Upgrade to Pro — share decks privately, control downloads, hide ads and more …

Active Galactic Nuclei: Laboratory for Gravitational Physics

Active Galactic Nuclei: Laboratory for Gravitational Physics

Talk presented at the 29th Midwest Relativity Meeting, Grand Valley State University, Grand Rapids, MI, USA, October 2019

Ashkbiz Danehkar

October 04, 2019
Tweet

More Decks by Ashkbiz Danehkar

Other Decks in Science

Transcript

  1. Active Galactic Nuclei
    Laboratory for Gravitational Physics
    Image Credit: NASA/JPL-Caltech
    Image Credit: NASA/JPL-Caltech
    Ashkbiz Danehkar
    Department of Astronomy, University of Michigan
    [email protected]
    The 29th Midwest Relativity Meeting, Grand Rapids, Michigan, USA, October 4th, 2019

    View Slide

  2. 10/04/2019 Midwest Relativity Meeting
    2
    Gravity Timeline
    1687: Newtonian gravity
    1915: General Relativity
    1960-1975: golden age of GR
    (Kip Throne 1995)
    – Cambridge (Sciama’s group)
    – Hamburg GR group (Jordan)
    – Potsdam AEI (Ehlers’ group)
    – Syracuse (Bergmann’s grp)
    – UT Austin (Schild’s group)
    – ...
    local interaction (Einstein field equations)
    non-local long-range interaction (Binanchi identities)
    Trumper 1964, Hawking 1966, Ellis 1971

    View Slide

  3. 10/04/2019 Midwest Relativity Meeting
    3
    Gravity Timeline
    1992-present: golden age of cosmology
    (Alan Guth 2001)
    2019: EHT imaging of SMBH in M87
    2016: LIGO detection of gravitational waves

    (Weiss+Throne+Barich 2017)
    1995: acceleration expansion of the universe
    (Perlmutter+Schmidt+Riess 2011)
    1974: Test of GR in a binary pulsar (Hulse+Taylor 1993)

    View Slide

  4. 10/04/2019 Midwest Relativity Meeting
    4
    Active Galactic Nuclei (AGN)
    2019: EHT imaging of SMBH in M87
    First Image of a Supermassive Black Hole
    Credit: Science History Images / Alamy Stock Photo

    View Slide

  5. 10/04/2019 Midwest Relativity Meeting
    5
    Active Galactic Nuclei (AGN)
    X-ray Observations of AGN (1999-present)
    Chandra X-ray Observatory (1999-present)
    XMM-Newton, X-ray Multi-Mirror Mission (2000-present)
    NuSTAR, Nuclear Spectroscopic Telescope Array (2012-present)
    Gierlinski + 1999
    Lonanov 2007
    Credit: Roen Kelly @ Astronomy

    View Slide

  6. 10/04/2019 Midwest Relativity Meeting
    6
    Active Galactic Nuclei (AGN)
    AGN Unified Model (radio-loud & -quiet AGN, Seyfert I & II Galaxies)
    Beckmann & Shrader 2012,
    Active Galactic Nuclei
    Unified Models for AFNs
    Antonucci, ARA&A, 1993, 31, 473
    Unified Schemes for AGNs
    Megan Urry & Padovani, 1995, PASP, 107,
    803
    (Bernie Fanaroff &
    Julia Riley 1974)
    AGN Unified Model
    • Radio-Quiet AGN
     Seyfert I (BLR+NLR,
    compact outflows)
     Seyfert II (NLR)
    • Radio-Loud AGN
     FR I (compact radio jets)
     FR II (extended radio jets)
     Blazar (relativistic beams)
    (Carl Seyfert 1942)

    View Slide

  7. 10/04/2019 Midwest Relativity Meeting
    7
    Active Galactic Nuclei (AGN)
    Dermer & Giebles 2016
    AGN Classification (radio-loud & -quiet AGN, Seyfert I & II Galaxies)
    Blandford, Netzer, Woltjer 1990, Active Galactic Nuclei

    View Slide

  8. 10/04/2019 Midwest Relativity Meeting
    8
    Ultra-fast Outflow in AGN
    Detection of relativistic outflows in X-ray

    Seyfert I PG 1211+143
    Ionized outflow at -0.06c and -0.11 c
    Danehkar + 2018
    Pounds + 2003,2006,2009
    Ionized outflow at -0.06c

    View Slide

  9. 10/04/2019 Midwest Relativity Meeting
    9
    Ultra-fast Outflow in AGN
    Detection of relativistic outflows in X-ray

    Seyfert I PDS 456
    Ionized outflow at -0.24c and -0.48 c
    Biossay-Malaquin, Danehkar + 2019

    View Slide

  10. 10/04/2019 Midwest Relativity Meeting
    10
    Ultra-fast Outflow in AGN
    Detection of relativistic outflows in X-ray
    Cappi 2006

    View Slide

  11. 10/04/2019 Midwest Relativity Meeting
    11
    Ultra-fast Outflow in AGN
    Correlation between outflow kinematics and physical conditions
    Tombesi + 2013
    (Ultra-fast outflows)
    (Warm Absorbers)

    View Slide

  12. 10/04/2019 Midwest Relativity Meeting
    12
    Ultra-fast Outflow in AGN
    X-ray Ionized Outflows in AGN
    Ionization parameter
    Gas density
    Radius
    Column
    density Shell thickness
    Outflow
    velocity
    Luminosity (0.0136-
    13.6 keV)
    King & Pounds 2015; XMM-Newton & Suzaku
    (42 radio-quiet, Tombesi et al 2011; 51 AGN, Gofford et al. 2013)
    BH
    mass

    View Slide

  13. 10/04/2019 Midwest Relativity Meeting
    13
    Ultra-fast Outflow in AGN
    Theories for Relativistic Outflows in AGN

    strong magnetic field in accretion flow/disk
    of rotating BH
    – Blandford-Znajek process (1977) for strong jets from flow
    – Blandford-Payne process (1982) for slow winds from disk

    frame dragging (gravitomagnetism indirectly)
    – Penrose process (1971)
    – Kerr spacetime of rotating BH
    – extracting black-hole rotational energy

    frame dragging + magnetic field
    (e.g. Narayan & Quataert 2005)

    gravitomagnetism (directly)?
    Frame dragging+magnetic
    (Narayan & Quataert 2005)
    Blandford-Znajek process
    (Thorne 1995)

    View Slide

  14. 10/04/2019 Midwest Relativity Meeting
    14
    Supermassive Black Hole Spin
    Black Hole Spin Measurement (see Brenneman 2013)

    Thermal Continuum Fitting (UV observation)
    – stellar-mass black hole
    – AGN (may problematic due to UV absorption lines!)

    Inner Disk Reflection Modeling
    – AGN (X-ray)

    High Frequency Quasi-Periodic Oscillations
    – AGN + stellar-mass black hole (fully not developed)

    X-ray Polarimetry
    – Need sensitive X-ray polarimter (not available now!)

    Imaging the Event Horizon Shadow
    – Need Very Long Baseline Interferometry (in development)
    – Suitable only for Sgr A* and M87
    a = J c / G M2
    (a: BH spin, J: angular momentum, M: BH mass, G: gravitational constant, c: speed of light)

    View Slide

  15. 10/04/2019 Midwest Relativity Meeting
    15
    Supermassive Black Hole Spin
    Relativistically broadened Kα iron line (6.4 keV)
    Compton hump (> 10keV)
    Black Hole Spin Measurement from X-ray
    a = - 1
    a = 0
    a = 1
    Image credit: NASA/JPL-Caltech

    View Slide

  16. 10/04/2019 Midwest Relativity Meeting
    16
    Supermassive Black Hole Spin
    BH Spin from Reflection Modeling

    kerrconv (Brenneman & Reynold 2006)

    relline (Dauser + 2010)

    xillver (Garcia + 2010,11,13)

    relxill (Garcia + 2014)
    Dauser & Garcia + 2014

    View Slide

  17. 10/04/2019 Midwest Relativity Meeting
    17
    Supermassive Black Hole Mass
    BH Mass from Reverberation Mapping Technique (Kaspi + 2000)

    Variation in light curves of broad emission line region (BLR) in Seyfert I AGN

    Time delay in variation of BLR luminosity (Hb 4861A) relative to
    variation of accretion disk luminosity (continuum 5100A)
    www.techfreaq.de
    Bentz + 2006

    View Slide

  18. 10/04/2019 Midwest Relativity Meeting
    18
    SMBH Spin Implication
    Black Hole Spin Implication for a Unified AGN Model?
    Garofalo + 2010
    Beckmann & Shrader 2012,
    Active Galactic Nuclei
    AGN Unified Model
    - Radio-Quiet AGN: Seyfert I, Seyfert II
    - Radio-Loud AGN: FR I, FR II (extended radio jets)

    View Slide

  19. 10/04/2019 Midwest Relativity Meeting
    19
    SMBH Spin Implication
    Black Hole Spin Implication for a Unified AGN Model?
    Danehkar +

    View Slide

  20. 10/04/2019 Midwest Relativity Meeting
    20
    Future Direction for X-ray Astronomy

    XRISM, X-Ray Imaging and Spectroscopy Mission (2022)
    – Japan Aerospace Exploration Agency (JAXA)
    – Replacement for Hitomi, ASTRO-H (2016, failed)

    ATHENA, Advanced Telescope for High Energy Astrophysics (2031)
    – European Space Agency (ESA)

    Lynx X-ray Observatory (proposed 2035)
    – National Aeronautics and Space Administration (NASA)

    Arcus X-ray observatory (proposed 2023)
    – NASA

    View Slide

  21. 10/04/2019 Midwest Relativity Meeting
    21
    Proposed Direction for Numerical GR

    Finite-difference Time-domain (FDTD; 1980)

    Discontinuous Time-domain Method (FETD; 2000)

    Finite Element Method (FEM; 1973)

    Finite Integration Technique (FIT, 1977)

    ….
    ?
    For Maxwell EM equations, there are several numerical methods:
    For Einstein field equations (local gravitational interaction), there are several
    numerical methods (see review by Font 2003 for numerical GR; Fornt 2008 for
    GR+MHD)
    For example, for Bianchi dynamical formulas of non-local (Weyl) gravitational fields:
    Newtonian Tidal force
    Non-Newtonian effect
    Gravitational waves
    shear induction?
    computational
    hydrodynamics simulation
    not fully developed
    angular momentum

    Finite Difference Method (FDM; 1988)

    Smoothed Particle Hydrodynamics (SPH; 1977)

    Spectral Methods (1988)

    Flow Field-dependent Variation Method (FDV; 2002)

    ….
    One of reference books for mathematics of Weyl fields

    View Slide

  22. 10/04/2019 Midwest Relativity Meeting
    22
    Summary
    Implication of Supermassive Black Hole Angular Momentum for AGN Outflows?

    Relativistic Outflows in AGN measured from
    – blue-shifted highly-ionized absorption lines in X-ray spectra

    AGN Outflow Physical conditions from
    – photo-ionization modeling of absorbers

    Black Hole Spin measured from
    – relativistic Fe Kα line (6.4 keV)
    – Compton hump (> 10keV)

    Black Hole Mass measured from
    – time delay in BLR vs. disk light curves in
    Seyfert I AGN (Reverberation-mapping)

    Physical Mechanism behind
    relativistic outflows in AGN?
    – Need for larger sample and
    future X-ray observations (XRISM 2022, ATHENA 2031, Lynx 2035)
    – Future developments in numerical methods & simulations of GR hydrodynamics
    Credit: Roen Kelly @ Astronomy

    View Slide

  23. Image Credit: NASA/JPL-Caltech
    Image Credit: NASA/JPL-Caltech
    Thank you for your attention
    Thank you for your attention

    View Slide