Constraining the Location of Gamma-ray Emission in Blazar Jets Manasvita Joshi, Boston University Collaborators: Alan Marscher & Svetlana Jorstad (Boston.

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Presentation transcript:

Constraining the Location of Gamma-ray Emission in Blazar Jets Manasvita Joshi, Boston University Collaborators: Alan Marscher & Svetlana Jorstad (Boston University) Markus Boettcher (Ohio University) Granada, Spain, June 12, 2013

Contact Discontinuity Internal Shock Model Joshi M. & Boettcher M., 2011, ApJ, 727, 21

Multi-zone Approach With Radiation Feedback Joshi M. & Boettcher M., 2011, ApJ, 727, 21

Gamma-ray Emission Location γ-ray flares located within sub-pc BLR or within and downstream of “core” at pc scales. Core defined as an approximately stationary, bright, compact feature seen in mm-wave (7mm or 43 GHz) VLBI images and located at one end of the jet on pc scales. Enough observational evidences (Jorstad et al., Lahteenmaki et al., Leon-Tavares et al.) of coincidences of γ-ray outbursts with radio events on pc scales. Theoretical challenge to explain variability of γ-ray flares on intra-day time scales at such length scales. Could multi-zone instead of single zone do the trick? What are sources of external seed photons & the amount of their individual contribution to gamma-ray emission?

Goal Include anisotropy in external Comptonization calculation to better constrain the location of γ-ray emission in the jet. Develop a self-consistent scheme to dynamically follow the system along the jet axis. Role of intrinsic parameters. Interplay of various radiative processes responsible for different spectral states.

Methodology Radiation transfer code of Joshi & Böttcher (2011) with multi-zone feedback scheme. Include the contribution from accretion disk (ECD), broad line region (BLR; ECC), and dusty torus (ECDT). Evolve the system & follow the emission region to beyond BLR. Joshi, Marscher & Boettcher (2013, in prep.)

Disk + BLR + DT Schematic

BH R in z R out Accretion Disk Disk Schematic: Shakura- Sunyaev R in = 1.92e14 cm R out = 1.78e17 cm ε * Disk - optical to 10 keV Relevant Parameters:

BLR Schematic z Pos. 1 Pos. 2 Pos. 3 Jet Central Engine BLR Clouds Donea & Protheroe (2003); Liu & Bai (2006) R in R out los s r ε * BLR - IR to 3 keV Relevant Parameters:

Joshi, Marscher & Boettcher (2013, in prep.)

z Dust Torus Schematic R in R out RTRT r DT T * DT = 1200 K Relevant Parameters:

Flat Spectrum Radio Quasar (FSRQ)

EC BLR EC DT

Summary & Next Steps High energy emission significant from within BLR for this case of FSRQ. Anisotropy important for disk, BLR & DT contribution. Understanding of source(s) of seed photons:  Are there only 3 conventional sources?  Could stratification of BLR with various ionization lines originating from different distance resulting in larger size and location of BLR (Stern & Poutanen, 2011) do the trick?  Could single emission line cloud along the line of sight of emission region located further out in the jet be responsible?  Do we need to get creative with sources of seed photons at pc scales?

contd…. Careful with generalization of location of γ -ray emission. Apply the external Compton model to understand its effect on evolution of e - energy dist. and resulting SED of blazars.

Parameter Study