PROPERTIES, DYNAMICS, & SPECTRAL SIGNATURES OF CLOUDS IN AGN TIM WATERS PHD CANDIDATE UNLV (ADVISOR: DANIEL PROGA)

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1 PROPERTIES, DYNAMICS, & SPECTRAL SIGNATURES OF CLOUDS IN AGN TIM WATERS PHD CANDIDATE UNLV (ADVISOR: DANIEL PROGA) Figure credit: Active Galactic Nuclei, Wiley 2012

2 COMMON VIEW LOCAL SIMULATIONS Property Single cloud Global distribution Single cloud Global distribution Equilibrium Static vs. evolving Confined vs. state vs. evaporating outflowing Formation/ Thermal instability orbiting blobs vs. Regeneration vs. blobs uplifted from the disk condensing clumps (bloated star winds?) Velocity Unconstrained -10^4-10^4 km/s Density/ Temperature Constant Wide range (e.g., LOC model) Requires global simulations: Size Wide range Sub parsec to parsec Number 1 10^3-10^7 Shape Motion Emission/ Absorption Blobs, shells, Directed stream vs. slabs, filaments? failed wind vs. mist Keplerian orbit vs. Swarm vs. embedded in wind clumpy outflow Optically Self-shielding is thick vs. thin important?

3 Intercloud medium Cloud core Conductive interface e- e- e- Classical evaporation: tau_evap (Cowie & McKee 1977) Steady state configuration: line cooling balances conductive heating Begelman & McKee (1990)

4 CLOUD DYNAMICS: ACCELERATION, EVAPORATION, AND REGENERATION (SPITZER CONDUCTIVITY T^5/2) To view animation please visit

5 CLOUD FORMATION AND ACCELERATION DYNAMICS OF THE NONLINEAR REGIME OF TI See Proga & Waters (2015)

6 TI: THE NONLINEAR REGIME Saturation of TI is a cloud formation process, but it also naturally leads to cloud acceleration (PW15). Xrays UV

7 TI: THE NONLINEAR REGIME Saturation of TI is a cloud formation process, but it also naturally leads to cloud acceleration (PW15). Xrays UV

8 TI: THE NONLINEAR REGIME Saturation of TI is a cloud formation process, but it also naturally leads to cloud acceleration (PW15). v Xrays UV

9 COMMON VIEW LOCAL SIMULATIONS Property Single cloud Global distribution Single cloud Global distribution Equilibrium Static vs. evolving Confined vs. Accelerating state vs. evaporating outflowing clumpy flow Outflowing Formation/ Thermal instability orbiting blobs vs. Regeneration vs. blobs uplifted condensing clumps from the disk (bloated star winds?) Velocity Unconstrained -10^4-10^4 km/s Density/ Temperature Constant Wide range (e.g., LOC model) TI naturally leads to cloud regeneration v_flow + a*t Requires global simulations: Condensing clumps ~v_flow Size Wide range Sub parsec to parsec Number 1 10^3-10^7 Shape Motion Emission/ Absorption Blobs, shells, Directed stream vs. slabs, filaments? failed wind vs. mist Keplerian orbit vs. Swarm vs. embedded in wind clumpy outflow Optically Self-shielding is thick vs. thin important? lambda of max growth rate? 1 becomes many Clumpy medium

10 LOCAL OPTIMALLY EMITTING CLOUD PICTURE (LOC MODEL) From Baldwin et al. (1995) LUMINOUS ORBITING COVFEFE

11 CLOUD DENSITIES ARE CONSTRAINED TO RANGES DICTATED BY THE SED (AND CORRESPONDING S-CURVE) To view animation please visit

12 SINGLE ZONE!= SINGLE CLOUD

13 CLUMPS RESPOND TO IONIZING FLUX VARIABILITY shown here: 20% case To view animation please visit

14 CLUMPS RESPOND TO IONIZING FLUX VARIABILITY With (left) and without (right) 20% variability From Waters & Proga (2016)

15 A SPECTRAL SIGNATURE FOR CLOUD ACCELERATION PPC model ==>

16 A SPECTRAL SIGNATURE FOR CLOUD ACCELERATION From Waters et al. 2017

17 COMMON VIEW LOCAL SIMULATIONS Property Single cloud Global distribution Single cloud Global distribution Equilibrium Static vs. evolving Confined vs. Accelerating state vs. evaporating outflowing clumpy flow Outflowing Formation/ Thermal instability orbiting blobs vs. Regeneration vs. blobs uplifted condensing clumps from the disk (bloated star winds?) Velocity Unconstrained -10^4-10^4 km/s Density/ Temperature Constant Wide range (e.g., LOC model) TI naturally leads to cloud regeneration v_flow + a*t d_min - d_max T_min - T_max Requires global simulations: Condensing clumps ~v_flow Determined by S-curve Size Wide range Sub parsec to parsec Number 1 10^3-10^7 Shape Motion Emission/ Absorption Blobs, shells, Directed stream vs. slabs, filaments? failed wind vs. mist Keplerian orbit vs. Swarm vs. embedded in wind clumpy outflow Optically Self-shielding is thick vs. thin important? lambda of max growth rate? 1 becomes many Clumpy medium

X-ray signatures of AGN outflows: multi-dimensional radiative transfer simulations

X-ray signatures of AGN outflows: multi-dimensional radiative transfer simulations Stuart Sim Knox Long (STScI) Lance Miller (Oxford) Daniel Proga (UNLV) T. Jane Turner (UMBC) James Reeves (Keele) Overview