Blazars & GRBsBlazars & GRBs
Gabriele GhiselliniINAF-Osservatorio di INAF-Osservatorio di
BreraBrera
The fastest macroscopic The fastest macroscopic objects of the Universeobjects of the Universe
Torus ~1-10 Torus ~1-10 pcpc
Broad Line Broad Line Region ~0.2 pcRegion ~0.2 pc
Within RWithin RBLRBLR
UUBLRBLR= const= const
Within RWithin RTorusTorus
UUIRIR= const= const
RBLR
RTorus
dis
diskk
Big blazarsBig blazarsL>0.01LL>0.01LEdEd
dd
BLR <<0.2 BLR <<0.2 pcpc
weak weak coolingcooling
SSC onlySSC only
““ADAF d
isk”
ADAF d
isk”
L<0.01LL<0.01LEdEd
dd
BL LacsBL Lacs
Rdiss
FSRQs: emission FSRQs: emission lineslines many seed many seed photonsphotons
BL Lacs: no or BL Lacs: no or weak linesweak lines
Collimation Collimation correctedcorrected
Colli
mati
on
Colli
mati
on
corr
ect
ed
corr
ect
ed
Nem
men
+ S
cie
nce
Nem
men
+ S
cie
nce
2012
2012
blazarsblazars
GRBsGRBs
nnoo
RR
Jet opacity: blazarsJet opacity: blazars
nno o from Mfrom Mout out
~ 0.5~ 0.5 1 P1 Pjetjet
11 L LEddEdd
Jet opacity: GRBsJet opacity: GRBs
aTaT0044
kTkT00
~ n~ n+ +
~~
PPjet,51jet,51
MM11
10101515
1/21/2
3/43/4
Jet launchingJet launching
In GRBs we have 2 possibilities:In GRBs we have 2 possibilities:- internal pressure: - internal pressure: the huge optical depth traps the huge optical depth traps photons inside photons inside - magnetic field- magnetic field
In blazars:In blazars:- internal pressure: - internal pressure: the optical depth is smallthe optical depth is small- magnetic field- magnetic field
Jet launchingJet launching
In GRBs we have 2 possibilities:In GRBs we have 2 possibilities:- internal pressure: - internal pressure: the huge optical depth traps the huge optical depth traps photons inside photons inside - magnetic field- magnetic field
In blazars:In blazars:- internal pressure: - internal pressure: the optical depth is smallthe optical depth is small- magnetic field- magnetic field
Magnetic field:Magnetic field:- Produced and amplified by the disk- Produced and amplified by the disk- Link with accretion - Link with accretion
Blandford & ZnajekBlandford & Znajek U UBB ~ ~ cc2 2 @ @ RRs s
This explains why PThis explains why Pjj ~ L ~ Ldd
B ~ 10B ~ 101515-10-101616 G in GRBs G in GRBsB ~ 10B ~ 1044 G in blazars G in blazarsB ~ 10B ~ 1099 G in galactic superluminals G in galactic superluminals
Fermi Fermi FSRQsFSRQs
Power in cold protons Power in cold protons (1 per emitting e-)(1 per emitting e-)
Power in rel. Power in rel. electronselectrons
Power in Poynting Power in Poynting fluxflux
Power in radiation Power in radiation ((model indipendentmodel indipendent))
Disk luminosityDisk luminosity
MMoutout /M/Min in for blazars and for for blazars and for
GRBsGRBsPPjetjet = = MMoutoutcc
22
LLdd = = MMinincc22for for blazars:blazars:
MMoutout /M/Min in for blazars and for for blazars and for
GRBsGRBsPPjetjet = = MMoutoutcc
22
LLdd = = MMinincc22for for blazars:blazars:
PPjetjet
LLd d
MMouou
t t MMin in
== ~ 10~ 10--
22
blazarsblazars
MMoutout /M/Min in for blazars and for for blazars and for
GRBsGRBsPPjetjet = = MMoutoutcc
22
LLdd = = MMinincc22for for blazars:blazars:
for for GRBs:GRBs:
MMin in
~~
0.1 M0.1 MOO
ttburstburst
PPjetjet
LLd d
MMouou
t t MMin in
==
MMouou
t t MMin in
==cc22 0.1 0.1 MMOO
EEkk~ 5.5x10~ 5.5x10-4-4
22
EEk5k5
22
~ 10~ 10--
22
blazarsblazars
Blazars: the Blazars: the redder redder the more powerful the more powerful coolingcooling
GRBs: the GRBs: the bluer bluer the more the more powerfulpowerful heating?? heating?? ??
““Amati
Amati
””““G
hir
land
Ghir
land
a”a”
EEp
eak
p
eak
[keV
][k
eV
]
EE [erg][erg]
ConclusionsConclusions
Jets are the most efficient Jets are the most efficient engine of Natureengine of Nature
Compare jet power and LCompare jet power and Ldiskdisk
as a function of the accretion as a function of the accretion rate. Normalize to Eddington.rate. Normalize to Eddington.
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
TheThe “blazar“blazar sequence”sequence”FSRQs
BL LacsBL Lacs
BATBAT
IntegraIntegrall
FSRQsFSRQs
BL LacsBL Lacs
Lin
e
Lin
e
stre
ng
thst
ren
gth
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
FSRQsFSRQs
BL LacsBL Lacs
M/M
M/M
Edd
Edd
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
Next talk by M
eyer
Next talk by M
eyer
Sb
arr
ato
+ 2
01
1S
barr
ato
+ 2
01
1
SDSS+1LACSDSS+1LAC
Do we really need to divide blazars?Do we really need to divide blazars?
5x105x10--
44
EW<5A
EW>5A
Narayan & Yi 1995: LBLR/LEdd ~
10-3
Sharma+ 2007: LBLR/LEdd ~ 10-
5
M-M- Plotkin+ Plotkin+ 20112011
UVOTUVOT
XRTXRT
FermiFermi
GG
, Tavecch
io &
Gh
irla
nd
a 2
009
GG
, Tavecch
io &
Gh
irla
nd
a 2
009
Low energy synchro Low energy synchro peak: leave the disk peak: leave the disk naked!naked!
torus disk X-ray
corona
synchrsynchroo
SSC
SSC
EECC
MM BHBH=2x1
0
=2x10
99
The jet cannot have less power than what The jet cannot have less power than what required to produce the observed required to produce the observed luminosity:luminosity:
PPjetjetLLobsobs
22>>
If PIf Pjetjet is twice as much, is twice as much, halves. halves.
We can take that as the minimum PWe can take that as the minimum Pjet.jet.
This limit is model-independent.This limit is model-independent.
1 proton per electron 1 proton per electron no no pairspairs
Having pairs would reduce PHaving pairs would reduce Pjetjet. .
But where are they created?But where are they created?
PausePause
• PPjetjet ~ Mc ~ Mc22,, even larger than Leven larger than Ldd
• For For all all M/MM/MEddEdd
• BL LacsBL Lacs ADAF ADAF FSRQs FSRQs SS SS
• LLBLRBLR/L/LEddEdd divides divides BL Lacs BL Lacs from FSRQsfrom FSRQs
• Matter, not magnetic, dominated Matter, not magnetic, dominated
PPr r = radiation ~ = radiation ~
LLobsobs//22PPe e = relat. = relat.
electronselectronsPPp p = protons= protons
PPB B = B-field= B-field RR
jet power and accretion jet power and accretion luminosityluminosity
~1017 cm
Shakura-Sunjaev disk: Ld
Pjet = Pe+Pp+PB
What is a blazar?What is a blazar?
A jetted AGN, whose jet is relativistic A jetted AGN, whose jet is relativistic ((~10) and is “pointing at us”.~10) and is “pointing at us”.
To be more quantitative:To be more quantitative:
viewview
For each blazar, For each blazar, 2222 radio-loud AGN radio-loud AGN pointing elsewhere: FR I and FRII radio-pointing elsewhere: FR I and FRII radio-galaxiesgalaxies
3 months, 10 3 months, 10
BL LacsBL LacsFlatFlat
SteepSteep FSRQsFSRQs
LL
Fossati
et
al.
1998;
Don
ato
et
al.
Fossati
et
al.
1998;
Don
ato
et
al.
2001
2001
M/M/MM EddEdd
GG
, M
ara
sch
i, T
avecc
hio
200
9G
G,
Mara
sch
i, T
avecc
hio
200
9
2 years– 4Ackermann+ 2011