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Polarized Emission And Black Hole Shadow Image of Sagittarius A*

Polarized Emission And Black Hole Shadow Image of Sagittarius A*. Lei Huang Center for Astrophysics, USTC Institute of Astronomy & Astrophysics, Academia Sinica Collaborators: Siming Liu, Rohta Takahashi, Mike J. Cai, Zhi-Qiang Shen, Ye-Fei Yuan. Outline. 1. Radiative transfer

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Polarized Emission And Black Hole Shadow Image of Sagittarius A*

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  1. Polarized Emission And Black Hole Shadow Image of Sagittarius A* Lei Huang Center for Astrophysics, USTC Institute of Astronomy & Astrophysics, Academia Sinica Collaborators: Siming Liu, Rohta Takahashi, Mike J. Cai, Zhi-Qiang Shen, Ye-Fei Yuan. Muduleye L. HUANG @GCWorkshop2009,Shanghai

  2. Outline 1. Radiative transfer 2. Results based on accretion flow with plasma wave heating mechanism 3. Accretion Flow Structure Estimation with 1.3mm VLBI 4. Black Hole Spin Estimation with 1.3mm VLBI Muduleye L. HUANG @GCWorkshop2009,Shanghai

  3. B B 1. Radiative Transfer North North East Line of sight Muduleye L. HUANG @GCWorkshop2009,Shanghai

  4. B B 1. Radiative Transfer Rotation matrix: North North East Line of sight The four-vectors of reference coordinates (aµ , bµ ) are calculated according to the parallel transport in general relativistic theory (Chandrasekhar 1983). Muduleye L. HUANG @GCWorkshop2009,Shanghai

  5. B B 1. Radiative Transfer North North East Line of sight Muduleye L. HUANG @GCWorkshop2009,Shanghai

  6. B B 1. Radiative Transfer North RM RRM 0 North East Line of sight Muduleye L. HUANG @GCWorkshop2009,Shanghai

  7. 1. Radiative Transfer North Decomposition on LP modes East Muduleye L. HUANG @GCWorkshop2009,Shanghai

  8. 1. Radiative Transfer North Decomposition on LP modes Decomposition on CP modes East Muduleye L. HUANG @GCWorkshop2009,Shanghai

  9. 1. Radiative Transfer North Decomposition on LP modes Decomposition on CP modes Decomposition on Natural modes East where are solved from (Melrose 1997) Muduleye L. HUANG @GCWorkshop2009,Shanghai

  10. 1. Radiative Transfer Relationship between modes: Emissivity: implying Muduleye L. HUANG @GCWorkshop2009,Shanghai

  11. (Pseudo-Newtonian potential adopted, rin = 6M) 2. Results based on accretion flow with plasma wave heating mechanism Heating mechanism by turbulent plasma wave – Muduleye L. HUANG @GCWorkshop2009,Shanghai

  12. 2. Results based on accretion flow with plasma wave heating mechanism Relativistic birefringence effects Muduleye L. HUANG @GCWorkshop2009,Shanghai Huang et al. (2009)

  13. 2. Results based on accretion flow with plasma wave heating mechanism Degeneracy between Te and bp RM = n . B Smaller bp, larger RM (Flare-dominated) Muduleye L. HUANG @GCWorkshop2009,Shanghai Huang et al. (2009)

  14. Kerr Metric adopted rin=r+ 2. Results based on accretion flow with plasma wave heating mechanism Small bp leads to large RM to decrease CP in sub-mm band. Muduleye L. HUANG @GCWorkshop2009,Shanghai

  15. 3. Accretion Flow Structure Estimation with 1.3mm VLBI • H: Hawaii, including JCMT and SMA, S: SMTO, C: CARMA, L: LMT, A: Chilean, including ASTE and ALMA, P: PdBI, M: MT-COOK Muduleye L. HUANG @GCWorkshop2009,Shanghai

  16. 3. Accretion Flow Structure Estimation with 1.3mm VLBI • H: Hawaii, including JCMT and SMA, S: SMTO, C: CARMA, L: LMT, A: Chilean, including ASTE and ALMA, P: PdBI, M: MT-COOK More information comes from detections along more directions. Potential to detect valley points on baselines between Hawaii and Western U.S. Flares may happen !! Muduleye L. HUANG @GCWorkshop2009,Shanghai Compactness and symmetry of the emission region would be measured with ALMA joined. Huang, Takahashi, & Shen (2009)

  17. 4. Black Hole Spin Estimation with 1.3mm VLBI Plasma wave heating mechanism Classical RIAF Model-independent: Shadow shape; Periodicity Model-dependent Muduleye L. HUANG @GCWorkshop2009,Shanghai Huang, Takahashi, & Shen (2009), VLBI data from Doeleman et al. (2008)

  18. Summary We consider the effects of relativity and birefringence self-consistently in the radiative transfer. LP and CP observations can give constraints on orientation, mass accretion rate, and plasma bp. The structure of the accretion flow, including the central black hole shadow, can be detected by potential 1.3mm-VLBI stations. The black hole spin parameter cannot be well-estimated without imaging, or periodicity detection. Muduleye L. HUANG @GCWorkshop2009,Shanghai

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