report on wp1 (theory and phenomenology) at the hap ...sigl/hap-topic1-sigl.pdf · 4/11/2014 ·...

Report on WP1 (Theory and Phenomenology) at the HAP midterm review 4.11.2014 presented by Günter Sigl, University of Hamburg

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04.11.2014 Helmholtz Alliance for Astroparticle Physics 2

WP2 acceleration

WP1 propagation

WP1 detection

WP3 non-acceleration

04.11.2014 Helmholtz Alliance for Astroparticle Physics

The detailed tasks: Work Packages

• WP1: Propagation and Detection (G.Sigl) – galactic cosmic rays: GALPROP, DRAGON – extragalactic cosmic rays: CRPropa+Galaxy – air showers, LHC input for cross sections

• WP2: Particle-Acceleration Sources (M.Pohl) – analytical+numerical models, plasma physics – link to gamma-ray and neutrino observations

• WP3: Dark Matter and Non-Acceleration (M.Klasen) – predictions of relic densities, direct and indirect

signatures

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Global Goals

• achieving strong collaboration between the German theory groups

• provide a common platform for multi-messenger astroparticle physics

• provide a base for interpreting data of all experiments involved in the Alliance

• strengthen the links with astronomy, astrophysics and particle physics

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WP1: Propagation and Detection

• work on a more modular version, CRPropa 3.0, is close to completion (collaboration between Aachen, Hamburg and Wuppertal), https://crpropa.desy.de/CRPropa3

• detailed model fits to Pierre Auger data within the Monte Carlo-Astrophysics task in the Pierre Auger collaboration

• PROPOSAL algorithm for lepton propagation completed for all charged leptons, used in IceCube analysis chain

• detailed works on the small scale structure of primordial magnetic fields

• galactic cosmic ray propagation in structured magnetic fields, relevance for anisotropies (collaboration with APC)

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milestones achieved:

https://crpropa.desy.de/CRPropa3



• fundamental calculations and tests of Lorentz symmetry violations

• CASPAR coding workshop held in Hamburg 15.-19.9.2014, ca. 20 students working on DRAGON (galactic CR), CRPropa (extragalactic CR), DarkSUSY (dark matter), and gamma-astrophysics

• CASPAR workshop on galactic and extragalactic cosmic rays held in Hamburg 10.-19.9.2013, new collaborations started

• successful code retreat 12.-14.9.2012 in Zeuthen, new collaborations started

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milestones achieved (continued):



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modularized propagation code CRPropa 3.0:

Module List

Magnetic fieldTabulated data

SourceModel

Infrared backgroundRadio background...

Check isActive ?

Galacticlensing

SpectrumEvolutionDirection Composition...

External librariesSOPHIADINT...

UniformGrid...

Candidate

Deflection

Observer

Boundary Output

Interaction

position, type, ...isActive?



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CRPropa 3d Simulations: Combine Anisotropy with Spectrum and Composition

can considerably strengthen constraints on source characteristicsand distributions

see poster on CRPropa and astrophysical scenarios



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TeV scale cosmic ray anisotropies observed by IceCube and other experiments:

0 +360

0.94 0.96 0.98 1 1.02 1.04 1.06 1.08can be explained by propagation in structured magnetic fields: diffusion approximation breaks down within one magnetic scattering length from the observerG. Giacinti, G. Sigl, Phys. Rev. Lett. 109 (2012) 071101

simulated relative intensity



Next Steps:

• extend physics of and couple existing codes: GALPROP, DRAGON (-> poster), CRPropa, UHECR propagation in galactic magnetic fields, PROPOSAL

• implement more detailed models of the infrared background and extragalactic magnetic fields (collaboration with cosmologists)

• extend PROPOSAL algorithm to neutrals, adapt to GPUs • improve air shower simulations, use LHC input for more

reliable composition determination, quantify theoretical uncertainties

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WP2: Acceleration Sources

• theory of acceleration involves many orders of magnitude in length scale

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Baring

Plasma Astrophysics Effects:

• Weibel Instability • Bell instability • Plasma wake-field Acceleration

in high Poynting flux outflows

Energy Loss Processes:

• electromagnetic radiation • interactions

review Bykov et al., “Particle Acceleration in relativistic outflows”, Space Science review 173 (2012) 309



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Active Galactic NucleiAGN jets are large-scale magnetic structures How are the small-scale emission zones formed ?

Kinetic PIC simulations of shear layers in jets -> small-scale magnetic fields

By component: e-p plasma e+-e--plasma

Consequences for shear acceleration Can we distinguish?



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Active Galactic Nuclei:

2-D spatially-resolved modeling:

• Localized acceleration

• Self-consistent escape

• Self-consistent spectral evolution

• All light-travel-time effects



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Supernova Remnants:Time-dependent transport of magnetic power spectrum Ew

Solved in parallel with hydrodynamic evolution and cosmic-ray transport Drastically changes particle spectra compared to Bohm assumption (red below)



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Supernova Remnants:

PIC simulations of Bell‘s non-resonant instability

New: also spatial gradients considered. à No periodic boundaries

Realistic assessment of saturation and cosmic-ray acceleration rate

elec.

CR-el

ions

px

py

A plasma shock in the cosmic-ray precursor?



Next Steps:

• model particle acceleration and transport in AGNs, including secondary electromagnetic and neutrino fluxes, and temporal and spatial fluctuations

• inhomogeneous jets: radiation and cosmic ray production • further constrain cosmic ray source properties using data

from multiple messengers • determine origin of IceCube neutrinos

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WP3: Dark Matter and Non-Acceleration Signatures

• strong overlap with cosmology and astrophysics – gravitational growth of inhomogeneities determines

large and small-scale structure of dark matter – subtract astrophysical foregrounds for indirect dark

matter detection • strong overlap with particle physics

– dark matter candidates – collider signatures

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• investigated Feebly Interacting Massive Particle (FIMP) in models with additional scalar doublet and three singlet fermions (scotogenic model), arXiv:1405.1259

• investigated two-component (1 fermion, 1 scalar) dark matter models, arXiv:1406.0617

• higher order corrections to dark matter (co-)annihilation • electroweak corrections to direct detection cross sections

for inert Higgs dark matter • influence of non-spherical halo on dark matter detection,

arXiv:1405.6240 -> poster by Garani (Bonn)

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milestones achieved:



• minimal dark matter models • investigated relation between sterile neutrinos and

leptogenesis (arXiv:1409.0659) • computed complete SUSY-QCD corrections to neutralino

+stop-> top+gluon (arXiv:1409.2898) • joint experimental and theoretical dark matter meeting

February 2013 in Münster, mentioned in CERN courier • DM@NLO Collaboration Meeting 18 - 22 June 2012 in

Münster, O(10) participants from DESY HH, KIT, LAPTH Annecy, LPSC Grenoble, WWU Münster

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milestones achieved (continued):



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M. Klasen, J. Ruiz-Alvarez, C. Yaguna, Phys. Rev. D87 (2013) 075025

Weak corrections to direct detection of inert Higgs doublet dark matter



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Strong corrections to SUSY dark matter relic density

B. Herrmann, M. Klasen, K. Kovarik,M. Meinecke, P. Steppeler, Phys. Rev. D 89 (2014) 114012



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Viable parameter space of freeze-in singlet fermion dark matter

M. Klasen, C. Yaguna, JCAP 1311 (2013) 039



• dark matter review: M.Klasen, M.Pohl, G.Sigl • continuation of the DM @ NLO program (stop+stop->weak

and strong final states with Sommerfeld corrections), collaboration with M.Beneke (Munich) and M.Drees (Bonn)

• further investigation of minimal dark matter and neutrino sector, in particular radiative see-saw, collaboration with W.Winter (Zeuthen)

• extend existing tools to other dark matter candidates: light dark matter, little Higgs, extra dimensions, non-standard electroweak breaking

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Next Steps:


Thank you for your attention !

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report on wp1 (theory and phenomenology) at the hap ...sigl/hap-topic1-sigl.pdf · 4/11/2014 ·...

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