10/28/2010 SEAL@GSFC 1 MHD Accretion-Disk Winds - PowerPoint Presentation

1. 10/28/2010 SEAL@GSFC1MHD Accretion-Disk Winds and the Blazar Sequence Demos Kazanas, Chris Shrader (NASA/GSFC)Keigo Fukumura, Sean Scully (JMU)Markos Georganopoulos (UMBC)(based on work by Fukumura, Kazanas, Contopoulos, Behar ApJ (2010), 715, 636 ApJ (2010), 723, L228Credit: NASA/CXC

2. 10/28/2010 SEAL@GSFC2Demos Kazanas (NASA/GSFC) CollaboratorsEhud Behar (Technion, Israel)Ioannis Contopoulos (Academy of Athens, Greece)J. Garcia (CUA/GSFC)T. Kallman (NASA/GSFC)T. Sakamoto (UMBC/GSFC)C. Shrader (USRA/GSFC)J. Turner (UMBC/GSFC)Acknowledgement:

3. The Blazar Sequence (Fossati)10/28/2010 SEAL@GSFC3

4. Does this systematic reflect a broader AGN property or is it limited to blazars?What is the nature of this correlation and how connects to the general AGN physics?(Accounts have been proposed by Ghisellini et al suggesting balance between electron acceleration and losses in AGN vicinity).Our thesis is that it signifies a universal underlying AGN structure hinted to from RQ AGN, in particular from Seyfert X-ray spectroscopy. 10/28/2010 SEAL@GSFC4

5. Dust reprocessing, n(r) ~ 1/r (Rowan-Robinson 1995)10/28/2010 SEAL@GSFC5

6. The Scientific MethodIt is a capital mistake to theorize before one has the data. Insensibly, one begins to twist facts to suit theories, instead of theories to suit facts. Sir Arthur Conan DoyleIt is also a good rule not to put too much confidence in experimental results, until they have been confirmed by theory. Sir Arthur EddingtonFirst you get your facts; then you can distort them at your leisure. Mark Twain10/28/2010 SEAL@GSFC6

7. The general idea is to enlarge, complement, modify this well known cartoon10/28/2010 SEAL@GSFC7

8. 10/28/2010 SEAL@GSFC8Some Facts of AGN absorbers Absorption features are ubiquitous in the spectra of AGN, GBHC. 50% of all AGN were shown to exhibit UV and X-ray absorption features (Crenshaw, Kraemmer, George 2002). These features have a very broad range of velocities both in UV and X-rays (a few 100’s – 30,000 km/sec in the UV and a few 100’s – >100,000 km/sec in X-rays). X-ray features span a factor of ~105 in ionization parameter indicating the presence of ions ranging from highly ionized (H-He - like Fe) to neutral, all in 1.5 decades in X-ray energy! These “live” in very different regions of ionization parameter space and likely in different regions of real space.

9. 10/28/2010 SEAL@GSFC9MCG 6-30-15 Holczer+10Crenshaw+03Netzer+(03)X-ray spectrum of NGC 3783

10. 10/28/2010 SEAL@GSFC10BAL QSO: X-ray AbsorptionsX-ray Absorption line (Fe XXV)Spectral index vs. wind velocityBrandt+(09); Chartas+(09)Chandra/XMM/SuzakuEffect of ionizing spectrum(!?)Fe resonance transitionsX-ray absorber High-velocity outflows: v/c~0.1-0.7 in Fe XXV/XXVI

11. 10/28/2010 SEAL@GSFC11Galactic Black Hole (GBH) BinariesGRO J1655-40: High ionization: log(x[erg cm s-1]) ~ 4.5 - 5.4 Small radii: log (r[cm]) ~ 9.0 - 9.4 High density: log(n[cm-3]) ~ 14Chandra DataMiller+(08) M(BH)~7Msun M(2nd)~2.3MsunNASA/CXC/A.HobartMiller+(06)

12. 10/28/2010 SEAL@GSFC12 Outflowing Ionized Absorbers in UV/X-ray  Photoelectric absorption (1) Moderate Outflows ~ various charge state (~100-1,000 km/sec; Nh ~1021-22 cm-2)  Many charge state from X-ray-bright AGNs e.g. MCG-6-30-15, IRAS 13349+2438 (2) Massive Fast Outflows ~ K-shell resonance (v/c~0.1-0.7; Nh ~1023-24 cm-2)  H/He-like ions from hard-X-ray-weak AGNs e.g. PDS 456, PG 1211+143, APM 08279+5255 Magnetically-Driven Accretion-Disk Winds

13. 10/28/2010 SEAL@GSFC13Our thesis (and hope) is that these diverse data (including those of galactic X-ray sources) can be systematized witha small number of parameters (2) (Elvis 2000; Boroson 2002 )

14. Flows (accretion or winds) and their ionization structure are invariant (independent of the mass of gravitating object;ADAF) if:Mass flux is expressed in terms of Eddington mass flux The radius in terms of the Schwarzschild radiusThe velocities are Keplerian10/28/2010 SEAL@GSFC14

15. 10/28/2010 SEAL@GSFC15Radio-quiet Seyfert AGNsMCG-6-30-15:(z = 0.007749)PhotoelectricAbsorption: Lines Edges Slow ~ 100 km/sec @ low-x High ~ 1,900 km/sec @ high-x Integrated NH ~ 5.3 x 1021 cm-2Holczer+(10)(see also Otani+96, Reynolds+97, Sako+03, Miller+08) Chandra/HETGSslowfast(HETGS)(RGS)slowfast“Warm Absorber”

16. 10/28/2010 SEAL@GSFCX-ray-Bright AGNs QSO: IRAS 13349+2438: (z = 0.10764) X-ray bright, IR-loud/radio-quiet QSO X-ray obs. with ROSAT, ASCA, Chandra, XMM-Newton Ions with various charge state Fe XVII ~ 300 km/sec Potential velocity scatter Integrated NH ~ 1.2x1022 cm-2 Chandra dataHolczer+(07)16

17. Narrow-Line Seyferts (PG QSOs)10/26/2010 CRESST/UMBC17PG 1211+143Pounds+Reeves(09)PDS 456Reeves+(09) “Narrow” Hb line < 2,000 km/sec Weak O III/Hb ratio Strong “Soft X-ray Excess” Highly-blueshifted absorption lines PG 0844+349Pounds+(03)(v/c ~ 0.2)(v/c ~ 0.25)(v/c ~ 0.1)Chandra/XMM-Newton data

18. Credit: NASA/CXC/PSU/M.Weiss/G.Chartas10/28/2010 SEAL@GSFC18Broad Absorption Line (BAL) QSOs: APM 08279+5255z = 3.91 ~10% of optically-selected QSOs Faint X-ray relative to O/(F)UV continua Broad C IV line ~ 2,000-30,000 km/sec Highly-blueshifted ~ 10,000-30,000 km/sec NRAO/AUI/NSF,STScI

19. 10/28/2010 SEAL@GSFC19BAL QSO: UV Apsorptions APM 08279+5255: (z = 3.91) Lensed QSO (x100) Optically-bright IR-loud, radio-quiet High-velocity outflows v/c~0.04-0.1 in C IV (UV: Keck/HIRES)Ellison+(99)l7295l7305UV C IV doubletSrianand+Petitjean(00)

20. 10/28/2010 SEAL@GSFC20Holczer+(07)ionizationBehar(09)AMD(x) = dNH / dlogx ~ (logx)pcolumncolumnionizationAbsorption Measure Distribution (AMD) (5 AGNs) presence of nearly equal NH over ~4 decades in x (p~0.02)where x = L/(n r2)(0.02 < p < 0.29)

21. For radiatively driven winds one obtains 10/28/2010 SEAL@GSFC21Flows not drivenRadiatively !Column density decreasesWith increasing ionization

22. 10/28/2010 SEAL@GSFC22Fundamental Questions: Geometry? Spatial location? Properties? Physical origin?

23. 10/28/2010 SEAL@GSFC23 Accretion disks necessarily produce outflows/winds (launched initially with Keplerian rotation) Driven by some acceleration mechanism(s) Local X-rays heat up and photoionize plasma along the way Need to consider mutual interactions between ions & radiation To AMD through MHD WindsBlandford+Payne(82)Contopoulos+Lovelace(94)Konigl+Kartje(94)Contopoulos(95)Murray+(95;98)Blandford+Begelman(99)Proga+Kallman(04)Everett(05)Schurch+Done(07,08)Sim+(08;10) & more…Konigl+Kartje(94)accelerated

24. Magnetically-Driven Outflows11/19/2010 MSU/Physics24Magnetohydrodynamics (MHD) (At least) 2 candidates: GRO J1655-40 Miller+(06,08) NGC 4151 Kraemer+(05) Crenshaw+Kraemer(07)

25. 10/28/2010 SEAL@GSFC25MHD Disk-Wind Solutions Steady-state, axisymmetric MHD solutions (2.5D): 5 “conserved” quantities: Energy, Ang.Mom., Flux, Ent., Rot.(Contopoulos+Lovelace94)(Prad=0) Look for solutions that the variables separate

26. Assume Power Law radial dependence for all variables10/28/2010 SEAL@GSFC26 Solve for their angular dependence using the force balance equation in the q-direction (Grad-Safranov equation).This is a wind-type equation that has to pass through the appropriate critical points.

27. The density has a very steep q-dependence with the polar column being 103 – 104 smaller than the equatorial. The wind IS the unification torus (Konigl & Kartje 1994). 10/28/2010 SEAL@GSFC27MHD Wind Angular Density Profile T. Fischeret al.(2012) e (q-p/2)/0.2

28. 10/28/2010 SEAL@GSFC28Simple Wind Solutions with n~1/rDensityLaunch siteAt small latitudes vt >> vp (disk-like) while at high latitudes vt ~1/r but vp ~ constant (wind-like). (Fukumura+10a)PoloidalvelocityToroidalvelocity[cm-3]

29. With the above scalingsIn order that n(r)~1/r, s = 1 andThe mass flux in the wind increases with distance!! (Behar+ 03; Evans 2011; Nielsen et al. 2011). Or rather, most of the accreting gas “peels-off” to allow only a small fraction to accrete onto the black hole (Blandford & Begelman 1999).There is mounting observational evidence that the mass flux in the wind is much higher than that needed to power the AGN/LMXRB.Feedback! Edot ~ mdot v2 ~r-1/2 ; Momentum input: Pdot ~ mdot v ~ logr  Equal momentum per decade of radius! 10/28/2010 SEAL@GSFC29

30. By expressing BH luminosity in terms of dimensionless variables ( or ) the ionization parameter can now be expressed in the dimensionless variablesFor s=1, x(r) ~ 1/r ; species “living” in lower x-space should come from larger distances.The radiation seen by gas at larger distances requires radiative transfer thru the wind.10/28/2010 SEAL@GSFC30

31. Calculate the photon and B-field densities10/28/2010 SEAL@GSFC31

32. Compton Dominance Condition10/28/2010 SEAL@GSFC32This condition depends only on one global Parameter, namely the wind mass flux rate!

33. A precise calculation can be carried out by computing the scattered specific intensity and then integrating over angles to obtain the energy density10/28/2010 SEAL@GSFC33D

34. 10/28/2010 SEAL@GSFC34We seek “q=1” self-similar wind: B(r,q) ~ B(q)/r n(r,q) ~ F(q)/r (i.e. equal column per decade in radius) LoS velocity ~ 1/r1/2 (Keplerian profile) x(r,q) ~ G(q)/r (w/o attenuation)DensityLoS column densityIonization parameterx = r/rs(c.f. Ueda+03; Tueller+08)(Contopoulos+Lovelace94)MHD Disk-Wind Solutions

35. 10/28/2010 SEAL@GSFC35Photoionization with XSTAR (e.g. Kallman+Bautista01) LoS Radiation Transfer1D computational zones IonizationDistributionLoSRadiation Source[cm-3]Density

36. 10/28/2010 SEAL@GSFC36Modeling AMD with n~1/rModerately-ionized: (above Fe XVII)~100-300 km/sec@ low ionizationHighly-ionized:(Fe XXV/XXVI)~1,000-3,000 km/sec@ high ionization Const. AMDFlat AMD (Model)columnvelocityionizationFlat AMD (Data)Holczer+(07)(q=1)

37. Fe Ionic Abundances and AMD for LoS angle 30 deg10/28/2010 SEAL@GSFC37

38. 10/28/2010 SEAL@GSFC38Modeling Absorption SpectraWind optical depthLine photo-absorption cross-sectionfij = oscillator strength DnD = broadening factor H(a,u) = Voigt function(e.g. Mihalas78)

39. 10/28/2010 SEAL@GSFC39“torus?”~1-10 pc“corona”~AUsNASA/CXCDisk WindGallagher(07)“big blue bump”~lt days[Infrared]BAL QSO SEDSee;Elvis+(94)Richards+(06)[O/UV][X-ray]aox = 0.384 log (f2 keV / f2500 Å) tells you X-ray weaknessaox

40. Implications, Tests All accreting BH have winds with velocities reaching v~0.5 c! We do not perceive them because they are highly ionized. While NH and x are scale invariant for MHD flows the invariance is broken by atomic physics and radiative processes: Gas densities scale like ~1/M implying that forbidden lines should not be present in the galactic LMXRB spectra. Low ionization species are also absent in LMXRBs because the size of winds is limited by the presence of the companion. The dust sublimation distance in LMXRBs is generally beyond the edge of the disk  No Sy2-like IR spectra for galactic sources.10/28/2010 SEAL@GSFC40

41. 10/28/2010 SEAL@GSFC41Apply the model to BAL QSOs by changing only aOX : The decrease in ionizing X-rays allow for FeXXV very close to the BH  hi FeXXV velocity, absorption of CIV forming photons  CIV forms also at small distances leading to hi CIV velocity (but smaller than that of FeXXV). mdot = 0.5 kT(in) = 5eV GX = 2 aOX = -2Injected SED (Fn)Log(density)Fukumura+(10b)

42. AMD10/28/2010 SEAL@GSFC42 mdot = 0.5 kT(in) = 5eV GX = 2 aOX = -2Production of CIV and FeXXV/XXVI

43. 43Correlations with Outflow VelocityVelocity Dependence on SED (X-ray)10/28/2010 SEAL@GSFC X-ray data of APM 08279+5255 from Chartas+(09) Model from Fukumura+(10b)

44. Correlations of column with velocity10/28/2010 SEAL@GSFC44

45. Ha – Bolometric Luminosity10/28/2010 SEAL@GSFC45Using the scalingone can calculaten^2 V and then theHalpha luminosityBy integrating out to x ~ 10^6 to obtainL Ha ~ M mdot^2

46. IR EmissionDust reprocessing: For n(r)~1/r, equal energy per decade of radius is absorbed and emitted as dust IR emission at progressively decreasing temperature. This leads to a flat nuFnu IR spectrum 10/28/2010 SEAL@GSFC46

47. The Blazar Sequence10/28/2010 SEAL@GSFC47The blazar spectra becomedominated by the contributionof an External Compton component as their luminosityincreases. This is easily explained by scattering of the continuum source radiation whose influenceDecreases like mdot^2 , while that of the magnetic field likemdot^1

48. 10/28/2010 SEAL@GSFC48

49. Conclusions (final)We have produced an MHD model for ionized AGN outflows with 3 parameters: mdot (dimensionless), inclination angle q, and aOX . However the relation between and aOX and luminosity 10/28/2010 SEAL@GSFC49Implies that AGN can be described with only two parameters . So there is hope for understanding them! Also, the well known picture

50. 10/28/2010 SEAL@GSFC50Should be modified to Include these winds …

51. 10/28/2010 SEAL@GSFC51(Note that different LoS can see different continua; X-ray and UV absorbers need not be identical)Microlensing technique (e.g. Morgan+08; Chartas+09a)  UV regions > X-ray regions (x ~10)torus

52. Thank you!10/28/2010 SEAL@GSFC52

53. 10/28/2010 SEAL@GSFC53SummaryWe propose a simplistic (self-similar) MHD disk-wind model: Key ingredients  mdot (column) LOS angle (velocity) Fn (SED; G, aOX, MCD…etc.) q (field geometry + density structure) This model (in part) can account for interesting observables: Observed AMD (i.e. local column distribution NH as a function of x) Observed wind kinematics and outflow geometry: Seyferts  ~100-300 km/s (Fe XVII); ~1,000-3,000 km/s (Fe XXV) BAL QSOs  ~ 0.04-0.1c (UV C IV); ~ 0.4-0.8c (X-ray Fe XXV)

54. END10/28/2010 SEAL@GSFC54

55. 10/28/2010 SEAL@GSFC55*Acceleration Process(es)1. Compton-heated wind (e.g. Begelman+83, Woods+96) “ Central EUV/X-ray  heating a disk  thermal-wind” Issue  Too large radii…2. Radiatively-driven (line-driven) wind (e.g. Proga+00, Proga+Kallman04) “UV radiation pressure  accelerate plasma” Issues  Overionization @ smaller radii…  Ionization state freezing out…3. Magnetocentrifugally-driven wind “Large-scale B-field  accelerate plasma” Issue  Unknown field geometry…

56. 10/28/2010 SEAL@GSFC56Issues (Future Work)Wind Solutions (Plasma Field): (Special) Relativistic wind Radiative pressure (e.g. Proga+00;Everett05;Proga+Kallman04) Radiation (Photon Field): Realistic SED (particularly for BAL quasars) Different LoS between UV and X-ray (i.e. RUV > RX by x10…) Including scattering/reflection (need 2D radiative transfer) (Ultimate) Goals: Comprehensive understanding of ionized absorbers within a single framework (i.e. disk-wind) AGNs/Seyferts/BAL/non-BAL QSO with high-velocity outflows (e.g. PG 1115+080, H 1413+117, PDS 456 and more…) Energy budget between radiation and kinetic energy…

57. 10/28/2010 SEAL@GSFC57Broad Absorption Line (BAL) QSOs Became known with ROSAT/ASCA survey Large C IV EW(absorb) ~ 20-50 A ~ 30,000 km/sec ~10% of optically-selected QSOs Faint (soft) X-ray relative to O/UV continua High-velocity/near-relativistic outflows: v/c ~ 0.04 - 0.1 (e.g. UV C IV) v/c ~ 0.1 - 0.8 (e.g. X-ray Fe XXV) High intrinsic column of ~ 1022 cm-2 (UV) >~ 1023 cm-2 (X-ray)

58. 10/28/2010 SEAL@GSFC58Review on Absorption Features: Crenshaw, Kraemer & George 2003, ARAA, 41, 117 (Seyferts) Brandt et al. 2009, arXiv:0909.0958 (Bright Quasars)

59. 10/28/2010 SEAL@GSFC59ENDChandra surveyGallagher+(06)

60. Para.CL94BP82Br-1r-5/4vr-1/2r-1/2rr-1r-3/2M_windr1/2r1/2Mdot(mass loss rate) ~ 10-6 Mo/yr Fo (ai/1AU)5/2 (M/Mo)-1/2 (Bo/1G)2 ~ 6x1019 g/sec Fo (ai/1AU)5/2 (M/Mo)-1/2 (Bo/1G)2 ~ 6x1013-16 g/sec (ai/1AU)5/2 for M=108Mo, Fo=0.0-0.1, Bo=1-10Gr ~ ai-1 Fo(Bo/vo)2 r*6010/28/2010 SEAL@GSFC

61. 10/28/2010 SEAL@GSFC61Lya C IV10. Normal galaxies vs. BAL quasarsMg IIHaHbLya NVSi IVC IVbroad absorption lines(P Cygni profiles)normalBAL

62. 10/28/2010 SEAL@GSFC62Ramirez(08)

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64. 10/28/2010 SEAL@GSFC6412. Quasars – SED (UV/X-ray property)Chandra BAL QSO surveyGallagher+(06)UV-bright, X-ray-faint!aox = 0.384 log (f2 keV / f2500 Å) tells you X-ray weakness2 keV2500 ÅElvis+(94)Richards+(06)?

65. 10/28/2010 SEAL@GSFC65fainter in X-rays228 SDSS Quasars with ROSAT (Strateva et al. 2005)UV Luminosity vs. aoxbrighter in X-raysDefine:Daox = aox - aox (Luv)log(Luv) (ergs s-1 Hz-1)

66. 10/28/2010 SEAL@GSFC66XMM-Newton dataChartas+(09)G ~ 1.7 – 2.1 Log(NH) ~ 23-24T(var) ~ 3.3 days (~10 rg)X-ray

67. 10/28/2010 SEAL@GSFC67Feb. 2010 @JapanFace-down view (e.g. ~30deg)  low NH, low v/cOptimal view (e.g. ~50deg)  high NH, high v/c(ii) Velocity dependence on LoS

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