Models of neutrino production in cosmic sources

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Models of neutrino production in cosmic sources Cecilia Lunardini

Models of neutrino production in cosmic sources

Cecilia Lunardini

Arizona State University

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Structure of this talk

Introduction: astrophysical ν spectrum from eV to EeV High energy neutrinos at IceCube: hypotheses and models

Active Galactic Nuclei (AGN) Tidal Disruption Events (TDEs) others

Summary and future prospects

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Introduction

Astrophysicalν spectrum from eV to EeV

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Unified neutrino spectrum

fig. from Vitagliano, Tamborra and Raffelt, Rev.Mod.Phys. 92 (2020) 45006 (transients not included)

sub-eV : Cosmicνbackground (CνB),νs from Big Bang Nucleosynthesis (BBN)

1 - 50 MeV : Diffuse Supernova Neutrino Background (DSNB) 0.1 - 10 PeV : diffuse extragalacticνflux (from source + cosmogenic)

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Cν B: a dream for the (distant) future

de-coheredmass

eigenstatesfrom the first second post-Big Bang detectable withO(100) g ofH₁³, with precision energy measurement

sensitive to Dirac vs Majorana neutrinos, sterile states

Electron Kinetic EnergyHKeL

ElectronSpectrumHdGdEeL +m4

+mΝ -mΝ

Kend0»18.6keV Β-decayendpointHKendL

CΝB

SterileΝ

Weinberg, Phys.Rev. 128 (1962) 1457-1473 ; Cocco, Mangano and Messina, JCAP 06 (2007) 015 Long, CL and Sabancilar, JCAP 08 (2014) 038 PTOLEMY experiment, Betts et al., e-Print: 1307.4738

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DSNB: a dream for the (near) future

Thermalνs from cosmological supernovae

neutrino image of diverseSN population detectable at

upcoming SuperK-Gd and JUNO

due to background abatement

ææ æææ ô

ôôôôôôôôô

0 10 20 30 40 50

10^-4 0.001 0.01 0.1 1 10 100

EMeV Fcm-2MeV-1s-1

Experimental limits

Super-K,Ν SNO,Ν KamLAND,Ν Super-K,Ν

Super-K indirect,Ν Super-K,Ν Borexino,Ν

Bisnovatyi-Kogan and Seidov, Sov. Ast. 26 (1982) 132.

Krauss, Glashow, and Schramm, Nature 310 (1984) 191-198

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High energy extragalactic ν s: a dream come true

Multi-decade operation at IceCube, more than 100 neutrinos detected

a mixed originpicture is emerging, 5 individual sources identified

Name Type p Ref.

NGC 1068 AGN 0.008 Aartsen et al. (2020) TXS 0506+056 blazar 0.001 Aartsen et al. (2018) PKS 1502+106 blazar 0.01 Taboada & Stein (2019) PKS 1424-41 blazar 0.05 Kadler et al. (2016) AT2019dsg TDE 0.002 Stein et al. (2020)

Bartos et al., e-Print: 2105.03792

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High energy neutrinos at IceCube

hypotheses and models: AGN, TDEs, and others

Theme:

What can we learn on the diffuse flux from the 5 identified sources and their neutrinos?

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Blazars and other Active Galactic Nuclei (AGN)

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The Unified AGN model: Blazars are AGN

fig. from E. Zackrisson, PhD thesis

Blazar = on-axis view (jet pointing towards us) sub-types: BL-Lac, FSRQ, ...

Quasar, Seyfert = off axis view

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Blazars: SMBH with jet pointing to Earth

fig. from Gao, Fedynitch, Winter and Pohl, Nat. Astron. 3, 88?92 (2019)

p acceleration in internal shocks,p+γ→....→νµ, νe

account for ∼80% of total extragalactic gamma ray fux

Inoue and Totani, 2009, ApJ 702, 523; Ackermann et al., 2015, ApJ 799, 86

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TXS0506+056: multi-messenger theory

TXS0506+056 : a flaring AGN

neutrino spectrum and fluence constrained by multi-wavelength, multi-time data fully consistent hadron/lepton/ν/γ/

time-evolving simulation required

Gao, Fedynitch, Winter and Pohl, Nat. Astron. 3, 88?92 (2019)

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diffuse Blazar flux

sub-PeV flux not reproduced

can account for PeV events

stacking limit requires strong evolution

enhanced contribution of unresolved sources (higher baryonic loading)

suppressed FSRQ contribution

Palladino, Rodrigues, Gao and Winter, Astrophys.J. 871 (2019) 1, 41

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Other AGN: NGC1068 as a IceCube hotspot

NGC1068 : Seyfert-2 (off-axis view AGN) and starburst galaxy ν flux higher thanγ-ray: dense environment withγabsorption Disk-corona model: p accelerated by plasma turbulence

Murase, Kimura and Meszaros, Phys.Rev.Lett. 125 (2020) 1, 011101 Inoue, Khangulyan and Doi, Astrophys.J.Lett. 891 (2020) 2, L33 Kheirandish, Murase and. Kimura, e-Print: 2102.04475

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Disk-corona: multimessenger consistency

fits NGC1068ν spectrum at 10-100 TeV

consistent withγ-ray spectrum

Inoue, Khangulyan and Doi, Astrophys.J.Lett. 891 (2020) 2, L33

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Diffuse flux from AGN coronae

could reproduce medium-energy IceCube data if CR carry only∼few% of thermal energy future test: MeV gamma rays

10^-9 10^-8 10^-7 10^-6 10^-5 10^-4

10^-410^-310^-210^-110⁰10¹ 10²10³10⁴ 10⁵10⁶10⁷ E2[GeV cm-2s-1sr-1]

E [GeV]

AGN corona AGN corona (cascade) AGN corona X (thermal e)

reacceleration

10-100 TeV (medium-energy ) GeV-TeV PeV

MeV

Murase, Kimura and Meszaros, Phys.Rev.Lett. 125 (2020) 1, 01110

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Tidal Disruption Events (TDEs)

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Supermassive black holes as star-shredders

a star is torn apart by SuperMassive Black Hole (SMBH) part of the debris are accreted, a flare is produced

in extreme cases, a relativistic hadronic jet forms→neutrino production!

∼90 TDEs observed, 3 with evidence of jets

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Month/year long transients

∼1/2 of star’s mass remains bound, falls back onto the SMBH

flare fades when mass accretion rate drops below Eddington Luminosity, LEdd'

1.3 10⁴⁴ ^erg_s

M 10⁶M

. typical duration

∆T ∼ O(0.1−1) yr

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IceCube-191001A and AT2019dsg

Opt-UV by Zwicky Transient Facility (ZTF); X-rays from Swift, NICER.

neutrino detected5 months post-peak(dotted line)

p-value of 0.2% to 0.5% of random association;∼3σsignificance.

R. Stein et al., Nature Astron. 5 (2021) 510-518

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AT2019dsg basic facts

z'0.05 (dL'230 Mpc). Optical-UV, X-ray thermal spectra.

Optical-UV

TBB= 3.35eVRBB'5 10¹⁴cm,LBB= 2.88·10⁴⁴erg s⁻¹

X-ray

T_X ∼0.06 keV,R_X ∼3−7 10¹¹cm, L_X ∼2.5 10⁴³ erg s⁻¹ ([0.3−8]keV) L_X ∼4 10⁴⁴ erg s⁻¹ ([0.1−10] keV).

Radio

radio emission nearly constant with increasing radius of emission R_radio=O(10¹⁶)cm

(indication of mildly relativistic outflow)

van Velzen, et al., Astrophys.J. 908 (2021) 1, 4; R. Stein et al., Nature Astron. 5 (2021) 510-518

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Interpretation: jetted model

hadronic jet with internal shocks

late/sustained neutrino production due to backscattered X-rays + decreasing collision radius (Rc)

Winter and Lunardini, Nat. Astron. 5, 472-477 (2021

jet

observer

fast flow

slow flow

X-ray Opt-UV

RC

RX R_BB

t.AE_,

t t t ?^.

ammm#AMmnmmy•

I _I

E_-ao⇒y _Hi :

^v ^ay-^,

jet

observer

fast flow

slow flow

X-ray Opt-UV

RC p

RX RBB

e.ie:779

immunoassay

Hitherward

.

.tl if

^a

• I _y

T

it

^I ⁱ ^-

Rradio

Left: early times (t.17days); Right: late times (t&17days)

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Inspiration from MHD simulations

Observed blackbody radius and bolometric luminosity match the

“Unified TDE model” for M'10⁶M

Dai, McKinney, Roth, Ramirez-Ruiz, & Miller, Astrophys. J. 859, L20 (2018)

Unified model predicts:

jet withL^phys_jet '20LEdd'3 10⁴⁵ ^erg_s

M 10⁶M

;

outflow with velocity decreasing from fast to slow away from jet funnel

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Results: neutrino luminosity explains late observation

-50 0 50 100 150 200 250 300

41 42 43 44 45 46

t-tpeak[days]

Log10L[ergs-1]

BB

Neutrinos X-rays

observed unattenuated

isotropized Ledd

Ljetphys

Lpiso

Jet ceases

result: red (neutrino) curve; inputs: all other curves. Arrow: time of neutrino detection

numerical calculation done with NeuCosmA code

see Lunardini and Winter, arXiv:1612.03160, and refs. therein.

double peak in Lν due to interplay of decline ofL^isotr_X ^.and decrease of RC (i.e., increase in neutrino production efficiency)

→reproduces late time neutrino detection!

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Neutrino fluence and expected number of events

Total t-tpeak<100 days t-tpeak≥100 days

3 4 5 6 7 8 9

-8 -6 -4 -2 0 2

Log10Eν[GeV]

Log10Eν2ℱμ[GeVcm-2]

GFU,Nμ∼0.05

PS,Nμ∼0.26

Eν

GFU: gamma-ray follow-up effective area ; PS: point source effective area

good agreement with likely neutrino energy

number of predicted events: N_µ∼0.05−0.26 depending on effective detector area used

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Contribution to diffuse flux at IceCube

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can contribute to up to∼30% of diffuse flux

low energy spectrum requires strong evolution of parameters with BH mass

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Alternate models for TDE neutrinos

isotropic outflow interacting with UV photons non-relativistic shocks forming in the environment

neutrino production from the accretion disk (radiatively inefficient accretion flows, magnetically arrested disk states, etc.)

hot corona similar to that of AGN

Stein et al. , Nat. Astron. 5 (2021) 510-518;

Fang, Metzger, Vurm, Aydi & Chomiuk, Ap.J. 904 (2020) 1, 4;

Hayasaki & Yamazaki, ApJ, 886 114 (2019);

Murase, Kimura, Zhang, Oikonomou & Petropoulou, ApJ. 902 (2020) 2, 108

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Other sources of high energy neutrinos

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Supernovae? GRBs? Starburst galaxies?

Stellar sources (supernovae, GRBs):

O(10⁻²) of total diffuse flux

Bartos et al., e-Print: 2105.03792

Starburst galaxies:

UHECR reservoirs could fit sub-PeV flux, if distribution of spectral indices is used

Ambrosone et al., Mon.Not.Roy.Astron.Soc. 503 (2021) 3

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Summary and future prospects

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The emerging protagonist: SuperMassive Black Holes

The 5 identified sources all involve SMBH

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Wishes for the future

Theory: develop a multimessenger unified SMBH model full consistency between CR,νand photon predictions dependence on SMBH mass, spin? Viewing angle?

Observation: increase point-source potential

increase sensitivity to less luminous sources (IceCube Gen-2) strengthen multi-messenger campaigns (extend telescopes networks, increase coverage in time and area)

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Thank you!

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Backup

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Models of neutrino production in cosmic sources