Benvenuti al Mera-TeV! 4-5-6 Ottobre 2011 Sala “POE” di OAB a Merate Sala “POE” di OAB a...

Benvenuti al Mera-TeV!

4-5-6 Ottobre 2011 4-5-6 Ottobre 2011 Sala “POE” di OAB a MerateSala “POE” di OAB a Merate

Lorenzo SironiLorenzo Sironi

FATE DOMANDE!FATE DOMANDE!

• Le domande sono gradite, anche prima della fine dei contributi.

• L'incontro è volutamente informale, e lo spirito è orientato alla

comprensione delle tematiche ed alla interazione tra i partecipanti.

SOCIAL EVENTSOCIAL EVENT

ww

Visita alle Cupole Zeiss e Ruths:Visita alle Cupole Zeiss e Ruths: Mercoledì 5, ore 18.15Mercoledì 5, ore 18.15

SOCIAL DINNERSOCIAL DINNER

• Taverna dei Cacciatori – Imbersago

• Ore 20.00 Mercoledì

• Partenza da Osservatorio ore 19.45

Pranzi e Pause Caffè Pranzi e Pause Caffè

Pranzi: alle 13.00 nel parco, di fronte alla Cupola Ruths

Coffe Breaks: nella Biblioteca, piano seminterrato edificio principale.

Buon Mera-TeV!!Buon Mera-TeV!!

BeamingBeaming

Radio-loud Radio-loud AGNsAGNs

Gamma Ray Gamma Ray BurstsBursts

~ 0.1 M~ 0.1 Moo yr yr-1-1

~20~20

~ 10~ 10-5-5 M Moo

in a few in a few sec sec ~300~300

Lorentz transformations: v Lorentz transformations: v along x along x

x’ = x’ = (x – vt) (x – vt)

y’ = yy’ = y

z’ = zz’ = z

t’ = t’ = (t – v (t – v x/cx/c22))

for for t = 0t = 0 x = x = x’/x’/ContractionContraction

for for x’ = 0x’ = 0 t = t = t’t’ time time dilationdilation

Text book special Text book special relativity relativity

x = x = (x’ + vt’) (x’ + vt’)

y = y’y = y’

z = z’z = z’

t = t = (t’ + v (t’ + v x’/cx’/c22))

To remember: mesons created at a height of ~15 km can reach the earth, even if their lifetime is a few microsec ct’life=hundreds of meters.

v=0 v=0 =1=1

v=0.866c v=0.866c =2=2

vv

Can we see contracted Can we see contracted spheres?spheres?

Einstein: Einstein: Yes!Yes!

James Terrel 1959James Terrel 1959

Roger Penrose Roger Penrose 19591959

v=0 v=0 =1=1

vv

NO!NO!

v=0.866c v=0.866c =2=2

Rotatio

n, not

Rotatio

n, not

contra

ctio

n!

contra

ctio

n!

Relativity with Relativity with photonsphotons

From rulers and clocksFrom rulers and clocks

to photographs and to photographs and frequenciesfrequencies

Or:Or:

from elementary particles to extended from elementary particles to extended objectsobjects

The moving squareThe moving square

==00=0.5=0.5

Your Your camera, very camera, very far awayfar away

The moving squareThe moving square

t=l’/ct=l’/c

vt=vt=l’l’

l’/l’/

lltottot = l’ ( = l’ (+1/+1/))

max:2max:21/21/2l’ (diag)l’ (diag)

min: l’ (for min: l’ (for =0)=0)

l’l’

l’cosl’cos = = l’ l’ coscos==

coscossinsin

TimeTime

CD = cCD = cttee – c – ctteecoscos

ttAA= = tte e (1-(1-coscos) )

ttAA= = ttee’ ’ (1-(1-

coscos) )

tte e = emission time in lab = emission time in lab

frame frame ttee’ = emission time in ’ = emission time in

comov. frame comov. frame tte e = = ttee’ ’

Relativistic Doppler Relativistic Doppler

factor factor ttAA= = ttee’ ’ (1-(1-coscos) ) = = ’ / ’ / (1-(1-coscos) )

==

11

(1-(1-coscos))

StandarStandard d relativitrelativityy

Doppler Doppler effecteffect

You change frame

You remain in lab frame

Relativistic Doppler Relativistic Doppler

factor factor

==

11

(1-(1-coscos))

22 for for =0=0oo for for =1/=1/foforr

==At small angles, Doppler wins over Spec. At small angles, Doppler wins over Spec. Relat.Relat.

25 light y

ears in

3 years… th

e

25 light y

ears in

3 years… th

e

velocity is

8.3 c

velocity is

8.3 c

Nucleo

v=0.99c

appapp = = sinsin

1-1-coscos

==vvappapp

= =

vvtteesinsinttee (1- (1-coscos))

ssappapp

ttAA

=0=0oo appapp=0=0

coscos==; ; sinsin=1/=1/

appapp==

=90=90oo appapp==

There is no There is no Correct?Correct?

Aberration of lightAberration of light


sinsin = sin = sin’/’/

dd==dd’/’/22

sinsin = = sinsin’/’/


KK’’

dd= = dd’/’/22

KK

vv

Observed vs intrinsic Observed vs intrinsic IntensityIntensity

33I’(I’(’’))

I(I())

I’(I’(’)’)

’’== ==invariainvaria

ntntI(I())==

I(I())cmcm2 2 s Hz s Hz steradsterad

==ergerg

==dAdA dt ddt d d d

EE

Observed vs intrinsic Observed vs intrinsic IntensityIntensity

33I’(I’(’’))

I(I())

I’(I’(’)’)

’’== ==invariainvaria

ntntI(I())==

I(I())cmcm2 2 s Hz s Hz steradsterad

==ergerg

==dA’dA’ dd’’//22

E’E’33I’(I’(’’))

==

II 44I’I’==

FF 44FF’’

==

blueshiftblueshift timetime22 aberration aberration

v=0

L=100 W

v=0.995c =10

L=16MW

L=10mW

L=0.6mW

v=0.995c =10

blazars

radiogalaxies

…….?

v=0.995c =10

blazars

radiogalaxies

blazars!

jet

counterjet (invisible)

v

v

Radiation Radiation processesprocesses

Radiation processesRadiation processes

Line emission and radiative transitions in atoms Line emission and radiative transitions in atoms and moleculesand molecules

Breemstrahlung/BlackbodyBreemstrahlung/Blackbody

Curvature radiationCurvature radiation

CherenkovCherenkov

AnnihilationAnnihilation

Unruh radiationUnruh radiation

Hawking radiationHawking radiation

SynchrotronSynchrotron

Inverse ComptonInverse Compton

V=0V=0EE

V

((=2))

Charge at Charge at time 9.00time 9.00

Contracted sphere…Contracted sphere… E-field lines at time E-field lines at time 9.00 point to… where 9.00 point to… where the charge is at 9.00the charge is at 9.00

EE

Breaking news: what happens with the gravitational field?Breaking news: what happens with the gravitational field?

dP = edP = e22aa22 sinsin22

dd44cc33

VV

http://www.cco.caltech.edu/~phys1/java/phys1/MovingCharge/MovingCharge.html

Stop at Stop at 8:008:00

dP = edP = e22aa22 sinsin22

dd44cc33

P = 2 eP = 2 e22aa22

33cc33

SynchrotronSynchrotron

Synchrotron Synchrotron Ingredients: Magnetic Ingredients: Magnetic field and relativistic field and relativistic chargescharges

Responsible: Lorentz Responsible: Lorentz forceforce

Curiously, the Lorentz Curiously, the Lorentz force doesn’t work.force doesn’t work.FFLL = = dd

dtdt ((mmv)v)

== eecc

v x Bv x B

Total losses Total losses

PPee = P’ = P’ee

Please, PPlease, Pee is not is not

PPreceivedreceived!!!!

P=E/t and E and t Lorentz P=E/t and E and t Lorentz transform in the same waytransform in the same way

Total Total losses losses 2e2e22

==

3c3c33a’a’22

==

2e2e22

3c3c33(a’(a’22 + a’ + a’22 ) )PPee = =

P’P’ee

Total Total losses losses


==

2e2e22

3c3c33aa2222

2e2e22==

3c3c33a’a’22

==

2e2e22

3c3c33(a’(a’22 + a’ + a’22 ) )PPee = =

P’P’ee

a’a’ = = 22a a

aa’’|||| = = 00

a = a = e v B sine v B sin

mcmc



==

2e2e22

3c3c33aa2222

2e2e22==

3c3c33a’a’22

==

2e2e22

3c3c33(a’(a’22 + a’ + a’22 ) )PPee = =

P’P’ee

a’a’ = = 22a a

aa’’|||| = = 00


mcmc

PPSS(() ) ==

2e2e44

3m3m22cc33

BB222 2 2 2

sinsin22



==

2e2e22

3c3c33aa2222

2e2e22==

3c3c33a’a’22

==

2e2e22

3c3c33(a’(a’22 + a’ + a’22 ) )PPee = =

P’P’ee

a’a’ = = 22a a

aa’’|||| = = 00


mcmc

PPSS(() ) ==

2e2e44

3m3m22cc33

BB222 2 2 2

sinsin22

PPSS(() ) ==

22TTcUcUBB2 2 2 2

sinsin22



==

2e2e22

3c3c33aa2222

2e2e22==

3c3c33a’a’22

==

2e2e22

3c3c33(a’(a’22 + a’ + a’22 ) )PPee = =

P’P’ee

a’a’ = = 22a a

aa’’|||| = = 00


mcmc

PPSS(() ) ==

2e2e44

3m3m22cc33

BB222 2 2 2

sinsin22

PPSS(() ) ==

22TTcUcUBB2 2 2 2

sinsin22<P<PSS> >

==4 4 TTcUcUBB

2 2 22

33

If pitch angles are If pitch angles are isotropicisotropic

Log ELog E

Log

Log

PP

SS

vv2 2 ~ E~ E

~ ~

EE22

Why Why 22????

PPSS(() ) ==

22TTUUBB2 2 2 2

sinsin22What happens when What happens when 0 ?0 ?Sure, but what happens Sure, but what happens to the to the receivedreceived power if power if you are in the beam of you are in the beam of the particles?the particles?

mcmc22 sin sineBeB

rrLL ==vv22

aa==

e e BB mmcc

==BB = 1/T T = 1/T T = 2= 2 r rLL/v/v

Synchrotron Synchrotron SpectrumSpectrumCharacteristic Characteristic

frequencyfrequency

This This is notis not the characteristic the characteristic frequencyfrequency

e v B sine v B sin

mcmca =a =

v<<cv<<c

v ~ cv ~ c

ttAA = ? = ?

SS = =

1

ttAA

== 22

eeBB22mcmc

Compare with Compare with B. B. S S = = BB 33

The real stuffThe real stuff

x=

x1/3

The real stuffThe real stuff

x=

Max synchro frequencyMax synchro frequencyGuilbert Fabian Rees 1983Guilbert Fabian Rees 1983

shockshock

ttsynsyn = T = T 66mmeecc22TTBB2222

==22 m mee

cc eBeB

maxmax ~~ BB1/21/2

11

hhS,maxS,max ~ B ~ B maxmax = m = meecc22//FF = 70 MeV = 70 MeV..

22

(+ beaming)(+ beaming)

Emission from many Emission from many particlesparticles

N(N() = K) = K-p-p The queen of The queen of relativistic relativistic distributionsdistributions

Log

N

()

Log Log

Log

)

(() ) dd= =

11

44N(N() P) PSS

dd



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44KK-p-p B B2222 d d

dd

Emission is Emission is peaked! peaked!

SS ==22eeBB22mm

cc

dd dd



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44K BK B(1+p)/2 (1+p)/2 (1-p)/2(1-p)/2



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44 K BK B+1 +1 --

==p-1p-1

22

power

power

lawlaw

power power lawlaw

(() ) ~ ~ 11

44 K BK B+1 +1 --

So, what?So, what?

44Vol Vol (() ) ~~ss

2 2 R R K BK B+1+1 --

F(F() ) ~ ~ 44dd22

Log

Log

F

)

K K

BB+1+1 If you know s and R

Two unknowns, one equation… we need another one

Synchrotron self-Synchrotron self-absorptionabsorption

• If you can emit you can also absorbIf you can emit you can also absorb• Synchrotron is no exceptionSynchrotron is no exception• With Maxwellians it would be easy With Maxwellians it would be easy

(Kirchhoff law) to get the absorption (Kirchhoff law) to get the absorption coefficientcoefficient

• But with power laws?But with power laws?• Help: electrons able to emit Help: electrons able to emit are also are also

the ones that can absorb the ones that can absorb

A useful trickA useful trick

-p-p

Many Many Maxwellians Maxwellians with with kT=kT=mcmc22

I(I() = 2 ) = 2 kTkT 22/c/c22

= 2 = 2 mcmc2222/c/c22

Log Log

Log

Log

N

(N

(

==22eeBB22mm

cc

~ (B)B)1/21/2 5/25/2

BB1/21/2~~ There is no K There is no K

!!

From data to physical From data to physical parametersparameters

get Bget B insert B insert B and get Kand get K

t belongs to thick

and thin part. Then in principle one observation is enough

Inverse Inverse ComptonCompton

Inverse ComptonInverse Compton Scattering is one the basic interactions Scattering is one the basic interactions

between matter and radiation.between matter and radiation. At low photon frequencies it is a At low photon frequencies it is a

classical process (i.e. classical process (i.e. e.m. wavese.m. waves)) At low frequencies the cross section is At low frequencies the cross section is

called the Thomson cross section, and it called the Thomson cross section, and it is a peanut.is a peanut.

At high energies the electron recoils, At high energies the electron recoils, and the cross section is the Klein-and the cross section is the Klein-Nishina one.Nishina one.

= scattering = scattering angleangle

00

11

Thomson scatteringThomson scattering

• hvhv00 << m << meecc22

• tennis ball against a wall tennis ball against a wall

• The wall doesn’t moveThe wall doesn’t move

• The ball bounces back with the same The ball bounces back with the same speed (if it is elastic)speed (if it is elastic)

11= = 00

Thomson cross sectionThomson cross section

ddTT

dd==

rr0022

22(1+cos(1+cos22))

TT == rr0022

3388

==rr00mmeecc22

ee22

a a peanutpeanut

Hurry up!

Hurry up!

Why a peanut?Why a peanut?


E

B


dd

dP dP ee22aa22

44cc33

sinsin22==RemembRemember:er:

EE

BB

ddTT

dd==

rr0022

22(1+cos(1+cos22))

1122

100%

100%

P

ol

Pol

no no PolPol

Direct ComptonDirect Compton

xx11 = = xx00

1+x1+x00(1-(1-

coscos))

x = x = hh

mmeecc22

xx00

xx11

Klein-Nishina cross sectionKlein-Nishina cross section

Klein-Nishina cross Klein-Nishina cross sectionsection

~ E~ E-1-1

Klein-Nishina cross Klein-Nishina cross sectionsection

Inverse Compton: typical Inverse Compton: typical frequencies frequencies Thomson regimeThomson regime

Rest frame K’

x’x’11=x’=x’

xxx’x’

xx11

Lab frame K

Min and max frequenciesMin and max frequencies

==180180oo 11=0=0o o

xx11=4=422

xx

==00oo 11=180=180o o

xx11=x/4=x/422

Total loss rateTotal loss rate

vtvtTT

Everything in the lab frameEverything in the lab frame

n(n() = density of seed photons of energy ) = density of seed photons of energy =h=h

vvrelrel = “relative velocity” between photon and = “relative velocity” between photon and

electron velectron vrelrel = c-vcos = c-vcosc(1-c(1-coscos))

Hurry up!

Hurry up!


vtvtTT

There are many There are many 11, because there are many , because there are many

11.. We must average the term 1-.. We must average the term 1-coscos11, ,

getting getting

Hurry up!

Hurry up!


There are many There are many 11, because there are many , because there are many

11.. We must average the term 1-.. We must average the term 1-coscos11, ,

getting getting

UUradrad

{{

Hurry up!

Hurry up!


If seed are isotropic, average over If seed are isotropic, average over and and take out the power of the incoming take out the power of the incoming radiation, to get the net electron losses:radiation, to get the net electron losses:

UUradrad

{{

<P<Pcc> => = 4 4 TTccUUradrad2 2 22

33

<P<PSS> >

==4 4 TTccUUBB

2 2 2 2

33

Compare with Compare with synchrotron synchrotron losses:losses:

Hurry up!

Hurry up!

Inverse Compton Inverse Compton spectrum spectrum

The typical frequency The typical frequency is: is:

Going to the rest frame of the e- we see Going to the rest frame of the e- we see 00

There the scattered radiation is There the scattered radiation is isotropizedisotropized

Going back to lab we add another Going back to lab we add another --factor.factor.

The real stuffThe real stuffdowdownn

upscatteriupscatteringng

The real stuffThe real stuffdowdownn

upscatteriupscatteringng

75%75%



Log

N

()

Log Log

Log

)

(() ) dd= =

11

44N(N() P) PCC

dd

Hurry up!

Hurry up!



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44KK-p-p U Uradrad22 d d

dd

Emission is Emission is peaked! peaked!

dd dd

44== 2 2 00

33

Hurry up!

Hurry up!



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44KUKUradrad (2-p)/2(2-p)/2 -1/2-1/2

Hurry up!

Hurry up!



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44 KUKUradrad --

==p-1p-1

22

power

power

lawlaw

power power lawlaw

Hurry up!

Hurry up!

Synchrotron Self Compton: Synchrotron Self Compton: SSCSSC

Due to synchro, Due to synchro, then proportional then proportional to: to:

cc B B+1 +1 --

cc(() ) ~ ~

22cc B B+1 +1 cc

-- Electrons work Electrons work twice twice

EndEnd

The moving barThe moving bar

app ~ 30

Gravity bends Gravity bends spacespace

There is max frequency of synchro radiation produced by shock-accelerated There is max frequency of synchro radiation produced by shock-accelerated electrons. Even if we have relativistic shocks, so that electrons. Even if we have relativistic shocks, so that can be ~1 for each can be ~1 for each passage through the shock, there is a max energy attainable which corresponds to passage through the shock, there is a max energy attainable which corresponds to a a ee for which for which

ttsynsyn [propto 1/( [propto 1/(eeBB22)] is comparable to the gyroperiod (propto )] is comparable to the gyroperiod (propto ee/B). /B).

This gives a max This gives a max ee scaling as 1/B scaling as 1/B1/21/2, ,

so that so that SS becomes independent of B becomes independent of B and which corresponds to a wavelength and which corresponds to a wavelength

ee22/m/meecc22=classical electron radius: i.e. a photon of energy =classical electron radius: i.e. a photon of energy

hhS,maxS,max = m = meecc22//FF = 70 MeV = 70 MeV..

Max synchro frequencyMax synchro frequencyGuilbert Fabian Rees 1983Guilbert Fabian Rees 1983

FFLL = = dd

dtdt ((mmv)v)

== eecc

v x Bv x B

PPSS(() ) ==

2e2e44

3m3m22cc33

BB222 2 2 2

sinsin22

PPSS(() ) ==

22TTcUcUBB2 2 2 2

sinsin22

rr00=e=e22/m/meecc22

TT = 8 = 8rr00/3/322

<P<PSS> >

==4 4 TTcUcUBB

2 2 22

33If pitch angles If pitch angles are isotropicare isotropic

=pitch =pitch angleangle

~constant, at ~constant, at least for one least for one gyroradius gyroradius

aa|| || = 0= 0

a = a = e v B sine v B sin mcmc

FFLL = = dd

dtdt ((mmv)v)

== eecc

v x Bv x B

PPSS(() ) ==

2e2e44

3m3m22cc33

BB222 2 22

sinsin22

PPSS(() ) ==

22TTcUcUBB2 2 22

sinsin22

rr00=e=e22/m/meecc22

TT = 8 = 8rr00/3/322

<P<PSS> >

==4 4 TTcUcUBB

2 2 22

33If pitch angles If pitch angles are isotropicare isotropic

a = a = e v B sine v B sin mcmc



Log

N

()

Log Log

Log

)

(() ) ~ ~ 11

44K BK B2 2 (2-p)/2(2-p)/2 -1/2-1/2

BB1/2 1/2 BB(2-p)/2 (2-p)/2

Benvenuti al Mera-TeV! 4-5-6 Ottobre 2011 Sala “POE” di OAB a Merate Sala “POE” di OAB a...

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