Astroparticle physics: interdisciplinary approach

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Astroparticle physics interdisciplinary approach
Extragalactic model
100Mpc
Galactic model
200kpc
Local Bubble
100pc
heliosphere
magnetosphere
detector
Exotics
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Extragalactic model
Cosmic Rays -sources (AGN...) acceleration
mechanism, chemical composition (Zgt1?)
(Egt1015eV) -propagation (diffusion in Bfield
0.01-1mG) (Sigl,Biermann et al) -gamma EGB ,
contribution at E1GeV for polar regions.
Experiments EAS Hires, Auger (2005) ,OWL,
EUSO(gt2010) GLAST (ex.gamma)
Large scale structures and DM(simulations) -
cosmological Nbody (NFW, Moore., et al),
analytical (A.V.Gurevich et al) large scale
anisotropy(anisotropic infall, caustics) -
inflation, dark energy, DM, toplogical objects -
baryogenesis, antimatter Relics - CMB, WIMPS,
neutrino, antimatter-gt universe composition
Experiments astro surveys Plank CMB (2008),
Ligo GW(2010), Relic n Auger , OWL, EUSO (relic
neutrino UHEneutrino Z resonance,EeasgtGZK)
Important for gamma and DM annihilation. Link to
cosmology
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Galactic model
escape
Leaky box r 20kpc zh/- 4-6kpc
Va
Vconv
R?8kpc
z
r
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Galactic model
Cosmic Rays(10 Mev- 1000GeV) - sources (SNR),
injection spectrum(1.6-2.5, breaks) , spatial
distribution - propagation LBoxrealistic gas,
ISRF,, losses . Conventional model - fit to
the local p,e spectrums, BC,Be -gt problem with
gamma(EGRET), ep,pb Experiments Pamela(2005),
AMS(2008), GLAST(2008) ballon(BESS, CAPRICE,
HEAT,ISOMAX)
Dark Matter - bulk profile Nbody
-cusped(B.Moore, NFW), rotation curve
decomposition-gtisothermal like (Burkert, Bloch) -
interaction with baryionic matter (compression,
friction, clumps destruction) - DM clumps -gt
connection to cosmology (V.Beresinskii,
V.Dokuchaev et al) - DM annihilation.
cc-gtWW-gtnnX(hard Mc), -gtbbar-gtXn (soft) - DM
candidates Experiments GLAST, AMS rotation
curves decomposition
Most developed area, many codes are available
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Local Bubble
Galactic average spectrums are different from
the localy measured. 'Optimized' models (Strong,
Moskalenko )
100 pc cavity after 20 SRN explosion during 10
Myr wash out CR gas density 10-3 (Ptuskin,
Breitschwerdt, Maiz-Apellaniz et al)
Propagation in LB - boundary condidtions from
the galactic model - diffusion similar to galaxy
, diffusion coefficient is smaller (Taillet,
Maurin et al) can be determined from heavy
nucleons Experiments TIGER, ECCO AMS, PAMELA
(decondary heavy nucleons)
CR long term variations factor of 5 in 100000
years
Very litle is known many free parameters...
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Heliosphere and magnetosphere
Solar modulation - affect all CR with Rlt10
GeV - force field FmodFLIS Ekin(Ekin2M)/T(T2M)
TEkinZ?/A, might be not enough. ? - is
difficult to measure.
??? ??? ??? ?
Contributes to uncetarnities....
Magnetosphere - internal, external B field model
(Tsyganenko et al, GEOPACK) - geomagnetical
cutoff - secondary trapped particles need
back tracing in real time field. (done in AMS01
for.ex)
Is working...
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Dark Matter finder software package
Susy mass spectrum
Annihilation yields
hadronisation tables
Plotting and analysis of signal and bkg.
Check relic density
Verification of the halo profile