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Active Galactic Nuclei. 4C15 - High Energy Astrophysics [email protected] http://www.mssl.ucl.ac.uk/. 6. Active Galactic Nuclei (AGN): AGN accretion; Sources of energy; Radio galaxies and jets; [2]. Introduction. Apparently stellar Non-thermal spectra High redshifts

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active galactic nuclei

Active Galactic Nuclei

4C15 - High Energy Astrophysics

[email protected]

http://www.mssl.ucl.ac.uk/

slide2
6. Active Galactic Nuclei (AGN): AGN accretion; Sources of energy; Radio galaxies and jets; [2]
introduction
Introduction
  • Apparently stellar
  • Non-thermal spectra
  • High redshifts
  • Seyferts (usually found in spiral galaxies)
  • BL Lacs (normally found in ellipticals)
  • Quasars (nucleus outshines its host galaxy)
agn accretion
AGN Accretion

Believed to be powered by accretion onto supermassive black hole

high luminosities

highly variable

Eddington limit => large mass

small source size

Accretion onto supermassive black hole

quasars finding their mass
Quasars - finding their mass

The Eddington Limit

Where inward force of gravity balances the outward ‘push’ of

radiation on the surrounding gas.

L

mass

Edd

So a measurement of quasar luminosity gives the minimum mass

– assuming radiation at the Eddington Limit

measuring a quasar s black hole
Measuring a Quasar’s Black Hole

Light travel time effects

If photons leave A and B at the same time, A arrives at the observer a time t ( = d / c ) later.

A

B

If an event happens at A and takes a time dt, then we see a change over a timescale t+dt. This gives a maximum value for the diameter, d, because we know that our measured timescale must be larger than the light crossing time.

d = c x t

c = speed of light

d = diameter

accretion disk and black hole
Accretion Disk and Black Hole
  • In the very inner regions, gas is believed to form a disk to rid itself of angular momentum
  • Disk is about the size of our Solar System
  • Geometrically thin, optically-thick
  • and radiates like a collection of
  • blackbodies
  • Very hot towards the centre
  • (emitting soft X-rays) and
  • cool at the edges (emitting
  • optical/IR).
accretion rates
Accretion Rates

Calculation of required accretion rate:

.

quasars
Quasars

This animation takes you on a tour of a quasar from beyond the galaxy, right up to the edge of the black hole.

  • Animation of a quasar

It covers ten orders of magnitude, ie the last frame covers a

distance 10 billion times smaller than the first.

  • Enter galaxy – see spiral arms and stars
  • Blue and white blobs are “narrow line” clouds
  • Red/yellow disc is molecular torus
  • Purple/green/yellow blobs are “broad line” clouds
  • Blue/white disc is the accretion disc
  • Note the jets perpendicular to accretion disc plane
accretion disk structure

Dissipation rate, D(R) is

= blackbody flux

R

Accretion Disk Structure

The accretion disk (AD) can be considered as

rings or annuli of blackbody emission.

disk temperature
Disk Temperature

Thus temperature as a function of radius T(R):

and if

then for

disk spectrum
Disk Spectrum

Flux as a function of frequency, n -

Total disk spectrum

Log n*Fn

Annular BB emission

Log n

black hole and accretion disk
Black Hole and Accretion Disk

For a non-rotating spherically symetrical BH, the

innermost stable orbit occurs at 3rg or :

and when

high energy spectra of agn
High Energy Spectra of AGN

Spectrum from the optical to medium X-rays

Low-energy disk tail

Comptonized disk

Balmer cont, FeII lines

high-energy disk tail

Log (nFn)

optical UV EUV soft X-rays X-rays

14 15 16 17 18

Log n

fe k a line
Fe Ka Line

Fluorescence line observed in Seyferts – from gas with temp of at least a million degrees.

FeKa

X-ray

e-

source of fuel
Source of Fuel
  • Interstellar gas
  • Infalling stars
  • Remnant of gas cloud which originally formed black hole
  • High accretion rate necessary if z cosmological - not required if nearby
the big bang and redshift
The Big Bang and Redshift
  • All galaxies are moving

away from us.

  • This is consistent with

an expanding Universe,

following its creation

in the Big Bang.

cosmological redshift
Cosmological Redshift
  • Continuity in luminosity from Seyferts to quasars
  • Absorption lines in optical spectra of quasars with

flux

l

alternative models
Alternative Models
  • Supermassive star - 10 solar mass star radiating at 10 J/s or less does not violate Eddington limit. It would be unstable however on a timescale of approx 10 million years.
  • May be stabilized by rapid rotation => ‘spinar’ - like a scaled-up pulsar

8

39

slide22
Also, general relativity predicts additional instability and star evolves into black hole.
  • Starburst nuclei - a dense cluster of massive, rapidly evolving stars lies in the nucleus, undergoing many SN explosions.
  • Explains luminosity and spectra of low-luminosity AGN
slide23
BUT SN phase will be short (about 1 million years) then evolves to black hole
  • radio observations demonstrate well-ordered motions (i.e. jets!) which are hard to explain in a model involving random outbursts
radio sources
Radio Sources
  • Only few % of galaxies contain AGN
  • At low luminosities => radio galaxies
  • Radio galaxies have powerful radio emission - usually found in ellipticals
  • RG 10 - 10 erg/s = 10 - 10 J/s
  • Quasars 10 - 10 erg/s = 10 - 10 J/s

38

43

31

36

43

47

36

40

radio galaxies and jets

150 kPc

Radio Lobes

Radio Lobes

5.7 MPc

Radio Galaxies and Jets
  • Cygnus-A →
  • VLA radio image at
  • n = 1.4.109 Hz
  • the closest powerful
  • radio galaxy
  • (d = 190 MPc)

← 3C 236 Westerbork radio image

at n = 6.08.108 Hz – a radio

galaxy of very large extent

(d = 490 MPc)

Jets, emanating from a central highly

active galaxy, are due to relativistic

electrons that fill the lobes

jets focussed streams of ionized gas

lobe

jet

energy carried out along channels

material flows back towards galaxy

hot spot

Jets: Focussed Streams of Ionized Gas
electron lifetimes
Electron lifetimes

For Synchrotron radiation by electrons:

Calculating the lifetimes in AGN radio jets.

If nm = 10 Hz (radio) ~ 4.17x10 E B

E B = 2.5x10 (J Tesla)

tsyn= 5x10 B E sec

For B = 10 Tesla, t ~3x10 sec, ~ 1 month

For B = 10 Tesla, t ~ 10 sec, ~ 3x10 yrs

36

2

8

2

2

-29

-13

-2

-1

-3

6

syn

-8

14

6

syn

shock waves in jets
Shock waves in jets

Lifetimes short compared to extent of jets => additional acceleration required. Most jet energy is ordered kinetic energy.

Gas flow in jet is supersonic; near hot spot gas decelerates suddenly => shock wave forms. Energy now in relativistic e- and mag field.

equipartition of energy
Equipartition of energy

Relative contributions of energy

What are relative contributions for minimum energy content of the source?

Energy in source

particles

magnetic field

slide30
Assume electrons distributed in energy according to power-law:

Total energy density in electrons,

Must express k and E as functions of B.

max

slide32
Hence:

So:

and the total energy density in electrons

then becomes:

finding e max
Finding Emax

Find E by looking for n :

max

max

So:

slide34
The energy density in the magnetic field is:

Thus total energy density in source is:

For T to be minimum with respect to B:

slide35
Thus:

So:

particle

magnetic field

slide36
And finally,

This corresponds to saying that the minimum energy requirement implies approximate equality of magnetic and relativistic particle energy or equipartition.

energy density in particles

energy density in magnetic field

equipartition in radio sources
Equipartition in Radio Sources

For Cygnus A → Lradio ~ 5.1037 J/s

  • If dlobe ~ 75 kPc = 2.3.1021 m and vjet ~ 103 km/s, then

tlife ~ 2.3.1021/106 = 2.3.1015 s ~ 7.107 years

  • Rlobe ~ 35 kPc = 1021 m and hence Vlobe = 4/3 p Rlobe3

= 5.1063 m3

  • Total energy requirement ~ 5.1037 x 2.3.1015 ~ 1053 J

and energy density ~ 1053/1064 = 10-11 J/m3

  • So from equipartition → B2/2mo ~ 10-11 or B ~ 5.10-9 Tesla
slide38

11

Maximum frequency observed is 10 Hz.

Thus electron acceleration is required in the lobes.

relativistic beaming
Relativistic Beaming

Plasma appears to radiate preferentially along its direction of motion:

Thus observer sees only jet pointing towards her - other jet is invisible.

Photons emitted in a

cone of radiation and

Doppler boosted

towards observer.

jet collimation
Jet collimation
  • Nozzle mechanism hot gas inside large, cooler cloud which is spinning: hot gas escapes along route of least resistance = rotation axis => collimated jet
  • But VLBI implies cloud small and dense and overpredicts X-ray emission
supermassive black hole
Supermassive Black Hole
  • Black hole surrounded by accretion disk
  • Disk feeds jets and powers them by releasing gravitational energy
  • Black hole is spinning => jets are formed parallel to the spin axis, perhaps confined by magnetic field
geometrically thick disk
Geometrically-thick disk
  • Black hole + disk; acc rate > Eddington
  • Disk puffs up due to radiation pressure
  • Torus forms in inner region which powers and collimates jets
  • Predicted optical/UV too high however, but still viable
slide44

Q 4.d) If the high energy electron spectrum in the galaxy is of the formN(E)  E-3/2, express the ratio of Inverse Compton-produced to Synchrotron-produced X-ray intensities in terms of gIC and gSynch.

Ratio = (no of electrons with )

(no of electrons with )

But:

Hence IIC/ISynch = [gIC/gSynch]2-3/2 = [gIC/gSynch]1/2

more about accretion disks

Q

Q

More about Accretion Disks
  • If n is the kinematic viscosity
  • for rings of gas rotating,
  • the viscous torque
  • exerted by the outer
  • ring on the inner will be
  • Q(R) = 2pR nS R2 (dW/dR) (1)
  • where the viscous force per unit length is acting on 2pR and
  • = Hr is the surface density with H (scale height) measured

in the z direction.

Disk self-gravitation is negligible so material in differential or

Keplerian rotation with angular velocity WK(R) = (GM/R3)1/2

more about accretion disks cont
More about Accretion Disks (Cont.)

The viscous torques cause energy dissipation of Q W dR/ring

Each ring has two plane faces of area 4pRdR, so the radiative dissipation from the disc per unit area is from (1):

D(R) = Q(R) W/4pR = ½ n S (RW)2 (2)

and since

W = WK = (G M/R3)1/2

differentiate and then

D(R) = 9/8 n S Q(R) M/R3 (3)

more about accretion disks cont47

From a consideration of radial mass and angular momentum

flow in the disk, it can be shown (Frank, King & Raine, 3rd

ed., sec 5.3/p 85, 2002) that

nS = (M/3p) [1 – (R*/R)1/2]

where M is the accretion rate and from (2) and (3) we then

have

D(R) = (3G M M/8pR3) [1 – (R*/R)1/2]

and hence the radiation energy flux through the disk faces is

independent of viscosity

More about Accretion Disks (Cont.)

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