Close binary systems Jean-Pierre Lasota Lecture 4 Accretion discs I.

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Presentation transcript:

Close binary systems Jean-Pierre Lasota Lecture 4 Accretion discs I

Accretion disc formation in a binary system

Eclipsing binary allow observing elements of the accretion configuration

(previous slide) (next slide)

ingress egress

For stationary, Keplerian discs the effective T varies like Brightness temperature Stationary, Keplerian discs do exist !

This is a non-stationary accretion disc; dwarf nova at minimum light

Double emission lines: result of differential (Keplerian rotation).

Doppler tomography

Magneto-Rotational Instability (MRI) creates turbulence in Keplerian accretion discs Higher velocity; lower angular mom. lower velocity; higher angular mom. (weak) magn. field This is unstable and transports ang. mom. outwards, i.e. allows accretion.

f=0 Epicyclic frequency Oscillator analogue: There exist solutions representing unstable modes

: Radial equations for a Keplerian accretion disc 1. Mass-conservation (continuity) equation: 2. Angular momentum conservation equation: Tidal torque

3. Momentum conservation Euler (equation) 4. Energy conservation equation - mid-plane temperature,