Presentation is loading. Please wait.

Presentation is loading. Please wait.

Stability of Accretion Disks WU Xue-Bing (Peking University)

Similar presentations

Presentation on theme: "Stability of Accretion Disks WU Xue-Bing (Peking University)"— Presentation transcript:

1 Stability of Accretion Disks WU Xue-Bing (Peking University)

2 Thanks to three professors who helped me a lot in studying accretion disks in last 20 years Prof. LU Jufu Prof. LI Qibin Prof. YANG Lantian

3 Content Why we need to study disk stability Stability studies on accretion disk models –Shakura-Sunyaev disk –Shapiro-Lightman-Eardley disk –Slim disk –Advection dominated accretion flow Discussions

4 1. Why we need to study stability? An unstable equilibrium can not exist for a long time in nature Some form of disk instabilities can be used to explain the observed variabilities (in CVs, XRBs, AGNs?) Disk instability can provide mechanisms for accretion mode transition unstable stable

5 Some instabilities are needed to create efficient mechanisms for angular momentum transport within the disk (Magneto-rotational instability (MRI); Balbus & Hawley 1991, ApJ, 376, 214) 1. Why we need to study stability?

6 How to study stability? Equilibrium: steady disk structure Perturbations to related quantities Perturbed equations Dispersion relation Solutions: –perturbations growing: unstable –perturbations damping: stable

7 2. Stability studies on accretion disk models Shakura-Sunyaev disk –Disk model (Shakura & Sunyaev 1973, A&A, 24, 337): Geometrically thin, optically thick, three-zone (A,B,C) structure, multi-color blackbody spectrum –Stability: unstable in A but stable in B & C Pringle, Rees, Pacholczyk (1973) Lightman & Eardley (1974), Lightman (1974) Shakura & Sunyaev (1976, MNRAS, 175, 613) Pringle (1976) Piran (1978, ApJ, 221, 652)

8 Disk structure (Shakura & Sunyaev 1973) 1. Inner part: 2. Middle part: 3. Outer part:

9 Shakura & Sunyaev (1976, MNRAS) Perturbations: –Wavelength –Ignore terms of order and comparing with terms of –Perturbation form Surface density Half-thickness –Perturbed eqs ( )

10 Shakura & Sunyaev (1976, MNRAS) Forms of u, h: For the real part of (R), Dispersion relation at < { "@context": "", "@type": "ImageObject", "contentUrl": "", "name": "Shakura & Sunyaev (1976, MNRAS) Forms of u, h: For the real part of (R), Dispersion relation at <

11 Thermally unstable Viscouslly unstable Radiation pressure dominated

12 Piran (1978, ApJ) Define Dispersion relation

13 Piran (1978, ApJ) Two solutions for the dispersion relation viscous (LE) mode; thermal mode An unstable mode has Re( )>0 A necessary condition for a stable disk Thermally stable Viscously stable (LE mode)

14 Piran (1978, ApJ) Can be used for studying the stability of accretion disk models with different cooling mechanisms (b and c denote the signs of the 2nd and 3rd terms of the dispersion relation)

15 Piran (1978, ApJ)

16 S-curve & Limit-cycle behavior Disk Instability Diffusion eq: viscous instability: Thermal instability: limit cycle: A->B->D->C->A... Outbursts of Cataclysmic Variables Smak (1984)

17 Variation of soft component in BH X-ray binaries Viscous timescale Typical timescals Viscous timescale Thermal timescale Belloni et al. (1997) GRS 1915+105

18 2. Stability studies on accretion disk models Shapiro-Lightman-Eardley disk –SLE (1976, ApJ, 207, 187): Hot, two- temperature (T i >>T e ), optically thin, geometrically thick –Pringle, Rees & Pacholczky (1973, A&A): a disk emitting optically-thin bremsstrahlung is thermally unstable –Pringle (1976, MNRAS, 177, 65), Piran (1978): SLE is thermally unstable

19 Pringle (1976) Define Disk is stable to all modes when When, all modes are unstable if

20 Pringle (1976) SLE: ion pressure dominates Ions lose energy to electrons Electrons lose energy for unsaturated Comptonization --> Thermally unstable!

21 2. Stability studies on accretion disk models Slim disk –Disk model: Abramowicz et al. (1988, ApJ, 332, 646); radial velocity, pressure and radial advection terms added –Optically thick, geometrically slim, radiation pressure dominated, super-Eddington accretion rate –Thermally stable if advection dominated

22 Abramowicz et al. (1988, ApJ) Viscous heating: Radiative cooling: Advective cooling: Thermal stability: S-curve: Slim disk branch

23 Papaloizou-Pringle Instability Movie (Produced by Joel E. Tohline, Louisiana State University's Astrophysics Theory Group) Balbus & Hawley (1998, Rev. Mod. Phys.) –One of the most striking and unexpected results in accretion theory was the discovery of Papaloizou-Pringle instability

24 Papaloizou-Pringle Instability Dynamically (global) instability of thick accretion disk (torus) to non-axisymmetric perturbations (Papaloizou & Pringle 1984, MNRAS, 208, 721) Equilibrium

25 Papaloizou-Pringle Instability Time-dependent equations

26 Papaloizou-Pringle Instability Perturbations Perturbed equations

27 Papaloizou-Pringle Instability A single eigenvalue equation for which describes the stability of a polytropic torus with arbitrary angular velocity distribution High wavenumber limit (local approximation), if Rayleigh (1916) criterion for the stability of a differential rotating liquid

28 Papaloizou-Pringle Instability Perturbed equation and stability criteria for constant specific angular momentum tori Dynamically unstable modes

29 Papaloizou-Pringle Instability Papaloizou-Pringle (1985, MNRAS): Case of a non-constant specific angular momentum torus Dynamical instabilities persist in this case Additional unrelated Kelvin-Helmholtz-like instabilities are introduced The general unstable mode is a mixture of these two

30 2. Stability studies on accretion disk models Advection dominated accretion flow –Narayan & Yi (1994, ApJ, 428, L13): Optically thin, geometrically thick, advection dominated –The bulk of liberated gravitational energy is carried in by the accreting gas as entropy rather than being radiated q adv =ρVTds/dt=q + - q - q + ~ q - >> q adv,=> cooling dominated (SS disk; SLE disk) q adv ~ q + >>q -,=> advection dominated

31 Advection dominated accretion flow Self-similar solution (Narayan & Yi, 1994, ApJ)

32 Advection dominated accretion flow Self-similar solution

33 Advection dominated accretion flow Stability of ADAF –Analyzing the slope and comparing the heating & cooling rate near the equilibrium, Chen et al. (1995, ApJ), Abramowicz et al. (1995. ApJ), Narayan & Yi (1995b, ApJ) suggested ADAF is both thermally and viscously stable (long wavelength limit) Narayan & Yi (1995b)

34 Advection dominated accretion flow Stability of ADAF –Quantitative studies: Kato, Amramowicz & Chen (1996, PASJ); Wu & Li (1996, ApJ); Wu (1997a, ApJ); Wu (1997b, MNRAS) –ADAF is thermally stable against short wavelength perturbations if optically thin but thermally unstable if optically thick –A 2-T ADAF is both thermally and viscously stable

35 Wu (1997b, MNRAS, 292, 113) Equations for a 2-T ADAF

36 Wu (1997b, MNRAS, 292, 113) Perturbed equations

37 Wu (1997b, MNRAS, 292, 113) Dispersion relation

38 Wu (1997b, MNRAS, 292, 113) Solutions –4 modes: thermal, viscous, 2 inertial- acoustic (O & I - modes) –2T ADAF is stable

39 Discussions Stability study is an important part of accretion disk theory –to identify the real accretion disk equilibria –to explain variabilities of compact objects –to provide possible mechanisms for state transition in XRBs (AGNs?) –to help us to understand the source of viscosity and the mechanisms of angular momentum transfer in the AD

40 Discussions Disk model –May not be so simple as we thought –Disk + corona; inner ADAF + outer SSD; CDAF? disk + jet (or wind); shock? –Different stability properties for different disk structure Stability analysis –Local or global –Effects of boundary condition –Numerical simulations

Download ppt "Stability of Accretion Disks WU Xue-Bing (Peking University)"

Similar presentations

Ads by Google