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

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

2 Collaborators J. Stone, T. Kallman, J. Raymond, M. Begelman, J. Ostriker, R. Kurosawa, J. Drew, A. Janiuk, M. Moscibrodzka, B. Czerny, A. Siemiginowska, S. Sim, A. Dorodnityn, S. Sim, S. Luketic, T. Waters, M. Giustini, 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 (please see other talks in this session)

9 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure - magnetic fields (please see other talks in this session) - and in some combinations.

10 OUTLINE 1. Introduction 2. Multidimensional, time-dependent simulations of disk winds driven by: - thermal expansion - radiation pressure - magnetic fields (please see other talks in this session) - 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 See a poster by Tim Waters

21 Accretion Disks in Various Objects Two examples:

22 Thermal Disk Winds

23 GRS Neilsen & Lee (2009) fig. from DP s 2009 News & Views

24 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...!!! future... ATHENA? GRO J Observations: Miller et al. (2006)

25 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)

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

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

28 X-ray and UV source

29 Luketic et al. (2010)

30 GRO J

31 GRO J

32 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 also Neilsen & Lee 2009)!

33 Radiation-Driven Winds

34 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

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

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

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

39 HD simulations and their line profiles

40 HD simulations and their line profiles

41 HD simulations and their line profiles

42 HD simulations and observations

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

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

45 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)

46 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)

47 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)

48 Drew & Proga (1999)

49 Drew & Proga (1999)

50 Drew & Proga (1999)

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

52 Thermal and Radiation- Driven Winds

53 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

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

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

56 M = 8 BH Γ = Msun

57 DP, Stone, & Kallman (2000) DP & Kallman (2004)

58 DP, Stone, & Kallman (2000) DP & Kallman (2004)

59 DP, Stone, & Kallman (2000) DP & Kallman (2004)

60 Paola Rodriguez-Hidalgo, DP, F. Hamann

61 Broad band spectra for various l.o.s. Schurch, Done, & DP (2009)

62 Broad band spectra for various l.o.s. Schurch, Done, & DP (2009)

63 Broad band spectra for various l.o.s. Schurch, Done, & DP (2009)

64 Broad band spectra for various l.o.s. 50 o 57 o 62 o 65 o 67 o Schurch, Done, & DP (2009)

65 Broad band spectra for various l.o.s. 50 o 57 o 62 o 65 o 67 o Schurch, Done, & DP (2009)

66 Broad band spectra for various l.o.s. 50 o 57 o 62 o 65 o 67 o Schurch, Done, & DP (2009)

67 Broad band spectra for various l.o.s. 50 o 57 o 62 o 65 o 67 o Schurch, Done, & DP (2009)

68 Broad band spectra for various l.o.s. Sim et al. (2010)

69 Broad band spectra for various l.o.s. Sim et al. (2010)

70 Broad band spectra for various l.o.s. Sim et al. (2010)

71 Broad band spectra for various l.o.s. Sim et al. (2010)

72 Quasar Irradiation

73 Quasar Irradiation

74 Quasar Irradiation

75 Quasar Irradiation?

76 Quasar Irradiation?

77 An outflow from an inflow

78 M = 8 BH 10 M SUN M = 26 D 10 g/ s =1.6M SUN T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV f = X 0.5 / yr

79 M = 8 BH 10 M SUN M = 26 D 10 g/ s =1.6M SUN T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV f = X 0.5 / yr Proga (2007)

80 M = 8 BH 10 M SUN M = 26 D 10 g/ s =1.6M SUN T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV 0.95 f = X 0.05 / yr

81 M = 8 BH 10 M SUN M = 26 D 10 g/ s =1.6M SUN T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV 0.95 f = X 0.05 / yr

82 M = 8 BH 10 M SUN M = 26 D 10 g/ s =1.6M SUN T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV 0.95 f = X 0.05 / yr Proga (2007)

83 M = 8 BH 10 M SUN M = 26 D 10 g/s =1.6M SUN/ yr T = X 8 x 7 10 K ρ( r o )= g/ cm f = UV 0.95 f = X 0.05

84 Effects of gas rotation, optical depth and X-ray background radiation

85 Effects of gas rotation, optical depth and X-ray background radiation DP, Ostriker, Kurosawa (2007)

86 Effects of gas rotation, optical depth and X-ray background radiation no rotation DP, Ostriker, Kurosawa (2007)

87 Effects of gas rotation, optical depth and X-ray background radiation no rotation rotation DP, Ostriker, Kurosawa (2007)

88 Effects of gas rotation, optical depth and X-ray background radiation no rotation rotation rotation and opt. thick DP, Ostriker, Kurosawa (2007)

89 Effects of gas rotation, optical depth and X-ray background radiation no rotation rotation no X-ray background rotation and opt. thick DP, Ostriker, Kurosawa (2007)

90 Effects of gas rotation, optical depth and X-ray background radiation no rotation rotation no X-ray background rotation and opt. thick X-ray background DP, Ostriker, Kurosawa (2007)

91

92 Dynamical model for clouds in NLR!?

93 Dynamical model for clouds in NLR!?

94 Dynamical model for clouds in NLR!?

95 3-diminesional simulations Kurosawa & DP (2009a)

96 Clouds properties density map temperature map Kurosawa & DP (2009a)

97 What is the limit for the mass supply rate? Kurosawa & DP (2009b)

98 What is the limit for the mass supply rate? Kurosawa & DP (2009b)

99 What is the limit for the mass supply rate? Kurosawa & DP (2009b)

100 What is the limit for the mass supply rate? Kurosawa & DP (2009b)

101 What is the limit for the mass supply rate? Kurosawa & DP (2009b)

102 What is the geometry of the outflow?

103 What is the geometry of the outflow? jet like

104 What is the geometry of the outflow? jet like i/o

105 What is the geometry of the outflow? jet like i/o disk-wind like

106 How efficient are the outflows? Kurosawa, DP, & Nagamine (2009)

107 How efficient are the outflows? 10^-4 Kurosawa, DP, & Nagamine (2009)

108 AGN feedback

109 AGN feedback Watt centrifugal governor of 1788

110

111

112

113

114

115

116

117

118 ?

119 ?

120 ?

121 Ciotti, Ostriker, & DP (2010)

122 Conclusions

123 Conclusions Simulations of accretion flows and their outflows provide important insights into the dynamics and geometry of the material that produces radiation. In particular, we can use the simulations to assess the effects of radiation on the flow properties. We can also explore coupling between accretion flows and they outflows as well as mass supply (e.g., various forms of feedback).

124 Conclusions Simulations of accretion flows and their outflows provide important insights into the dynamics and geometry of the material that produces radiation. In particular, we can use the simulations to assess the effects of radiation on the flow properties. We can also explore coupling between accretion flows and they outflows as well as mass supply (e.g., various forms of feedback). 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).

125 Future Works

126 Future Works Add effects of dust.

127 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic).

128 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic).

129 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic). Follow interaction of disk winds with outer inflows/outflows and incorporate these type of simulations into cosmological simulations

130 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic). Follow interaction of disk winds with outer inflows/outflows and incorporate these type of simulations into cosmological simulations

131 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic). Follow interaction of disk winds with outer inflows/outflows and incorporate these type of simulations into cosmological simulations

132 Future Works Add effects of dust. Add other modes of operation (e.g., radiatively inefficient accretion, magnetic). Follow interaction of disk winds with outer inflows/outflows and incorporate these type of simulations into cosmological simulations Most importantly, keep comparing the model predictions with observations of AGN.

133 Quenching Disk Corona DP (2005)

134 Quenching Disk Corona Disk DP (2005)

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

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

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

138 Where is the X-ray corona?

139 Where is the X-ray corona?

140 Where is the X-ray corona???

141 Where is the X-ray corona???

142 Where is the X-ray corona???

143

144 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)

145 Black Hole Accretion -> Outflow

146 Black Hole Accretion -> Outflow

147

148

149 Multi-component flow

150 Multi-component flow torus

151 Multi-component flow torus corona torus

152 Multi-component flow torus wind torus corona torus

153 Multi-component flow torus wind torus corona torus low l inflow

154 Multi-component flow torus wind torus corona torus low l inflow outflow/jet

155 Multi-component flow torus wind torus corona torus low l inflow outflow/jet see Moscribrodzka et al for spectra predicted by such flows

156 Does it have to be so complex?

157 Does it have to be so complex?

158 Does it have to be so complex?

159 Does it have to be so complex? Proga (2005)

160 Does it have to be so complex? Answer: No, it does not. Proga (2005)

161 Ciotti, Ostriker, & Proga (2010)

162 Ciotti, Ostriker, & Proga (2010)

163 Ciotti, Ostriker, & Proga (2010)

164 MHD Driven Winds

165 MHD and Radiation Driven Winds

166 MHD-LD Disk Winds DP (2003a)

167 MHD-LD Disk Winds DP (2003a)

168 MHD-LD Disk Winds DP (2003a)

169 MHD-LD Disk Winds DP (2003a)

170 The mass loss rate in MHD-LD winds.

171 The mass loss rate in MHD-LD winds.

172

173 A big picture L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd

174 A big picture L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

175 A big picture 1/(TOTAL UV LINE OPACITY) L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

176 A big picture 1/(TOTAL UV LINE OPACITY) AGN (SMBH) L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

177 A big picture 1/(TOTAL UV LINE OPACITY) AGN (SMBH) CV (WD) L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

178 A big picture 1/(TOTAL UV LINE OPACITY) FU Ori (MS S) AGN (SMBH) CV (WD) L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

179 A big picture 1/(TOTAL UV LINE OPACITY) FU Ori (MS S) AGN (SMBH) CV (WD) LMXB (NS) GBH (LM BH) L Edd = 4πcGM a σ L = M M a G 2r a Γ = L M = a σ L Edd 8πcr a Γ UV = L UV L Edd Proga (2002)

180 Conclusions

181 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating.

182 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability.

183 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?).

184 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?). The outflows are multi-temperature/phases (as in WA?).

185 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?). The outflows are multi-temperature/phases (as in WA?). The I/O solution is quite robust but its characteristics are sensitive to the geometry and SED of the central object radiation.

186 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?). The outflows are multi-temperature/phases (as in WA?). The I/O solution is quite robust but its characteristics are sensitive to the geometry and SED of the central object radiation. The mass supplied rate does not appear to be limited by the luminosity of AGN.

187 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?). The outflows are multi-temperature/phases (as in WA?). The I/O solution is quite robust but its characteristics are sensitive to the geometry and SED of the central object radiation. The mass supplied rate does not appear to be limited by the luminosity of AGN. The outflow is inefficient in removing energy.

188 Conclusions A significant fraction of the inflowing matter can be expelled by radiation pressure and heating. The non-rotating flow settles into a steady inflow/outflow solution. Gas rotation and large optical depth can lead to time variability. In time variable flows, dense clouds form (as in NRL of AGN?). The outflows are multi-temperature/phases (as in WA?). The I/O solution is quite robust but its characteristics are sensitive to the geometry and SED of the central object radiation. The mass supplied rate does not appear to be limited by the luminosity of AGN. The outflow is inefficient in removing energy. Disk winds are much more efficient than the large scale outflows

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