almost every galaxy hosts a bh 99% are silent 1% are active 0.1% have jets extragalactic jets: a new...
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Almost every galaxy hosts a BHAlmost every galaxy hosts a BH
99% are silent99% are silent
1% are active1% are active
0.1% have jets0.1% have jets
Extragalactic jets: a new Extragalactic jets: a new perspectiveperspective
G. Ghisellini in coll. with F. Tavecchio INAF-OABreraG. Ghisellini in coll. with F. Tavecchio INAF-OABrera
SynchrSynchroo
Inverse Inverse ComptonCompton(also possible(also possiblehadronic hadronic models)models)
Radio IR Opt UV X MeV Radio IR Opt UV X MeV GeV GeV
Blazars: Spectral Energy DistributionBlazars: Spectral Energy Distribution
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 LacsLBLLBL and and HBLHBL
By By modeling, modeling, we find we find physical physical parameters parameters in the in the comoving comoving frame.frame.
peakpeak is the is the
energy of energy of electrons electrons emitting at emitting at the peak of the peak of the SEDthe SED
EGRET EGRET blazarsblazars
TeV BL LacsTeV BL Lacs
Low power slow cooling large peak
Big power Big power fast fast cooling cooling small small peakpeak
Power of Power of jets in jets in blazarsblazars
……and X-ray and X-ray cavities,cavities,
Allen+, 2006, Allen+, 2006, Balmaverde+, Balmaverde+, 20082008
Power of Power of jets in jets in blazarsblazars
Tavecchio+ Tavecchio+ 20002000
Celotti, GG 2001Celotti, GG 2001
PPr r = radiation= radiation
PPe e = relat. = relat.
electronselectronsPPp p = protons= protons
PPB B = B-field= B-field RR
The power of blazar jetsThe power of blazar jets
Rdiss ~1017 cm
Ghisellini, Foschini, Tavecchio, Pian Ghisellini, Foschini, Tavecchio, Pian 20072007
AGILEAGILE!!3C 454.3 3C 454.3
SwifSwiftt
If one p per e-If one p per e-
Relat. Relat. electronselectrons
Magnetic FieldMagnetic Field
RadiationRadiation
Celo
tti &
Gh
isellin
i C
elo
tti &
Gh
isellin
i 2007
2007
High High powerpower
Powerful je
ts are
not
Powerful je
ts are
not
magnetically
dominated
magnetically
dominated
Celotti GG 2008Celotti GG 2008
Celo
tti G
G 2
008,
Mara
sch
i et
al.
C
elo
tti G
G 2
008,
Mara
sch
i et
al.
2008
2008
Pje
t
10x
100x
Disk accretion rate (Eddington Disk accretion rate (Eddington units)units)
LLd
isk
dis
k
PPje
tje
tJet power vs disk Lum.Jet power vs disk Lum.
e-p e-p decouplindecoupling g
Photon Photon trappingtrapping
BL Lacs, F
SRQ, QSO
GRBGRB
ss
PausePause
• Jet power is large. More than LJet power is large. More than Ldiskdisk
• Matter dominated. Not many pairsMatter dominated. Not many pairs
• PPBB is small is small
• Powerful jets Powerful jets mustmust be radiatively be radiatively inefficientinefficient
• Powerful jets do not deceleratePowerful jets do not decelerate
A new blazar sequenceA new blazar sequence
• Old one: based on 1 parameter: the observed luminosity
• Now: info on mass and accretion rate (spin? not yet)
• Info on jet power vs disk luminosity• Info on location of dissipation: must
be at some distance from BH. One zone is dominant (internal shocks?)
The key ideasThe key ideas
• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
1/2
The key ideasThe key ideas
• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• PB = B Pjet B propto R-1
• Pe = e Pjet
1/2
The key ideasThe key ideas• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
UBLR=cost
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• PB = B Pjet B propto R-1
• Pe = e Pjet
peak propto U-1; U-1/2
1/2
The key ideasThe key ideas• Rdiss proportional to MBH
• RBLR proportional to (Ldisk)
• For Ldisk/LEdd < Lc no BLR (BL Lacs)
• PB = B Pjet
• Pe = e Pjet
peak propto U-1; U-1/2
The key ansatzThe key ansatz• Pjet always proportional to M
1/2
MM22
MM
ADAFADAF (Narayan et (Narayan et al.)al.)
PPjetjet propto propto
LLdiskdisk
1/21/2
PPjet jet propto propto
LLdiskdisk
Simple consequencesSimple consequences
• RRdissdiss propto M; R propto M; RBLRBLR propto propto
(L(Ldiskdisk))1/21/2
BLRBLR
Low M, High LLow M, High Ldiskdisk Red Red
quasarquasar
High M, Low LHigh M, Low Ldiskdisk Blue Blue
quasarquasar
Simple consequencesSimple consequences
• Small M, small PSmall M, small Pjetjet, large B, red, large B, red
BLRBLR UUBLRBLR ~ the same ~ the same
Large Large UUBB
Give me MGive me MBHBH
and Land Ldiskdisk (or (or
LLBLRBLR) and I will ) and I will
tell you the tell you the SED of the jet SED of the jet and its powerand its power
Reproducing the Reproducing the “old” sequence“old” sequence
ConclusionsConclusions
• PPjetjet > L > Ldiskdisk
• Jets are matter dominatedJets are matter dominated• Link between M, M and observed SEDLink between M, M and observed SED• ““Blue” FSRQs may existBlue” FSRQs may exist• ““Red” low power FSRQs may existRed” low power FSRQs may exist• Implications about evolutionImplications about evolution
• GLAST + Swift + M + LGLAST + Swift + M + Ldiskdisk (or L (or LBLRBLR))
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