Igor V. Igor V. Moskalenko Moskalenko & & Andy W. Strong Andy W. Strong NASA/GSFC NASA/GSFC MPE, Germany MPE, Germany with with Olaf Olaf Reimer Reimer Bochum Bochum , Germany , Germany Topics to cover: Topics to cover: GALPROP: principles, internal structure, GALPROP: principles, internal structure, recent results, and perspective recent results, and perspective GALPROP: principles, inputs/outputs, calculations GALPROP: principles, inputs/outputs, calculations Recent results ( Recent results ( GeV GeV excess & excess & pbars pbars , extragalactic background) , extragalactic background) Dark Matter Dark Matter Near future developments Near future developments
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Igor V. Igor V. MoskalenkoMoskalenko && Andy W. StrongAndy W. StrongNASA/GSFC NASA/GSFC MPE, GermanyMPE, Germany
withwithOlafOlaf ReimerReimer
BochumBochum, Germany, Germany
Topics to cover:Topics to cover:
GALPROP: principles, internal structure, GALPROP: principles, internal structure, recent results, and perspectiverecent results, and perspective
Material & acceleration sites, nucleosynthesis (r-
vs. s-processes)
Stable secondaries: Li, Be, B, Sc, Ti, V
Radio (t1/2~1 Myr): 10Be, 26Al, 36Cl, 54Mn
K-capture: 37Ar,49V, 51Cr, 55Fe, 57Co
Short t1/2 radio 14C & heavy Z>30
Heavy Z>30: Cu, Zn, Ga, Ge, Rb
Nucleo-synthesis:
supernovae,
early universe,
Big Bang…
Solar
modulation
Diffuse γ-raysGalactic,
extragalactic:blazars, relic
neutralino
Dark Matter(p,đ,e+,γ)-
Nuclear component in CR: What we can learn?
Igor V. Moskalenko/NASA-GSFC 11 GLAST meeting/SLAC 2004/09/27-30
Fixing Propagation Parameters: Standard Way
Using secondary/primary nuclei ratio:•Diffusion coefficient and its index•Propagation mode and its parameters (e.g., reacceleration VA, convection Vz)
Zh increase
B/C
Be10/Be9
Inte
rste
llar
Ek, MeV/nucleon
Ek, MeV/nucleon
Radioactive isotopes:Galactic halo size Zh
Igor V. Moskalenko/NASA-GSFC 12 GLAST meeting/SLAC 2004/09/27-30
Peak in the Secondary/Primary Ratio
• Leaky-box model: fitting path-length distribution -> free function
B/C
• Diffusion models:Diffusive reaccelerationConvectionDamping of interstellar turbulenceEtc.
Measuring many isotopes in CR simultaneously may help to distinguish
Igor V. Moskalenko/NASA-GSFC 13 GLAST meeting/SLAC 2004/09/27-30
Heliosphere
Flux
20 GeV/n
Igor V. Moskalenko/NASA-GSFC 14 GLAST meeting/SLAC 2004/09/27-30
Electron Fluctuations/SNR stochastic events
GeV electrons 100 TeV electronsGALPROP/Credit S.Swordy
Energy losses
107 yr
106 yr
Bremsstrahlung
1 TeV
Ionization
Coulomb
IC, synchrotron
1 GeV
Ekin, GeV
E(dE
/dt)
-1,y
r
Electron energy loss timescale:1 TeV: ~300 000 yr100 TeV: ~3 000 yr
Igor V. Moskalenko/NASA-GSFC 15 GLAST meeting/SLAC 2004/09/27-30
CR Variations in Space & Time
More frequent SN in the spiral arms
Historical variations Historical variations of CR of CR intensity over intensity over 150 000 yr150 000 yr(Be(Be1010 in South Polar ice)in South Polar ice)
Konstantinov et al. 1990Electron/positron energy losses Different “collecting” areas A vs. p
Igor V. Moskalenko/NASA-GSFC 16 GLAST meeting/SLAC 2004/09/27-30
GALPROP Output/FITS files
Provides literally everything:• All nuclei and particle spectra in every grid point
(x,y,R,z,E) -FITS filesSeparately for π0-decay, IC, bremsstrahlung:• Emissivities in every grid point (x,y,R,z,E,process)• Skymaps with a given resolution (l,b,E,process)“CONSUMERS:”• AMS, Pamela – dark matter searches• ACE, TIGER – interpretation of isotopic abundances• HEAT – electrons, positrons• GLAST(?) – spectrum of the diffuse emission &
background model
Igor V. Moskalenko/NASA-GSFC 17 GLAST meeting/SLAC 2004/09/27-30
algorithmnumerical solution of cosmic-ray transport2D or 3D gridtime-independent or time-dependent
primary source functions (p, He, C .... Ni)source abundances, spectraprimary propagation -starting from maxA=64
source functions (Be, B...., e+,e-, pbars)using primaries and gas distributions secondary propagation
Igor V. Moskalenko/NASA-GSFC 18 GLAST meeting/SLAC 2004/09/27-30
GALPROP Calculations
Constraints• Bin size (x,y,z) depends on the computer speed, RAM; final run can be done
on a very fine grid ! • No other constraints ! –any required process/formalism can be implemented;
vectorization !!
Calculations (γ -ray related)Vectorization optionsHeliospheric modulation: routinely force-field, can use Potgieter model
1. For a given propagation parameters: propagate p, e, nuclei, secondaries(currently in 2D)
2.The propagated distributions are stored3.With propagated spectra: calculate the emissivities (π0-decay, IC, bremss)
in every grid point4. Integrate the emissivities over the line of sight: • GALPROP has a full 3D grid, but currently only 2D gas maps (H2, H I, H II)• Using actual annular maps (column density) at the final step• High latitudes above b=40˚ -using integrated H I distribution
Igor V. Moskalenko/NASA-GSFC 19 GLAST meeting/SLAC 2004/09/27-30
Near Future Developments
Full 3D Galactic structure:• 3D gas maps (from S.Digel, S.Hunter and/or smbd else)• 3D interstellar radiation & magnetic fields (A.Strong & T.Porter)Cross sections:• Blattnig et al. formalism for π0-production• Diffractive dissociation with scaling violation (T.Kamae)• Isotopic cross sections (with S.Mashnik, LANL; try to motivate BNL,
JENDL-Japan, other Nuc. Data Centers)Energy range:• Extend toward sub-MeV range to compare with INTEGRAL diffuse
emission (continuum; 511 keV line)Modeling the local structure:• Local SNRs with known positions and ages• Local Bubble –may be done at the final calculation stepHeliospheric modulation:• Implementing a complimentary drift model by M.PotgieterVisualization tool (started) using the classes of CERN ROOT package:
images, profiles, and spectra from GALPROP to be directly compared with data
Improving the GALPROP module structure (for DM studies) & developing a dedicated Web-site to allow for a communication with users
Igor V. Moskalenko/NASA-GSFC 20 GLAST meeting/SLAC 2004/09/27-30
Recent results
Igor V. Moskalenko/NASA-GSFC 21 GLAST meeting/SLAC 2004/09/27-30
Wherever you look, the GeV γ - ray excess is there !
4a-f
Igor V. Moskalenko/NASA-GSFC 22 GLAST meeting/SLAC 2004/09/27-30
Igor V. Moskalenko/NASA-GSFC 23 GLAST meeting/SLAC 2004/09/27-30
Positron Excess ?
HEAT (Coutu et al. 1999)
Are all the excesses Are all the excesses connected somehow ?connected somehow ?A signature of a new A signature of a new physics (DM) ?physics (DM) ?
Caveats:Systematic errors ? Systematic errors ? A local source of A local source of primary positrons ?primary positrons ?Large ELarge E--losses losses --> local > local spectrum…spectrum…
Leaky-BoxGALPROP
e+/e
E, GeV1 10 100
Igor V. Moskalenko/NASA-GSFC 24 GLAST meeting/SLAC 2004/09/27-30
Matter, Dark Matter, Dark Energy…
Dark Energy
Dark Matter
Visible atoms
SUSY DM candidate has also other reasons to exist -particle physics…
Supersymmetry is a mathematically beautiful theory, and would give rise to a very predictive scenario, if it is not broken in an unknown way which unfortunately introduces a large number of unknown parameters…
Lars Bergström (2000)
Igor V. Moskalenko/NASA-GSFC 25 GLAST meeting/SLAC 2004/09/27-30
Example “Global Fit:” diffuse γ’s, pbars, positrons GALPROP/W. de Boer et al. hepGALPROP/W. de Boer et al. hep--ph/0309029ph/0309029
Look at the combined (pbar,e+,γ) dataPossibility of a successful “global fit” can not be excluded -non-trivial !If successful, it may provide a strong evidence for the SUSY DM
Igor V. Moskalenko/NASA-GSFC 26 Nuclear Data-2004/09/28, Santa Fe
GeV excess: Optimized model
protons
x1.8
antiprotons
GeV excess: Optimized modelUses Uses all skyall sky and antiprotons & gammasand antiprotons & gammasto fix the nucleon and electron spectrato fix the nucleon and electron spectra
Uses antiprotons to fix the intensity of CR nucleons @ HEUses gammas to adjust
the nucleon spectrum at LEthe intensity of the CR electrons
(uses also synchrotron index)Uses EGRET data up to 100 GeV
electrons
x4x4
Igor V. Moskalenko/NASA-GSFC 27 GLAST meeting/SLAC 2004/09/27-30
Diffuse Gammas from Secondary Positrons/Electrons
e+~0.1e-
e+/e
electrons
positrons
gammas
e+=e-
sec.e-=10%
Importa
nt below
200
MeV
Heliosphere Interstellar
Igor V. Moskalenko/NASA-GSFC 28 GLAST meeting/SLAC 2004/09/27-30
Anisotropic Inverse Compton Scattering
Electrons in the halo see anisotropic radiationObserver sees mostly head-on collisions
e-
e-
head-on:large boost &more collisions
γγ
small boost &less collisions
γ
sun
Energy density
Z, kpc
R=4 kpc
Important @ high latitudes !
Igor V. Moskalenko/NASA-GSFC 29 GLAST meeting/SLAC 2004/09/27-30
Diffuse Gammas at Different Sky RegionsDiffuse Gammas at Different Sky Regions
Hunter et al. region:l=300°-60°,|b|<10°
Intermediate latitudes:l=0°-360°,10°<|b|<20°
Outer Galaxy:l=90°-270°,|b|<10°
Intermediate latitudes:l=0°-360°,20°<|b|<60°
Igor V. Moskalenko/NASA-GSFC 30 GLAST meeting/SLAC 2004/09/27-30
Strong et al. 2004Strong et al. 2004Elsaesser & Mannheim,
astro-ph/0405235
• Blazars• Cosmological neutralinos
Predicted vs. observedPredicted vs. observed
Igor V. Moskalenko/NASA-GSFC 34 GLAST meeting/SLAC 2004/09/27-30
Distribution of CR Sources & Gradient in the CO/H2
CR distribution from diffuse gammas (Strong & Mattox 1996)SNR distribution (Case &
Bhattacharya 1998)Pulsar distribution (Lorimer 2004)
sun
XXCOCO=N(H=N(H22)/W)/WCOCO::Histo –This work, Strong et al.’04----- -Sodroski et al.’95,’971.9x1020 -Strong & Mattox’96~Z-1 –Boselli et al.’02~Z-2.5 -Israel’97,’00, [O/H]=0.04,0.07 dex/kpc
Igor V. Moskalenko/NASA-GSFC 35 GLAST meeting/SLAC 2004/09/27-30
Again Diffuse Galactic Gamma Rays
Very good agreement !Very good agreement !
More IC in the GC –better agreement !
The pulsar distribution vs. R falls too fast OR
larger H2/CO gradient
Igor V. Moskalenko/NASA-GSFC 36 GLAST meeting/SLAC 2004/09/27-30
Conclusions I
Accurate measurements of diffuse gamma rays, secondary antiprotons, and other CR species simultaneously may provide a new vital information for Astrophysics – in broad sense, Particle Physics, and Cosmology.
Hunter et al. region:l=300°-60°,|b|<10°
Dark MatterGamma rays: GLAST is scheduled to launch in 2007 – diffuse gamma rays is one of its priority goals
B/C
Zh increase
Be10/Be9 CR species: New measurements at LE & HE simultaneously are highly desirable (Pamela, S-TIGER, AMS…), sec. positrons !
Igor V. Moskalenko/NASA-GSFC 37 GLAST meeting/SLAC 2004/09/27-30
Conclusions II
Antiprotons: Pamela (2005), AMS (2008) and a new BESS-polar instrument to fly a long-duration balloon mission (in 2004, 2006…), we thus will have more accurate and restrictive antiproton data
HE electrons: Several missions are planned to target specifically HE electrons
We must be ready!GALPROP is a propagation model to
play now
Igor V. Moskalenko/NASA-GSFC 38 GLAST meeting/SLAC 2004/09/27-30