic jet outflow with G 10 n Fn Qe p Proton-induced radiation mechanisms: Relativistic jet outflow with G ≈ 10 n. Fn Qe, p](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-26.jpg)
Proton-induced radiation mechanisms: Relativistic jet outflow with G ≈ 10 n. Fn Qe, p (g, t) Injection, acceleration of ultrarelativistic electrons and protons Blazar Models g-q g 1 n • Proton synchrotron g 2 g • pg → pp 0 → 2 g • pg → np+ ; p+ → m+nm n. Fn Synchrotron emission of primary e- n m+ → e + n e n m Hadronic Models → secondary m-, e-synchrotron • Cascades …
![List of Model Parameters SSC R Radius of the emission region G Bulk Lorentz List of Model Parameters SSC: R: Radius of the emission region G: Bulk Lorentz](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-27.jpg)
List of Model Parameters SSC: R: Radius of the emission region G: Bulk Lorentz factor qobs: Observing angle D = (G[1 – b. Gcosq])-1: Doppler boosting factor Linj : Power injected into relativistic electrons g 1: Low-energy cutoff of injected electron spectrum g 2: High-energy cutoff of injected electron spectrum q: Power-law index of injected electron spectrum B: Magnetic field h: Particle escape time scale parameter
![Constraints from Observations 1 Variability time scale tvar Causality R c Constraints from Observations 1) Variability time scale tvar → Causality => R ≤ c](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-28.jpg)
Constraints from Observations 1) Variability time scale tvar → Causality => R ≤ c tvar d/(1 + z) → Variability time scales ~ hours => R ≤ 1015 (tvar /hr)(d/10)/(1 + z) cm
![Constraints from Observations 2 Superluminal Motion The MOJAVE Project Lister et al Constraints from Observations 2) Superluminal Motion The MOJAVE Project (Lister et al. )](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-29.jpg)
Constraints from Observations 2) Superluminal Motion The MOJAVE Project (Lister et al. )
![Superluminal Motion The MOJAVE Project Lister et al Superluminal Motion The MOJAVE Project (Lister et al. )](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-30.jpg)
Superluminal Motion The MOJAVE Project (Lister et al. )
![Constraints from Observations To observer 2 Superluminal Motion Dtobs Dt 1 b Constraints from Observations To observer 2) Superluminal Motion: Dtobs = Dt (1 – b](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-31.jpg)
Constraints from Observations To observer 2) Superluminal Motion: Dtobs = Dt (1 – b cosq) v , app = v sinq 1 – b cosq G = (1 – b 2)-1/2 b = v/c This is maximum for b = cosq => v Dt sinq max G ≥ 30 at least in some blazars! v Dt cosq b app up to ~ 30 observed Jet b , app = Gb ≈ G q v Dt
![Constraints from Observations 3 Spectral Variability Constraints from Observations 3) Spectral Variability:](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-32.jpg)
Constraints from Observations 3) Spectral Variability:
![Spectral Variability Spectral Time Lags Spectral HardnessIntensity Diagrams Takahashi et al 1996 Spectral Variability Spectral Time Lags Spectral Hardness-Intensity Diagrams (Takahashi et al. 1996)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-33.jpg)
Spectral Variability Spectral Time Lags Spectral Hardness-Intensity Diagrams (Takahashi et al. 1996)
![Constraints from Observations 3 Spectral Variability If energydependent spectral time lags are related to Constraints from Observations 3) Spectral Variability: If energy-dependent (spectral) time lags are related to](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-34.jpg)
Constraints from Observations 3) Spectral Variability: If energy-dependent (spectral) time lags are related to energy-dependent synchrotron cooling time scale: dg/dt = -n 0 g 2 with n 0 = (4/3) c s. T u’B tcool = g/|dg/dt| = 1/(n 0 g) and nsy = 3. 4*106 (B/G) (d/(1+z)) g 2 Hz => Dtcool ~ B-3/2 (d/(1+z))1/2 (n 1 -1/2 – n 2 -1/2) => Measure time lags between frequencies n 1, n 2 → estimate Magnetic field (modulo d/[1+z])!
![Constraints from Observations Estimates from the SED n Fn C n Fn sy Constraints from Observations Estimates from the SED: n. Fn (C) / n. Fn (sy)](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-35.jpg)
Constraints from Observations Estimates from the SED: n. Fn (C) / n. Fn (sy) ~ u’rad / u’B → Estimate u’rad n. Fn (C) nsy = 4. 2*106 (B/G) (D/(1+z)) gp 2 Hz → Estimate peak of electron spectrum, gp n. Fn (sy) If g-rays are from SSC: n. C/nsy = gp 2 If g-rays are from EC (BLR or IR): nsy n. C ~ G 2 eext gp 2
![Constraints from Observations Estimates from the SED contd From synchrotron spectral index a Constraints from Observations Estimates from the SED (contd. ): From synchrotron spectral index a:](https://slidetodoc.com/presentation_image_h/2bbac276467b633c663d17b5143f994a/image-36.jpg)
Constraints from Observations Estimates from the SED (contd. ): From synchrotron spectral index a: n. Fn (C) Synchrotron/Compton (Thomson) peak flux: Fn n. Fn (sy) Electron sp. Index p = 2 a + 1 -a ~n u Ne(gp) gp 2 _____ n. Fnpk ~ d 4 (4/3) c s. T 4 p d. L 2 u = u. B for synchrotron; u = urad for Thomson nsy n. C → Constrain Ne(gp) → Ne
Reverberation
Active galactic nuclei
Active galactic nuclei
Ncp for agn
Kriti mohan disease
Agn rubik's cube
Agn
Nmr active and inactive nuclei
Galactic phonics ure
Galactic habitable zone
Galactic
All three models of urban structure
Galactic cap review
Galactic headquarters map
Urban realms model
Martina cardillo
Hoyt sector model
Galactic center radio transients
Galactic habitable zone
Combine vs galactic empire
Active high and active low
Primary vs secondary active transport
Primary active transport vs secondary active transport
Nuclei di cure primarie
The multiple nuclei model
Nuc arcuatus
Preoptic area hypothalamus
Nuclei
Nuclei cocleari
Multiple nuclei model
Trunchi cerebral desen
Sanded nuclei
Nuclei proxy
Atomic nuclei
The distinct threadlike structures that contain the genetic
Cerebellum function
The multiple nuclei model