Simulations of Mass Outflows from Accretion Powered Sources

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1 Simulations of Mass Outflows from Accretion Powered Sources Daniel Proga UNLV

2 Collaborators J. Drew J. Stone T. Kallman J. Raymond M. Begelman J. Ostriker R. Kurosawa A. Janiuk M. Moscibrodzka B. Czerny A. Siemiginowska A. Dorodnityn S. Sim S. Luketic T. Waters, and many more

3 OUTLINE

4 OUTLINE 1. Introduction

5 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by:

6 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion

7 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure

8 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure - magnetic fields

9 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure - magnetic fields - and in some combinations.

10 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure - magnetic fields - and in some combinations. 3. Conclusions

11 What can drive an outflow?

12 What can drive an outflow? Thermal expansion (evaporation, hydrodynamical escape)

13 What can drive an outflow? Thermal expansion (evaporation, hydrodynamical escape) Radiation pressure (gas, dust)

14 What can drive an outflow? Thermal expansion (evaporation, hydrodynamical escape) Radiation pressure (gas, dust) Magnetic fields

15 What can drive an outflow? Thermal expansion (evaporation, hydrodynamical escape) Radiation pressure (gas, dust) Magnetic fields In most cases, rotation plays a key role (directly or indirectly) especially in AD.

16 Accretion Disks vs Stars

17 Accretion Disks vs Stars

18 Accretion Disks vs Stars

19 Accretion Disks vs Stars

20 Accretion Disks vs Stars

21 Accretion Disks in Various Objects Two examples:

22 Thermal Disk Winds

23 X-ray Transient Sources Most of the accretion energy is emitted in X-rays. The radiation energy is still too low to drive an outflow from the inner disk. But the radiation from the inner disk can heat up the outer disk. However, spectral features of disk winds have not been seen from these systems until recently (Schulz & Brandt 2002;Miller et al. 2006, 2008; Kubota et al. 2007; Neilsen & Lee 2009). Thank you Chandra, XMM-Newton, and Suzaku...!!! IXO GRO J Observations: Miller et al. (2006)

24 X-ray Transient Sources GRO J Interpretation and spectral modeling: Miller et al. (2006, 2008), Netzer (2006), Kallman et al. (2009). Dedicated hydrodynamical simulations (Luketic et al. 2010) Observations: Miller et al. (2006)

25 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e The equations are solved using the ZEUS code (Stone & Norman 1992) extended by Proga, Stone, & Kallman (2000; see also Proga, Stone & Drew 1998, 1999; Proga & Kallman 2002, PD 2007, Kursowa & Proga 2008, 2009a, b)

26 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e The equations are solved using the ZEUS code (Stone & Norman 1992) extended by Proga, Stone, & Kallman (2000; see also Proga, Stone & Drew 1998, 1999; Proga & Kallman 2002, PD 2007, Kursowa & Proga 2008, 2009a, b)

27 X-ray and UV source

28 Luketic et al. (2010)

30 For more on the wind geometry see the poster by Tim Waters

31 GRO J

32 GRO J

33 GRO J The thermal wind is not dense enough to account for the observed wind. But does it mean that the thermal wind is unimportant? Maybe not because the wind mass lose rate can be as high as 5 times the disk accretion rate (see Neilsen & Lee 2009)!!!

34 Radiation-Driven Winds

35 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e

36 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e

37 Geometry

38 Geometry Radiation flux

39 Geometry Radiation flux

40 Geometry Radiation flux

41 L = D 1 L = S 0 L = D 3 L = S 0 L = D 3 L = S 3 13 L = D 3 L = S 9 Proga, Stone & Drew (1998)

42 But the disk emits the UV radiation only from a relatively narrow ring.

44 L(disk)=3 L(star)=0

45 L(disk)=3 L(star)=0 L(disk)=3 L(star)=3

46 HD simulations and their line profiles

47 HD simulations and their line profiles

48 HD simulations and their line profiles

49 HD simulations and observations

50 HD simulations and observations L = D 23.4L, SUN L = WD 0.25L, D M = a M SUN 1 yr

51 HD simulations and observations L = D 23.4L, SUN L = WD 0.25L, D M = a M SUN 1 yr

52 HD simulations and observations L = D 23.4L, SUN L = WD 0.25L, D M = a M SUN 1 yr CIV 1549 for IX Vel (Hartley et al. 2001); models Proga (2003b)

53 Drew & Proga (1999)

54 Drew & Proga (1999)

55 Drew & Proga (1999)

56 a M = M Sun M = WD 1M Sun 1 yr Drew & Proga (1999)

57 For more on the radiation driven outflows see talk by Ryuichi Kurosawa a M = M Sun M = WD 1M Sun 1 yr Drew & Proga (1999)

58 MHD and Radiation Driven Winds

59 MHD-LD Disk Winds DP (2003a)

60 MHD-LD Disk Winds DP (2003a)

61 MHD-LD Disk Winds DP (2003a)

62 MHD-LD Disk Winds DP (2003a)

63 The mass loss rate in MHD-LD winds.

64 The mass loss rate in MHD-LD winds.

65 Thermal and Radiation- Driven Winds

66 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e

67 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e

68 The equations of hydrodynamics Dρ Dt + ρ v = 0 ρ Dv = P + ρg + ρ f rad Dt ρ D e = P v + ρl Dt ρ P = (γ 1)e

69 M = 8 BH Γ = Msun

70 Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

71 Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

72 Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

73 Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

74 For more on synthetic spectra see talk by Stuart Sim Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

75 Quenching Disk Corona DP (2005)

76 Quenching Disk Corona Disk DP (2005)

77 Quenching Disk Corona Disk Disk and inflow/outflow DP (2005)

78 Quenching Disk Corona Disk Disk and inflow/outflow Disk and corona DP (2005)

79 Quenching Disk Corona Disk Disk and inflow/outflow Disk and corona Disk and??? DP (2005)

80 Where is the X-ray corona?

81 Where is the X-ray corona?

82 Where is the X-ray corona???

83 Where is the X-ray corona???

84 Where is the X-ray corona???

85 Conclusions

86 Conclusions Simulations of accretion flows and their outflows provide important insights into the dynamics and geometry of the material that produces radiation (we can use the simulations to assess the effects of radiation on the flow properties).

87 Conclusions Simulations of accretion flows and their outflows provide important insights into the dynamics and geometry of the material that produces radiation (we can use the simulations to assess the effects of radiation on the flow properties). The simulations can be and are used to compute synthetic spectra for direct comparison with the observations. As such, the simulations are useful in explaining specific spectral features as well as overall shape of the SED (not just pretty movies with complex equations/physics behind).

88 Conclusions Simulations of accretion flows and their outflows provide important insights into the dynamics and geometry of the material that produces radiation (we can use the simulations to assess the effects of radiation on the flow properties). The simulations can be and are used to compute synthetic spectra for direct comparison with the observations. As such, the simulations are useful in explaining specific spectral features as well as overall shape of the SED (not just pretty movies with complex equations/physics behind). In general, we have moved beyond spectra modeling: we can predict spectra based on a physical model, some properties of which can be determined from first principles.

Simulations of Winds. Daniel Proga University of Nevada, Las Vegas Princeton University

Simulations of Winds. Daniel Proga University of Nevada, Las Vegas Princeton University Simulations of Winds Daniel Proga University of Nevada, Las Vegas Princeton University Collaborators J. Stone, T. Kallman, J. Raymond, M. Begelman, J. Ostriker, R. Kurosawa, J. Drew, A. Janiuk, M. Moscibrodzka,