ACTIVEGALACTICNUCLEI:SOURCES
FORULTRAHIGHENERGYNEUTRINOS!
PeterL.Biermann
1
,
2
,
3
,
4
,
5
,withJuliaBecker
6
,
7
,and
AthinaMeli
8
1
MPIforRadioastronomy,Bonn,Germany
2
Dept.ofPhys.&Astron.,Univ.ofBonn,Germany
3
Dept.ofPhys.&Astr.,Univ.ofAlabama,Tuscaloosa,
AL,USA
4
Dept.ofPhys.,Univ.ofAlabamaatHuntsville,AL,
USA
5
Inst.Nucl.Phys.FZ,KarlsruheInst.ofTechn.(KIT),
Germany
6
Institutionf¨orFysik,G¨oteborgsUniv.,Sweden
7
Dept.ofPhys.,Univ.Dortmund,Dortmund,Germany
8
ECAP,Friedrich-AlexanderUniversit¨at
Erlangen-Nu¨rnberg,Germany
www.mpifr-bonn.mpg.de/div/theory
1
Sourcesofultrahighenergycosmicrays
•
Threecandidatesourceclasses:
•
(I)Radiogalaxies,andtheirjets
,drawingfrom
theISMandIGM,mostlyHydrogenandHelium
•
(II)Radiogalaxies
,andtheirjets,plowingthrough
WolfRayetstarexplosion
regionsfullofnew
highlyenrichedcosmicrays
•
Thisisthecurrentlybestbettoexplainthe
observedultrahighenergycosmicrays
•
(III)Starburstgalaxies
andtheir
GRBs
•
andasasubset,thestarburstphaseusuallypreceding
theactivityofafreshlyfedsupermassiveblackhole
•
Inallcases,thereshouldbehighenergyneutrinosfrom
interaction,anddecay
2
Ultrahighenergyneutrinos?
BUT:
•
Ifmostultrahighenergycosmicraysheavyions
•
Firstinteractiondoesnotproduceneutrinossodirectly
•
Onlymultiplestageinteractiongivesneutrinos
•
Howdowegetalargefluxofultrahighenergyneutri-
nos?
3
Figure1WRstarexplosionsinothergalaxies.SourceP.P.Kronberg2008
4
Figure2TheradiogalaxyArp220andevolution.SourceLectureS.Britzen
5
Figure3Starformationasfunctionofredshift.SourceLectureS.Britzen
6
360
o
0
o
90
o
?
90
o
MESSIER031
MESSIER033
NGC1569
NGC6946
NGC0055
SMC
MESSIER082
NGC0253
LMC
MESSIER094
CircinusGalaxy
MESSIER051a
NGC0891
NGC2903
NGC4945
MESSIER051
NGC4631
MESSIER066
NGC3628
NGC0660
NGC2146
NGC1808
NGC3079
MESSIER077
NGC1097
NGC7582
NGC7552
NGC1365
NGC3256
ESO173
?
G015
NGC3690
Figure4AitoffprojectioningalacticcoordinatesoftheselectionfromNEDin60
µ
m,redshift
z
≤
0
.
0125,flux
densitybrighterthan50Jy,starburstselected,sampleof32candidatesourcesand100virtualeventsfromthis
sourcesandweightedcontribution.DoubleMonte-CarlotosimulatetheintermittentnatureofGammaRay
Bursts
7
Evolutionofanactivityepisode:
•
Twogalaxiesmerge,bothmayhaveacentralsuper-
massiveblackhole
•
stageI:Feedingacentralstarburst,thestarburstdom-
inatestheenergeticsoftheemission;thisisaccom-
paniedbytheformationofmanymassivestars,Wolf
Rayetstars,theirexplosionsandmanygammaray
bursts
•
stageII:Feedingthecentralblackholes,theblackholes
takesover
•
stageIII:Theblackholesmerge,induceaspin-flip:for
awhilebothjetdirectionsarevisible
•
stageIV:Theactivitydiesdown,reachingalimitwhen
justoneredgiantstarfeedstheblackhole
8
Radiogalaxies,jets,hotspots,shocksand
shear-flowsasacceleratorsandphasemixers
Figure5RadiogalaxiesFR-IandFR-II.SourceLectureS.Britzen
9
Figure6CenAinX-rays.SourceHardcastlepapers
10
360
o
0
o
90
o
?
90
o
Figure7Theskyinsuper-massiveblackholes,
>
3
.
10
8
M
?
:Aitoffprojectioningalacticcoordinatesof528
NEDcandidatesourcesinthecaseofacompletesubsample,massiveBlackHole(M
BH
>
3
∗
10
8
M
?
).The
choicewasmadefromacompletesampleof10,284candidatebrighterthan0.03Jyat2micron,andselected
atz
<
0
.
025:sourceL.Caramete
11
360
o
0
o
90
o
?
90
o
NGC5128
?
CenA
?
NGC4374
?
M84
?
NGC4486
?
M87
?
NGC1052
IC1459
NGC4261
NGC4696
NGC5090
IC4296
NGC4782
?
3
NGC1316
?
FornaxA
?
Figure8AitoffprojectionofgalacticcoordinatesofNEDsampleof11candidatesourcesfromcompletesamples
at5GHzand2micron;thisisourbestestimateatpresentforthestrongestsourcesofultrahighenergycosmic
rays.Thestrongestcontributorsinsuchanall-skysurveyarepredictedtobeVirA(M87=NGC4486),CenA
(NGC5128),andForA(NGC1316):sourceL.Caramete
12
Accretionvs.Spin-down:poweringthejet
•
Twolimitstoconnectingrelativisticjetstothecentral
blackholes:
•
Theaccretionlimit,whenthemagneticfieldisgov-
ernedbycurrentaccretion
•
Thisapproachdescribeswellallactivebinarystarswith
blackholes,lowluminosityAGN,andsomehighactiv-
ityAGN
•
Thespin-downlimit,whenthemagneticfieldisgov-
ernedbypastactivity
•
Thisseemstocoverthevastmajorityofblackholes-
andobservationallytheyareallactive
•
Thispertainstoextremelylowlevelsofaccretion
•
ThePoyntingfluxisthelowerlimittotheenergyflow
alongjets,validinthelimitofnegligiblebaryonicload
13
Thebaryonicload
•
EnergyflowovermassflowgivesLorentzfactor:Today
wethinkoftypically50forAGNjets,butconsider
structuredjets
•
Example:10
45
erg
/
s,and3
·
10
?
4
M
?
/yr
implya
Lorentzfactorof50:singlestarwanderingintojet?
•
AtsuchaPoyntingflux,chargedparticlescanbecon-
finedupto
Z
10
20
eV,where
Z
istheircharge.
•
Baryonsfromnearbystarwithwindcanalsofeedaccre-
tiondisk,probablyaredgiantstar:believedtohappen
inourGalacticcenter
•
Baryonsfromaccretiondisk,atabout0
.
1
M
?
/yr
(effi-
ciencyforjetpoweringassumedat10percent)forthis
power
14
Deterministicchaosinemission?
•
Jetaswellasbackgroundstars(spectralpeakat2
µ
)
produceradiationfield:photons
•
Shocksinjetproducehighenergyions,protons
•
Interactwithphotons:producingnewleptonsofmuch
higherenergythanpossiblebystraightacceleration
•
Interactwithmagneticfieldsandphotons,makefur-
therleptons,furtherphotons,cascadedowninenergy
•
Basicexemplaryequation(May
Nature
261
,459,1976)
X
i
+1
=
aX
i
(1
?
X
i
)
(1)
•
X
i
couldbeveryhighenergyleptonsattime
i
•
Chaoticregion:
a
=3
.
57to
a
=4
•
Onepossiblereasonforextremeshorttermvariability
15
Attempttoscaletheneutrinoproductionfromthesour-
cesofultrahighenergycosmicrays(J.Becker):
Figure9Amodelforthecompactjetstructure.SourceBecker&Biermann2009
16
p
γ −> ... ν
proton
emission
log(dN /dE *E dE )
ν
ν
ν
ν
~ z
−1
~ z
−1
log(z /pc)
+2
−3
−2
−1
0
+1
+3
~ z
−1
neutrino
production
p
p
p
p
p
p
p
log(B)
ν
ν
ν
ν
ν
ν
ν
ν
ν
ν
ν
ν
ν
p
p
p
pp
p
p
p
p
p
p
p
p
p
p
p
SRS (FR−I)
∼τ
Disk
p
p
p
p
ν
j
j
j
j
FRS (BL Lac)
Figure10NeutrinoproductioninAGN.SourceBecker&Biermann2009
17
•
Thelargestinteractionforultrahighenergy
protons
andions
isatthefirststrongshock,nearabout3000
r
g
•
Ion-
γ
leadstosinglenucleons,secondstagep-
γ
:Lumi-
nosityscaleswith
τ
ionγ
×
τ
pγ
,soaccentuates
flaring
!
•
Chargedpiondecayalsoleadstoveryenergeticelec-
tronsandpositrons,thatthemselvesalsoemitphotons,
coveringadifferentphotonenergyrange
•
Theresultingfluxshouldscalewiththe
square
ofthe
photonfield.Onecouldimagineathirdstage,withIC
ontheresultingleptons,sothirdpowerpossible
•
Infact,allstrongGeVandTeVsourcesareflatspec-
trumradiosources:all
highlyvariable
Flatspectrumradiosources
predictedtobestrongflaringneutrinoemitters
18
Figure11Predictionsofextragalacticneutrinos
19
Ultrahighenergyneutrinosourcecandidates
360
o
0
o
90
o
?
90
o
1226
?
02
0521
?
36
1253
?
05
2251
?
15
0316
?
41
2134
?
00
0831
?
55
1127
?
14
0438
?
43
1641
?
39
2200
?
42
2203
?
18
0923
?
39
0637
?
75
2223
?
05
0834
?
20
2345
?
16
1549
?
79
0428
?
53
0537
?
44
1345
?
12
0742
?
10
0440
?
00
0208
?
51
0851
?
20
Figure12Aitoffprojectioningalacticcoordinatesofthe25flatandinvertedradiospectrumsourceshighest
influxdensityat2.7GHz.Thesesourcesareprimecandidatestobeultrahighenergyneutrinoandphoton
sources.3C279=1253-05,seeMannheimetal.1992
20
KeyConcepts
•
Threemainsourceclasses:
•
60
µ
-selectedsources,withFIR/Radio
?
250,star-
burstswithlotsofGRBs:primeexampleM82
•
5GHZselectedradiosourceswithsteepspectrum:
UHECRsourcecandidates:primeexampleCenA
•
5GHzselectedflatspectrumradiosources:HEneu-
trinocandidatesources:primeexample3C279
•
Sourceswillbeextremelyvariable,withspikes
Bestbet:Flaringneutrinoemissionfrom
flatradiospectrumAGN
21
Acknowledgement
WorkwithPLBwassupportedbycontractAUGER05
CU5PD1/2viaDESY/BMBandbyVIHKOSviaFZ
Karlsruhe;byErasmus/SokratesEU-contractswithethe
universitiesinBucharest,Cluj-Napoca,Budapest,Szeged,
Cracow,andLjubljana;bytheHumboldtFoundation;and
byresearchfoundationsinKorea,China,Australia,India
andBrazil.
References
[1]
Beck,R.,Brandenburg,A.,Moss,D.,Shukurov,A.,
&Sokoloff,D.,
AnnualRev.ofAstron.&Astro-
phys.
34
,155-206(1996).
[2]
Becker,J.K.,
J.Phys.:Conf.Ser.
136
022055
(2008),
http://www.iop.org/EJ/abstract/1742-
6596/136/2/022055
22
[3]
Becker,J.K.,&Biermann,P.L.,
Astropart.Phys.
31
,138(Januar2009)
[4]
Biermann,L.,
Z.f.Naturf.
5a
,65-71(1950)
[5]
Biermann,L.,Schlute¨r,A.,
Phys.Rev.
82
,863-868
(1951)
[6]
Biermann,P.L.,
Astron.&Astroph.
271
,649
(1993);astro-ph/9301008(CR-I)
[7]
CosmicraysII.Evidenceforamagneticrotator
Wolf-Rayetstarorigin,Biermann,P.L.,&Cassinelli,
J.P.,
Astron.&Astroph.
277
,691(1993);astro-
ph/9305003(CR-II)
[8]
Biermann,P.L.,inProc.EriceMeetingDec.2000,
Eds.H.J.deVegaetal.,
Phasetransitionsinthe
earlyUniverse:TheoryandObservations
,p.543
-557(2001)
[9]
Birk,G.T.,Wiechen,H.,Lesch,H.&Kronberg,P.
P.,2000,
Astron.&Astroph.
353
,108-116(2000)
23
[10]
Blasi,P.,Burles,Sc.,Olinto,A.V.,
Astrophys.J.
514
,79(1999),astro-ph/9812487
[11]
Blasi,P.,Olinto,A.V.,
Phys.Rev.
D59
,ms.023001
(1999),astro-ph/9806264
[12]
Cho,Vishniac,Beresnyak,Lazarian&Ryu,
arXiv:0812.0817(acceptedforpublicationinApJ)
[13]
Clarke,T.,Kronberg,P.P.,B¨ohringer,H.,in
Diffuse
thermalandrelativisticplasmaingalaxyclusters
,
RingbergConference,Eds.H.B¨ohringer
etal.
,Max-
Planck-InstitutfurExtraterrestrischePhysik,p.82
(1999)
[14]
Clarke,T.,Kronberg,P.P.,B¨ohringer,H.,
Astro-
phys.J.Letters
547
,L111-L114(2001),astro-
ph/0011281
[15]
Cowling,T.G.,
SolarElectrodynamics
,1953,in
TheSun,Ed.Kuiper,G.P.,Univ.ofChicagoPress,
Chicago
24
[16]
Das,Kang,Ryu,&Cho2008
Astrophys.J.
,
[17]
Duschl,W.J.,Strittmatter,P.A.,&Biermann,P.L.,
Astron.&Astroph.
357
,1123-1132(2000),astro-
ph/0004076
[18]
Enßlin,T.A.,Biermann,P.L.,Kronberg,P.P.,&
Wu,X.-P.,
Astrophys.J.
477
,560,(1997),astro-
ph/9609190
[19]
Everett,J.E.,etal.,TheMilkyWay’sKiloparsec-
ScaleWind:AHybridCosmic-RayandThermally
DrivenOutflow,
Astrophys.J.
674
,258-270(2008)
[20]
Galea,C.,M.Sc.thesis,UniversityofBucuresti
(2002)
[21]
Ultra-high-energycosmicrayaccelerationbyrela-
tivisticblastwaves,Gallant,Y-A.,Achterberg,A.,
Month.Not.Roy.Astr.Soc.
305
,L6-L10(1999)
25
[22]
Ginzburg,V.L.,Syrovatskii,S.I.,
Astron.Zh.
40
,
466-476(1963);transl.in
Sov.Astron.A.J.
7
,357
-364(1963)
[23]
Ginzburg,V.L.&Syrovatskii,S.I.,
Theoriginof
cosmicrays
,PergamonPress,Oxford(1964),Rus-
sianedition(1963).
[24]
Han,J.L.,Qiao,G.J.,
Astron.&Astroph.
288
,759
(1994)
[25]
Han,J.L.,Manchester,R.N.,Berkhuijsen,E.M.,
Beck,R.,
Astron.&Astroph.
322
,98(1997)
[26]
Han,J.L.,Manchester,R.N.,Qiao,G.J.,
Month.
Not.Roy.Astr.Soc.
306
,371(1999)
[27]
Jokipii,J.R.,Rateofenergygainandmaximum
energyindiffusiveshockacceleration,
Astrophys.J.
313
,842-846(1987)
[28]
Kaneda,H.,
etal.Astrophys.J.
491
,638(1997)
26
[29]
Khanna,R.,&Camenzind,M.,
Astrophys.J.Let-
ters
435
,L129-L132(1994)
[30]
Kim,K.T.,
etal.
,
Nature
341
,720-723(1989)
[31]
Krause,F.,Steenbeck,M.,
Z.f.Naturf.
22a
,671
-675,(1967),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.81
[32]
Krause,F.,Habilitationsschrift,Univ.ofJena,1967,
translatedinNCAR-TN/IA-60
Theturbulentdy-
namo
,editedbyP.H.Roberts,M.Stix,1971,p.103
[33]
Krause,F.,
Monatsb.Dt.Akad.Wiss.
11
,188
-194,(1969),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.313
[34]
Krause,F.&Beck,R.,
Astron.&Astroph.
335
,
789(1998)
27
[35]
Kronberg,P.P.,
Rep.Prog.Phys.
,
57
,325-382
(1994)
[36]
Kronberg,P.P.,Lesch,H.,Hopp,U.,
Astrophys.J.
511
,56-64(1999)
[37]
Kronberg,P.P.in
TheOriginsofGalacticMag-
neticFields
,24thmeetingoftheIAU,JointDiscus-
sion14,August2000,Manchester,England.
[38]
Kronberg,P.P.in
HighEnergyGamma-RayAs-
tronomy
,InternationalSymposiumheld26-30June,
2000,inHeidelberg,Germany.AIP)Proc.,vol.
558
,
451(2001)
[39]
Kulsrud,R.M.,Cen,R.,Ostriker,J.P.,Ryu,D.,
As-
trophys.J.
480
,481(1997)
[40]
Kulsrud,R.M.,
AnnualRev.ofAstron.&Astro-
phys.
37
,37(1999).
[41]
Lerche,I.&Parker,E.N.,
Astrophys.J.
168
,231
(1971)
28
[42]
Lerche,I.&Parker,E.N.,
Astrophys.J.
176
,213
(1972)
[43]
Krause,F.,Radler,K.H.&Rudi¨ger,G.,Thecosmic
dynamo:proceedingsofthe157thSymposiumofthe
InternationalAstronomicalUnionheldinPotsdam,
F.R.G.,September7-11,1992,publ.1993
[44]
Lin,C.C.,Yuan,C.,&Shu,FrankH.,
Astrophys.
J.
155
,721(1969);Erratumin
Astrophys.J.
156
,
797(1969)
[45]
Lynden-Bell,D.,Pringle,J.E.,
Month.Not.Roy.
Astr.Soc.
168
,603-637(1974)
[46]
Mestel,L.,Roxburgh,I.W.,
Astrophys.J.
136
,615
-626(1962)
[47]
Parker,E.N.,DynamicsoftheInterplanetaryGas
andMagneticFields.,
Astrophys.J.
128
664(1958)
[48]
Parker,E.N.,
Astrophys.J.
157
,1129(1969)
29
[49]
Parker,E.N.,
AnnualRev.ofAstron.&Astro-
phys.
8
,1(1970)
[50]
Parker,E.N.,
Astrophys.J.
160
,383(1970)
[51]
Parker,E.N.,
Astrophys.J.
162
,665(1970)
[52]
Parker,E.N.,
Astrophys.J.
163
,255(1971)
[53]
Parker,E.N.,
Astrophys.J.
163
,279(1971)
[54]
Parker,E.N.,
Astrophys.J.
164
,491(1971)
[55]
Parker,E.N.,
Astrophys.J.
165
,139(1971)
[56]
Parker,E.N.,
Astrophys.J.
166
,295(1971)
[57]
Parker,E.N.,
Astrophys.J.
168
,239(1971)
[58]
Parker,E.N.,
Astrophys.Sp.Sc.
22
,279(1973)
[59]
Parker,E.N.,
Astrophys.J.
198
,205-209(1975)
[60]
Parker,E.N.,
NewYorkAcademySciencesAn-
nals
,
257
,141-155,(1975)
30
[61]
R¨adler,K.-H.,
Z.f.Naturf.
23a
,1841-1851(1968),
translatedinNCAR-TN/IA-60
Theturbulentdy-
namo
,editedbyP.H.Roberts,M.Stix,1971,p.247
[62]
R¨adler,K.-H.,
Z.f.Naturf.
23a
,1851-1860(1968),
translatedinNCAR-TN/IA-60
Theturbulentdy-
namo
,editedbyP.H.Roberts,M.Stix,1971,p.267
[63]
R¨adler,K.-H.,
Monatsb.Dt.Akad.Wiss.
11
,194
-201,(1969),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.291
[64]
R¨adler,K.-H.,
Monatsb.Dt.Akad.Wiss.
11
,272
-279,(1969),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.301
[65]
R¨adler,K.-H.,
Monatsb.Dt.Akad.Wiss.
12
,468
-472,(1970),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.309
31
[66]
Rybicki,G.B.,Lightman,A.P.,
Radiativeprocesses
inastrophysics
,WileyInterscience,NewYork,1979
[67]
Ryu,D.,Kang,H.,Biermann,P.L.,
Astron.&As-
troph.
335
,19-25(1998),astro-ph/9803275
[68]
Ryu,Kang,Cho,&Das2008
Science
[69]
Seemann,H.&Biermann,P.L.,
Astron.&Astroph.
327
,273(1997),astro-ph/9706117
[70]
Shu,F.H.,
Astrophys.J.
160
,89(1970)
[71]
Shu,F.H.,
Astrophys.J.
160
,99(1970)
[72]
Shu,F.H.,
etal.
,
Astrophys.J.
172
,557(1972)
[73]
Simard-Normandin,M.&Kronberg,P.P.,
Astro-
phys.J.
242
,74-94(1980)
[74]
Snowden,S.L.,
etal.
,
Astrophys.J.
485
,125
(1997).
[75]
SpitzerJr.,L.,
Physicsoffullyionizedgases
,1962,
2nded.,WileyInterscience,NewYork.
32
[76]
SpitzerJr.,L.,
Diffusematterinspace
,1968,Wi-
leyInterscience,NewYork.
[77]
CosmicraysIV.Thespectrumandchemicalcompo-
sitionabove10
4
GeV,Stanev,T.,Biermann,P.L.,&
Gaisser,T.K.,
Astron.&Astroph.
274
,902(1993);
astro-ph/9303006(CR-IV)
[78]
Steenbeck,M.,Krause,F.,
Monatsb.Dt.Akad.
Wiss.
7
,335-340,(1965),translatedinNCAR-
TN/IA-60
Theturbulentdynamo
,editedbyP.H.
Roberts,M.Stix,1971,p.21
[79]
Steenbeck,M.,Krause,F.,R¨adler,K.-H.,
Z.f.
Naturf.
21a
,369-376,(1966),translatedinNCAR-
TN/IA-60
Theturbulentdynamo
,editedbyP.H.
Roberts,M.Stix,1971,p.29
[80]
Steenbeck,M.,Krause,F.,
Z.f.Naturf.
21a
,1285
-1296(1966),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.49
33
[81]
Steenbeck,M.,
etal.Monatsb.Dt.Akad.Wiss.
9
,
714-719(1967),translatedinNCAR-TN/IA-60
Theturbulentdynamo
,editedbyP.H.Roberts,M.
Stix,1971,p.97
[82]
Steenbeck,M.,Krause,F.,
Astron.Nach.
291
,49-
84(1969),translatedinNCAR-TN/IA-60
Thetur-
bulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.147
[83]
Steenbeck,M.,Krause,F.,
Astron.Nach.
291
,271
-286(1969),translatedinNCAR-TN/IA-60
The
turbulentdynamo
,editedbyP.H.Roberts,M.Stix,
1971,p.221
[84]
Valinia,A.,Marshall,F.E.,
Astrophys.J.
505
,134
-147(1998).
[85]
Vall´ee,J.P.,
Astron.J.
99
,459(1990).
[86]
V¨olk,H.J.&Atoyan,A.M.,
Astrophys.J.
541
,88
-94(2000).
34
[87]
vanderWel,A.,Franx,M.,vanDokkum,P.G.,
Huang,J.,Rix,H.-W.,Illingworth,G.D.,
Astro-
phys.J.Letters
636
,L21-L24(2006);astro-
ph/0511581
[88]
“Superluminalnon-ballisticjetswinginthequasar
NRAO150revealedbymm-VLBI”,Agudo,I.,etal.,
Astron.&Astroph.Letters
476
,L17(2007)
[89]
“Correlationofthehighestenergycosmicrays
withnearbyextragalacticobjects”,AUGER-
collaboration,
Science
318
,939-943(9November
2007);arXiv:0711.2256
[90]
“Correlationofthehighest-energycosmicrayswith
thepositionsofnearbyactivegalacticnuclei”,
AUGER-collaboration,
Astropart.Phys.
29
,188-
204(2008);arXiv:0712.2834
[91]
“Neutrinosfromactiveblackholes,sourcesoful-
trahighenergycosmicrays”,Becker,J.K.,&Bier-
35
mann,P.L.,submittedto
Astropart.Phys.
(2008);
arXiv:0805.1498
[92]
“TheactivejetinNGC4258anditsassociated
shocks”,Cecil,G.,etal.,
Astrophys.J.
536
,675
(2000)
[93]
“ThesmallestAGNhostgalaxies”,Greene,J.E.,
Barth,A.J.,&Ho,L.C.,
NewAstron.Rev.
50
,739
-742(2006);astro-ph/0511810
[94]
“VLBAcontinuumobservationsofNGC4258:Con-
straintsonanadvection-dominatedaccretionflow”,
Herrnstein,J.R.etal.,
Astrophys.J.Letters
497
,
L69(1998)
[95]
“Theinnerjetofanactivegalacticnucleusasre-
vealedbyaradio-to-
γ
-rayoutburst”,Marscher,A.P.
etal.,
Nature
452
,966-969(2008)
[96]
“TheblackholeaccretiondiskinNGC4258:Oneof
Nature’smostbeautifuldynamicalsystems”,Moran,
J.,AIPConf.inpress(2008);arXiv:0804.1063
36
[97]
“FastGrowthofsupermassiveblackholesinGalax-
ies”,Munyaneza,F.,&Biermann,P.L.,
Astron.&
Astroph.
436
,805-815(2005);astro-ph/0403511
[98]
“Degeneratesterileneutrinodarkmattersinthe
coresofgalaxies”,Munyaneza,F.,&Biermann,P.L.,
Astron.&Astroph.Letters
458
,L9-L12(2006);
astro-ph/0609388
[99]
“AsearchforCOinMarkarianandSeyfertgalaxies”,
Wilson,T.L.;Biermann,P.;Fricke,K.J.,
Astron.
&Astroph.
79
,245-246(1979)
[100]
“Superluminalnon-ballisticjetswinginthequasar
NRAO150revealedbymm-VLBI”,Agudo,I.,etal.,
Astron.&Astroph.Letters
476
,L17(2007)
[101]
“Correlationofthehighestenergycosmicrays
withnearbyextragalacticobjects”,AUGER-
collaboration,
Science
318
,939-943(9November
2007);arXiv:0711.2256
37
[102]
“Correlationofthehighest-energycosmicrayswith
thepositionsofnearbyactivegalacticnuclei”,
AUGER-collaboration,
Astropart.Phys.
29
,188-
204(2008);arXiv:0712.2834
[103]
“Neutrinosfromactiveblackholes,sourcesoful-
trahighenergycosmicrays”,Becker,J.K.,&Bier-
mann,P.L.,submittedto
Astropart.Phys.
(2008);
arXiv:0805.1498
[104]
“TheactivejetinNGC4258anditsassociated
shocks”,Cecil,G.,etal.,
Astrophys.J.
536
,675
(2000)
[105]
“ThesmallestAGNhostgalaxies”,Greene,J.E.,
Barth,A.J.,&Ho,L.C.,
NewAstron.Rev.
50
,739
-742(2006);astro-ph/0511810
[106]
“VLBAcontinuumobservationsofNGC4258:Con-
straintsonanadvection-dominatedaccretionflow”,
Herrnstein,J.R.etal.,
Astrophys.J.Letters
497
,
L69(1998)
38
[107]
“Theinnerjetofanactivegalacticnucleusasre-
vealedbyaradio-to-
γ
-rayoutburst”,Marscher,A.P.
etal.,
Nature
452
,966-969(2008)
[108]
“TheblackholeaccretiondiskinNGC4258:Oneof
Nature’smostbeautifuldynamicalsystems”,Moran,
J.,AIPConf.inpress(2008);arXiv:0804.1063
[109]
“FastGrowthofsupermassiveblackholesinGalax-
ies”,Munyaneza,F.,&Biermann,P.L.,
Astron.&
Astroph.
436
,805-815(2005);astro-ph/0403511
[110]
“Degeneratesterileneutrinodarkmattersinthe
coresofgalaxies”,Munyaneza,F.,&Biermann,P.L.,
Astron.&Astroph.Letters
458
,L9-L12(2006);
astro-ph/0609388
[111]
“AsearchforCOinMarkarianandSeyfertgalaxies”,
Wilson,T.L.;Biermann,P.;Fricke,K.J.,
Astron.
&Astroph.
79
,245-246(1979)
39
