Probing Galactic Centres with Tidal Disruption Events
Almog Yalinewich
21.5.19
Journey to the Galactic Centre
A glimpse to the Supermassive Black Hole in M87
Galactic Centre Mysteries
Star formation in extreme environments
Star - Central Black Hole interactions
Gas Accretion
The Twist
Types of Galactic Centres
Active
Very bright
Quiescent
very close
Tidal Disruption Events
Evidence
Schematic
Tidal Radius
Apoapse Distance
Tidal Radius
To black hole
Black Hole Mass Limit
Tidal radius
gravitational radius
Apoapse Distance
To black hole
Forensics
?
Optical and X - Ray Signals
Outflow Driven Radio
black hole & accretion disc
cold outflow
cold ambient medium
hot outflow
hot ambient medium
Non Thermal Radio
Radio supernova
Synchrotron
Fermi Acceleration
Diffuse Shock Acceleration
think about adiabatic compression
Self Absorption
Synchrotron Spectra for ASASSN-14li
Degeneracy
Origin of the Outflow
Accretion disc Jet
Accretion disc Jet
Unbound debris
Unbound Debris
The Precursor
Energetics
Radio signal from ASASSN-14li
Simulations
High impact parameter
Simulations
Low impact parameter
Mass Velocity Distribution
high impact parameter
low impact parameter
Bow Shock
Shocked region = 3 x obstacle size
Density Profile for ASASSN 14li
Event Rate
Full loss cone
Empty loss cone
That's gas density.
What about the stellar density?
Generalised Bondi Problem
Governing Equations
Mach Number Profile
to the black hole
outside
Density Profile
Asymptotic Expansion
Total number of stars
Stellar density slope
Implications for ASASSN 14li
If there is no break
Governing equations can be solved analytically
Summary
Radio LoudĀ TDE -> density profile in a GC
Density profile -> Density of wind emitting stars
Wind emitting -> main sequence stars?
questions?
Probing Galactic Centres with Tidal Disruption Events
By almog yalinewich
Probing Galactic Centres with Tidal Disruption Events
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