galprop: principles, internal structure, recent results ... · pdf fileigor v. moskalenko...
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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
GALPROP: principles, inputs/outputs, calculationsGALPROP: principles, inputs/outputs, calculationsRecent results (Recent results (GeVGeV excess & excess & pbarspbars, extragalactic background), extragalactic background)Dark MatterDark MatterNear future developmentsNear future developments
Igor V. Moskalenko/NASA-GSFC 2 GLAST meeting/SLAC 2004/09/27-30
Transport EquationTransport Equation
df
Vpdtdp
p
ppppDpp
VxxD
prqttpr
τψ
τψ
ψψ
ψ
ψψ
ψ
−−
⋅∇−
∂∂
−
∂∂
∂∂
+
−∇⋅∇+
=∂
∂
rr
rrr
rr
31
22
][
),(),,( sources (SNR, nuclear reactions…)sources (SNR, nuclear reactions…)
convectionconvectiondiffusiondiffusion
diffusive reaccelerationdiffusive reacceleration
EE--lossloss convectionconvection
fragmentationfragmentation radioactive decayradioactive decay
ψψ((rr,p,t),p,t) –– density per total momentum
Igor V. Moskalenko/NASA-GSFC 3 GLAST meeting/SLAC 2004/09/27-30
CR Propagation: Milky Way Galaxy
Halo
Gas, sources
100 pc
40 kpc
Sun
4-12
kpc
0.1-0.01/ccm
1-100/ccm
Intergalactic space
1 kpc~3x1018 cmOptical image: Cheng et al. 1992, Brinkman et al. 1993Radio contours: Condon et al. 1998 AJ 115, 1693
R Band image of NGC8911.4 GHz continuum (NVSS), 1,2,…64 mJy/ beam
NGC891
Igor V. Moskalenko/NASA-GSFC 4 GLAST meeting/SLAC 2004/09/27-30
CR Interactions in the Interstellar Medium
e+-
Sources:SNRs, Shocks,Superbubbles
Particle accelerationPhoton emission P
HeCNO
X,γ
gas
gas
B
ISRF
π
e+-
+-
P_
LiBeB
ISM
diffusionenergy losses
reaccelerationconvection
etc. π0
synchrotronsynchrotron
IC
bremss
Chandra
ACE
BESS
Halo
disk
escape
HeCNOsolar
modulation
AMS
p
GLAST
Igor V. Moskalenko/NASA-GSFC 5 GLAST meeting/SLAC 2004/09/27-30
GALPROP Input: galdef-files
GALPROP is parameter-driven (user can specify everything!)Grids• 2D/3D –options; symmetry options (full 3D, 1/8 -quadrants)• Spatial, energy/momentum, latitude & longitude grids• Ranges: energy, R, x, y, z, latitude & longitude • Time stepsPropagation parameters• Dxx, VA, VC & injection spectra (p,e)• X-factors (including R-dependence)Sources• Parameterized distributions• Known SNRs• Random SNRs (with given/random spectra), time dependent eq.Other• Source isotopic abundances, secondary particles (pbar , e±, γ,
synchro), anisotropic IC, energy losses, nuclear production cross sections…
Igor V. Moskalenko/NASA-GSFC 6 GLAST meeting/SLAC 2004/09/27-30
Grids
Z
R,x,y0 1 2 3 4 5 6 7
1
-1
Typical grid steps (can be arbitrary!)∆z = 0.1 kpc, ∆∆z = 0.01 kpc (gas averaging)∆R = 1 kpc∆E = x1.2 (log-grid)
Igor V. Moskalenko/NASA-GSFC 7 GLAST meeting/SLAC 2004/09/27-30
Gas Distribution
Sun
Molecular hydrogen H2is traced using J=1-0 transition of 12CO,concentrated mostly in the plane (z~70 pc, R<10 kpc)
Atomic hydrogen H Ihas a wider distribution (z~1 kpc, R~30 kpc)
Ionized hydrogen H II –small proportion, but exists even in halo (z~1 kpc)
Igor V. Moskalenko/NASA-GSFC 8 GLAST meeting/SLAC 2004/09/27-30
Interstellar Radiation FieldEnergy density
Energy density Sun
• Stellar• Dust• CMB
Igor V. Moskalenko/NASA-GSFC 9 GLAST meeting/SLAC 2004/09/27-30
Nuclear Reaction Network+Cross Sections
p,EC,p,EC,ββ++
ββ--, , nn
Be7 Be10
Al26
Cl36
Mn54
Plus some dozens of more complicated reactions.But many cross sections are not well known…
V49
Ca41
Cr51
Fe55Co57
Ar37
SecondarySecondary,,radioactive ~1 radioactive ~1 MyrMyr
& & KK--capturecapture isotopesisotopes
Igor V. Moskalenko/NASA-GSFC 10 GLAST meeting/SLAC 2004/09/27-30
Propagation parameters:Diffusion coeff., halo size, Alfvén speed,
convection velosity…
Energy markers:Reacceleration, solar
modulation
Local medium:Local Bubble
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
tertiary source functionstertiary propagation
γ-rays (IC, bremsstrahlung, πo-decay) radio: synchrotron
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
Reacceleration Model: Secondary PbarsReacceleration Model: Secondary Pbars
B/C ratio
Ek, GeV/nucleon
Antiproton flux
Ek, GeV
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…
Ω ≡ ρ/ρcrit
Ωtot =1.02 +/−0.02ΩMatter =4.4% +/−0.4%ΩDM =23% +/−4%ΩVacuum =73% +/−4%
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
pbars
e+
γ
Supersymmetry:MSSMLightest neutralino χ0
mχ ≈ 100-500 GeVS=½ Majorana particlesχ0χ0−> p, pbar, e+, e−, γ
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
Longitude Profiles |b|<5Longitude Profiles |b|<5°°
50-70 MeV
2-4 GeV
0.5-1 GeV
4-10 GeV
Igor V. Moskalenko/NASA-GSFC 31 GLAST meeting/SLAC 2004/09/27-30
Latitude Profiles: Inner Galaxy
50-70 MeV 2-4 GeV0.5-1 GeV
4-10 GeV 20-50 GeV
Igor V. Moskalenko/NASA-GSFC 32 GLAST meeting/SLAC 2004/09/27-30
Latitude Profiles: Outer Galaxy
50-70 MeV
2-4 GeV
0.5-1 GeV
4-10 GeV
Igor V. Moskalenko/NASA-GSFC 33 GLAST meeting/SLAC 2004/09/27-30
Extragalactic GammaExtragalactic Gamma--Ray BackgroundRay Background
E, MeVE, MeV
EE22xFxF
Sreekumar et al. 1998Sreekumar et al. 1998
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
Thank you !