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Exploring potential cosmic ray accelerators with neutrinos What do - - PowerPoint PPT Presentation

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Exploring potential cosmic ray accelerators with neutrinos What do we learn by injecting nuclei in Gamma-Ray Bursts? Denise Boncioli, Daniel Biehl, Anatoli Fedynitch, Walter Winter DESY Zeuthen, Germany denise.boncioli@desy.de PoS(ICRC2017)1064

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Exploring potential cosmic ray accelerators with neutrinos

What do we learn by injecting nuclei in Gamma-Ray Bursts?

Denise Boncioli, Daniel Biehl, Anatoli Fedynitch, Walter Winter DESY Zeuthen, Germany

denise.boncioli@desy.de

PoS(ICRC2017)1064

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 2

Cosmic-ray horizon

Aloisio, Boncioli, di Matteo, Grillo, Petrera, Salamida, arXiv:1705.03729 [astro-ph.HE], submitted to JCAP

> No information about sources above z~1 ! > Can neutrinos be used to test UHECR sources ?

The Pierre Auger Collaboration, ICRC2015

from theory from data

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 3

The role of neutrinos

> Main UHECR processes (energy of the photon in the nucleus rest frame):

  • ε´>150 MeV, photo-pion production (nucleons and nuclei)
  • ε´> 8 MeV, photo-disintegration (nuclei)

> Contributions to neutrino production:

  • pion decay
  • beta decay
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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 4

From the sources to detection

Neutrino production happens both in the source and in the propagation through extragalactic space!

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 5

Gamma-Ray Bursts as test case

Credit: NASA

→ shocks (single collision internal shock model) → particle acceleration (including nuclei !) → nuclear cascade (production of secondary nuclei and neutrinos)

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 6

Nuclear cascade in a GRB shell

Ejected fluences

  • Pure iron (56Fe) composition injected into a GRB shell
  • Ejected fluence

→ dependent on the escape mechanisms (for charged CRs) → dependent on the density of the radiation

➢

Collisions at large radius and/or low luminosity GRB → rarefied photon field → less interactions

Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 7

Nuclear cascade source classes: parameter space scan

> Pure iron (56Fe) composition injected into a GRB shell

Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 8

Source – Propagation Model

➔ UHECR spectrum at Earth ➔ Composition observables ➔ Neutrino fluxes ➔Produced in the source ➔Produced during propagation

propagation source

OUTPUT INPUT INPUT > Chemical composition

  • f accelerated CRs

> Spectrum of accelerated CRs > Photon spectrum in the source > Nuclear Physics > Escape mechanism for CRs > Distribution of sources > Spectra of background photons > Nuclear Physics > Interaction model in the Earth’s atmosphere

Many uncertainties affect the interpretation of the data !

  • Batista, Boncioli, di Matteo, van Vliet,

Walz, JCAP 1510 (2015) no.10, 063

  • Boncioli, Fedynitch, Winter, Scientific

Reports 7, 4882 (2017)

  • Pierre Auger Collaboration, JCAP 1704

(2017) no.04, 038 Nuclear Physics and UHECR interactions: Fedynitch, Boncioli, Winter, Poster at CRI session, PoS(2017)559

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 9

Source – Propagation Model

Fit of UHECR data above 10 EeV → excluding the ankle

Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A Extragalactic propagation → SimProp MC code First release: Aloisio, Boncioli, Grillo, Petrera, Salamida, JCAP 1210 (2012) 007 Last release: Aloisio, Boncioli, di Matteo, Grillo, Petrera, Salamida, arXiv:1705.03729 [astro-ph.HE], submitted to JCAP

pure Si at injection

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 10

Source – Propagation Model

Fit of UHECR data above 10 EeV → excluding the ankle

IceCube excluded region from GRB stacking analysis, Aartsen et al 2017 Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A Extragalactic propagation → SimProp MC code First release: Aloisio, Boncioli, Grillo, Petrera, Salamida, JCAP 1210 (2012) 007 Last release: Aloisio, Boncioli, di Matteo, Grillo, Petrera, Salamida, arXiv:1705.03729 [astro-ph.HE], submitted to JCAP pure Si at injection

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 11

Source – Propagation Model

Fit of UHECR data above 10 EeV → excluding the ankle

IceCube excluded region from GRB stacking analysis, Aartsen et al 2017 IceCube excluded region from cosmogenic neutrinos, Aartsen et al 2016 Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A Extragalactic propagation → SimProp MC code First release: Aloisio, Boncioli, Grillo, Petrera, Salamida, JCAP 1210 (2012) 007 Last release: Aloisio, Boncioli, di Matteo, Grillo, Petrera, Salamida, arXiv:1705.03729 [astro-ph.HE], submitted to JCAP pure Si at injection

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 12

“Mixed Composition Ankle Model”

A=1 A=[2,4] A=[5,22] A=[22,28]

Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A

Fit above 10 EeV → excluding the ankle

pure Si at injection

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 13

Summary

> We take into account the injection of nuclei (→ results from Pierre Auger Observatory about chemical composition) in Gamma-Ray Bursts and model the interactions in the source > Neutrino and CR production depend on the development of the cascade in the source → classification of sources in terms of population of the cascade → importance of uncertainties (from nuclear physics and astrophysics) > Ejected fluxes of CRs and neutrinos from the source are propagated to Earth → source-propagation model, including a fit of UHECR data > Neutrinos can efficiently test the GRB-UHECR paradigm !

  • Boncioli, Biehl, Fedynitch, Winter, PoS(ICRC2017)1064
  • Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A
  • Boncioli, Fedynitch, Winter, Scientific Reports 7, 4882 (2017)
  • A. Fedynitch, Poster at CRI session, PoS(2017)559
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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 14

Future directions

> Efficient combined source-propagation model → can be applied to other candidate sources, such as Active Galactic Nuclei → can be applied to other models for GRBs, such as multi-zone > More detailed parameter-space study including → variations in the propagation (EBL model, cross section model) → variations in the hypotheses at the sources (source distribution and evolution with redshift, mixed composition at the source, spectrum function at injection)

  • Boncioli, Biehl, Fedynitch, Winter, PoS(ICRC2017)1064
  • Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A
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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 15

BACKUP slides

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 16

Injection of nuclei and maximum energy

> Injection of nuclei with cut-off power law spectrum expected from Fermi shock acceleration in acceleration zone > Maximum energy reached when the sum of all energy loss processes exceeds the energy gain by the acceleration > Normalization to injection luminosity with “nuclear loading”

Here: k = 2 P = 2 Pair prod. typically sub-dom. here

> Talk by D. Biehl at Neucos Workshop

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 17

Beam of p, A, … Radiation zone: Ap, Aγ Interactio ns

QA’,out Qν,out Qγ,out

Evolution of density for particle species i Evolution of density for particle species i Energy loss: synchrotron adiabatic … Energy loss: synchrotron adiabatic … Escape: dynamical timescale interactions decays … Escape: dynamical timescale interactions decays …

Boltzmann Equations for each particle species (and energy bin) Boltzmann Equations for each particle species (and energy bin)

Injection from: acceleration zone interactions or decays Injection from: acceleration zone interactions or decays

Interactions

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 18

Energetics of the source

> Spectrum of GRBs: > Isotropic volume: > Normalization of the photon flux

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 19

GRB models

> Internal shock model (one-zone): the shells of plasma are assumed to collide at and the shell width is The collisions happen at the same radius > Internal shock model (multi-zone): (Kobayashi, Piran and Sari (1997)) shells of plasma are ejected from the central emitter, colliding at varying collision radii centered around a mean value. The key parameter is R > Photospheric models, for example in Rees and Meszaros (2005) > Magnetic reconnection models, for example in Zhang and Yan (2011)

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 20

Cosmic ray escape

> Neutrons can escape freely while charged particles can only escape if they can reach the edge of the shell within their Larmor radius: > The condition is satisfied if the maximal primary energy is limited by the adiabatic energy losses (typically when the radiation densities and the primary energies are low) > Direct escape will be suppressed if the source is optically thick to photo-hadronic interactions > Discussed in Baerwald et al (2013); the mechanism of escape affects the CR:neutrino ratio

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 21

Source class I: Empty Cascade

> Low luminosity / large collision radii > Only a few isotopes in the cascade populated relative to injected energy in primaries > Maximum energy determined by adiabatic cooling, i.e. rigidity-dependent / Peters cycle > Optically thin to photo-hadronic interactions of all species > Nuclei stay mostly intact and escape as CR

[DB, D. Boncioli, A. Fedynitch, W. Winter, arXiv:1705.08909]

> Talk by D. Biehl at Neucos Workshop

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 22

Source class II: Populated Cascade

> Intermediate luminosity / collision radii > Cascade broadly populated along the main diagonal relative to injected energy > Maximum energy determined by photo- hadronic processes, no Peters cycle! > Optically thick to photo-hadronic interactions

  • f heavy nuclei, still opt. thin to light nuclei

> Nuclei disintegrate partially

[DB, D. Boncioli, A. Fedynitch, W. Winter, arXiv:1705.08909]

> Talk by D. Biehl at Neucos Workshop

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 23

Source class III: Optically Thick Case

> High luminosity / small collision radii > Cascade populated but more narrow, most of the energy is dumped into nucleons > Maximum energy determined by photo- hadronic processes, no Peters cycle! > Optically thick to photo-hadronic interactions

  • f all species

> Nuclei disintegrate very efficiently

[DB, D. Boncioli, A. Fedynitch, W. Winter, arXiv:1705.08909]

> Talk by D. Biehl at Neucos Workshop

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 24

Prompt neutrinos: dependence on injection composition

> Total all flavor neutrino fluence for arbitrary (pure) injection composition > In energy range from ~ 10 TeV – 10 PeV hardly depending on the injection > Low energy differences because of neutrinos from beta decay, cutoff different since protons reach a higher max. energy (per nucleon)

> Talk by D. Biehl at Neucos Workshop

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 25

H injection, dip model

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 26

H injection, ankle model

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 27

Source – Propagation Model

Fit of UHECR data above 1 EeV → including the ankle Fit of UHECR data above 10 EeV → excluding the ankle

IceCube excluded region from GRB stacking analysis, Aartsen et al 2017 IceCube excluded region from cosmogenic neutrinos, Aartsen et al 2016 Biehl, Boncioli, Fedynitch, Winter, arxiv:1705.08909, submitted to A&A Extragalactic propagation → SimProp MC code First release: Aloisio, Boncioli, Grillo, Petrera, Salamida, JCAP 1210 (2012) 007 Last release: Aloisio, Boncioli, di Matteo, Grillo, Petrera, Salamida, arXiv:1705.03729 [astro-ph.HE], submitted to JCAP

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 28

“Dip”

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 29

“Dip”

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 30

“Ankle”

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 31

“Ankle”

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 32

Nuclear composition of GRB jets

  • Usual assumption:
  • GRB jet initially consists of free nucleons
  • nucleons can recombine into deuterium or alpha as the jet expands and cool but

nuclei heavier than carbon cannot be produced

  • The mechanisms to launch a relativistic jet is not yet completely understood → initial

composition is not necessarily free nucleons

  • some observations of GRBs suggest that their relativistic jets were initially

dominated by the magnetic field energy flux, being able to involve also heavy nuclei (A=56)

  • In Shibata & Tominaga, arXiv:1503.03662 [astro-ph.HE] , the jet is assumed to be

due to falling matter during a relativistic jet-induced explosion. They adopt Wolf- Rayet stars as progenitors

  • Other possibility: nucleosynthesis in from free nucleons in the central engine of

GRBs (Metzger et al, 2011)

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 33

Dip Model, primary Si propagated, best fit

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 34

Dip Model, primary Si propagated, point C

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 35

Ankle Model, primary Si propagated, best fit

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 36

Ankle Model, primary Si propagated, point C

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 37

Protons – dip model

> Robustness of dip feature: protons are collected from a large volume → feature not

sensitive to local over-density or deficit of sources

➔A.M. Hillas, Phys. Lett. 24A 677 (1967) ➔G.R. Blumenthal, Phys. Rev. D Vol 1 1596 (1970)

> Its observation has been considered as evidence for proton composition, for example

Berezinzky, Gazizov, Grigorieva Phys.Rev. D74 (2006) 043005

A=1

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 38

A=1

Protons – suppression of the flux

➔K. Greisen, PRL 16 748 (1966), ➔G.T. Zatsepin and V.A. Kuzmin, Sov. Phys. JETP Lett. 4 78

Muecke et al, Publ. Astron. Soc. Aust., 1999, 16, 160–6

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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 39

Nuclei – suppression of the flux

  • D. Allard, Astropart. Phys. 39-40 (2012) 33-43
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Denise Boncioli | Neutrinos and UHECRs | ICRC 2017 | Page 40

Nuclei – suppression of the flux

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Denise Boncioli | Nuclear Physics and Cosmic Rays | Sep 15th, 2016 | Page 41

Effects on the nuclear cascade

> One nuclide for each A > Only small fragments can be ejected in photodisintegration > The cascade is not completed, smaller masses are not populated

> Population of isotopes in terms of total energy per isotope and collision in the shock rest frame

DB, A. Fedynitch, W. Winter, arxiv:1607.07989

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Denise Boncioli | Nuclear Physics and Cosmic Rays | Sep 15th, 2016 | Page 42

Effects on the nuclear cascade

> Much more channels wrt PSB > Small fragments ejected: p, n, d, t, He-3, He-4 > Chart almost fully populated (however, this also depends on the target photon density) > PEANUT gives similar results

> Population of isotopes in terms of total energy per isotope and collision in the shock rest frame

DB, A. Fedynitch, W. Winter, arxiv:1607.07989

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Denise Boncioli | Nuclear Physics and Cosmic Rays | Sep 15th, 2016 | Page 43

Effects on the nuclear cascade

> Population of isotopes in terms of total energy per isotope and collision in the shock rest frame

> Cross sections reduced by:

  • 1 if the absorption cross section is

measured

  • 0.5 if any other cross section is

measured

  • 0 if no data available

> Relying on data, the cascade cannot be populated

DB, A. Fedynitch, W. Winter, arxiv:1607.07989

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Denise Boncioli | Nuclear Physics and Cosmic Rays | Sep 15th, 2016 | Page 44

UHECR composition at the source

> No propagation effects considered > Simplified model PSB leads to a sharper increase of composition wrt more sophisticated models > If only measured cross sections are included in the models, similar results to PSB

DB, A. Fedynitch, W. Winter, arxiv:1607.07989