galprop tutorial
DESCRIPTION
GALPROP tutorial. Igor Moskalenko (Stanford U.). Obtaining GALPROP. The link: http://www.mpe.mpg.de/~aws/dlp/zxc/kty/v42.3p/ Contains c++, fortran routines & input files (dat-files, compass gas maps, and isrf) Dedicated GALPROP Web-site will go online soon! - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/1.jpg)
GALPROP tutorial
Igor Moskalenko (Stanford U.)
![Page 2: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/2.jpg)
Igor V. Moskalenko 2 November 17, 2005 GALPROP manual/Rome2, Italy
Obtaining GALPROP
The link:http://www.mpe.mpg.de/~aws/dlp/zxc/kty/v42.3p/
Contains c++, fortran routines & input files (dat-files, compass gas maps, and isrf)
Dedicated GALPROP Web-site will go online soon!
– Controlled changes in GALPROP: tests + documentation +…
– New version(s) + archive versions– Post relevant information: best models, gas maps, ISRF,
nuclear cross sections…– Allow for communication with users – Ability to run GALPROP on-line…
![Page 3: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/3.jpg)
Igor V. Moskalenko 3 November 17, 2005 GALPROP manual/Rome2, Italy
I/O
galdef-filegas: COR, HIR, IAQ-filesRFComposite –(fits) file
dat-files (xsec, nuc.network)
GALPROP(c++ & fortran)
nuclei –(fits) file (R=Rsun)nuclei_full –(fits) file (whole galaxy)
γ-ray emissivities –(fits) files (brems, IC, π0)γ-ray skymaps –(fits) files (rings; brems, IC, π0)
FITSGALDEF
v42.3
v42.3
FITS
sameleveldirs
Heliospheric modulation: on-the-fly in a plotting routine
![Page 4: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/4.jpg)
Igor V. Moskalenko 4 November 17, 2005 GALPROP manual/Rome2, Italy
Example Makefile
#CXX = g++-2.95#FC = g77-2.95CFITSIO = ${GLAST_EXT}/cfitsio/v2470CPPFLAGS = -O3 -Wno-deprecated -I${CFITSIO}/includeFFLAGS =LIBS = -lm -lg2cFITSLIB = -L$(CFITSIO)/lib -lcfitsio -Wl, rpath,$(CFITSIO)/libLDFLAGS = $(FITSLIB) $(LIBS)FOBJS := $(patsubst %.f,%.o,$(wildcard *.f))CCOBJS := $(patsubst %.cc,%.o,$(wildcard *.cc))galprop: ${FOBJS} ${CCOBJS} $(CXX) *.o -o $@ ${LDFLAGS}
![Page 5: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/5.jpg)
Igor V. Moskalenko 5 November 17, 2005 GALPROP manual/Rome2, Italy
Some Editing
Tested for g++ v2.9x compiler.New g++ compiler v3.x is more strict –routines require
some editing:
using namespace std;
#include<iostream>#include<cstdlib>#include<string>#include<cctype>#include<fstream>#include<cmath>
![Page 6: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/6.jpg)
Igor V. Moskalenko 6 November 17, 2005 GALPROP manual/Rome2, Italy
GALPROP Input: galdef-filesGALPROP 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…
![Page 7: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/7.jpg)
Igor V. Moskalenko 7 November 17, 2005 GALPROP manual/Rome2, Italy
Algorithm
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
-rays (IC, bremsstrahlung, πo-decay) radio: synchrotron
(i) CR –fixing propagation
(ii) γ-rays
![Page 8: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/8.jpg)
Igor V. Moskalenko 8 November 17, 2005 GALPROP manual/Rome2, Italy
GALPROP Output/FITS files
Provides literally everything:• All nuclei and particle spectra in every grid point
(x,y,R,z,E) -FITS files
Separately 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)• Output of maps separated into HI, H2, and rings
to allow fitting X, metallicity gradient etc.
![Page 9: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/9.jpg)
Igor V. Moskalenko 9 November 17, 2005 GALPROP manual/Rome2, Italy
Spatial GridsZ
R,x,y0 1 2 3 4 5 6 7
1
-1
Typical grid steps (can be arbitrary!)Δz = 0.1 kpc, ΔΔz = 0.01 kpc (gas
averaging)ΔR = 1 kpcΔE = x1.2 (log-grid)
![Page 10: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/10.jpg)
Igor V. Moskalenko 10 November 17, 2005 GALPROP manual/Rome2, Italy
GALPROP CalculationsConstraints• 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
Calculations (γ -ray related)Vectorization options Now 64 bit to allow unlimited arrays Heliospheric modulation: routinely force-field, more sophisticated 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
![Page 11: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/11.jpg)
Igor V. Moskalenko 11 November 17, 2005 GALPROP manual/Rome2, Italy
Dark Matter in GALPROP
DM annihilation products:χ0χ0−> p, pbar, e+, e−, γ
A set of routines (gen_DM_source.cc) to assign• The DM density profile (NFW, isothermal etc.)• Source functions for p, pbar, e+, e−
• Source function for γ’s• A set of user-defined parameters (10 int, 10
double precision) in galdef-file
DM annihilation products particles are propagated in the same model as CR particles.
Calculation of skymaps for DM γ-rays
![Page 12: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/12.jpg)
Igor V. Moskalenko 12 November 17, 2005 GALPROP manual/Rome2, Italy
galdef_44_599278 -I
![Page 13: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/13.jpg)
Igor V. Moskalenko 13 November 17, 2005 GALPROP manual/Rome2, Italy
galdef_44_599278 -II
![Page 14: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/14.jpg)
Igor V. Moskalenko 14 November 17, 2005 GALPROP manual/Rome2, Italy
galdef_44_599278 -III
![Page 15: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/15.jpg)
Igor V. Moskalenko 15 November 17, 2005 GALPROP manual/Rome2, Italy
galdef_44_599278 -IV
![Page 16: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/16.jpg)
Igor V. Moskalenko 16 November 17, 2005 GALPROP manual/Rome2, Italy
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 Myrradioactive ~1 Myr
& & K-captureK-capture isotopesisotopes
![Page 17: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/17.jpg)
Igor V. Moskalenko 17 November 17, 2005 GALPROP manual/Rome2, Italy
Nuclear Reaction Network
III
III
IV
Vnuc_package.cc
![Page 18: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/18.jpg)
Igor V. Moskalenko 18 November 17, 2005 GALPROP manual/Rome2, Italy
nuc_package.cc: Stable & Long-lived Isotopes
![Page 19: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/19.jpg)
Igor V. Moskalenko 19 November 17, 2005 GALPROP manual/Rome2, Italy
nuc_package.cc: Long-Lived Isotopes
![Page 20: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/20.jpg)
Igor V. Moskalenko 20 November 17, 2005 GALPROP manual/Rome2, Italy
nuc_package.cc: “Boundary” Nuclei
![Page 21: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/21.jpg)
Igor V. Moskalenko 21 November 17, 2005 GALPROP manual/Rome2, Italy
isotope_cs_eval.dat
![Page 22: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/22.jpg)
Igor V. Moskalenko 22 November 17, 2005 GALPROP manual/Rome2, Italy
Transport Equations ~90 (no. of CR Transport Equations ~90 (no. of CR species)species)
ψψ((rr,p,t),p,t) – – density per total momentum
df
Vpdtdp
p
ppppDpp
VxxD
prqttpr
31
22
][
),(),,( sources (SNR, nuclear reactions…)sources (SNR, nuclear reactions…)
convectionconvectiondiffusiondiffusion
diffusive reaccelerationdiffusive reacceleration
E-lossE-loss convectionconvection
fragmentationfragmentation radioactive decayradioactive decay
![Page 23: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/23.jpg)
Igor V. Moskalenko 23 November 17, 2005 GALPROP manual/Rome2, Italy
Finite Differencing
![Page 24: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/24.jpg)
Igor V. Moskalenko 24 November 17, 2005 GALPROP manual/Rome2, Italy
Finite Differencing: Example
![Page 25: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/25.jpg)
Igor V. Moskalenko 25 November 17, 2005 GALPROP manual/Rome2, Italy
Tri-Diagonal Matrix
![Page 26: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/26.jpg)
Igor V. Moskalenko 26 November 17, 2005 GALPROP manual/Rome2, Italy
Coefficients for the Crank-Nicholson Method
![Page 27: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/27.jpg)
Igor V. Moskalenko 27 November 17, 2005 GALPROP manual/Rome2, Italy
Near Future DevelopmentsFull 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 –param.)• Isotopic cross sections (with S.Mashnik, LANL; try to motivate BNL,
JENDL-Japan, other Nuc. Data Centers)Modeling the local structure:• Local SNRs with known positions and ages• Local Bubble, local clouds –may be done at the final calculation
step (grid bin size ??)Energy range:• Extend toward sub-MeV range to compare with INTEGRAL diffuse
emission (continuum; 511 keV line)Heliospheric modulation:• Implementing a modern formalism (Potgieter, Zank etc.)Visualization 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)
![Page 28: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/28.jpg)
Igor V. Moskalenko 28 November 17, 2005 GALPROP manual/Rome2, Italy
More developments
Point sources: develop algorithm(s) for modeling the background and interface to the rest of GLAST software
Instrumental response: how to implement Diffuse emission analysis has to include point source catalog! At least, two diffuse models: with/without the “excess” Develop test case(s) to test the accuracy of the numerical
model (simple gas distribution, no energy losses, uniform ISRF etc.)
Complete C++ package: rewrite several fortran routines in C++ Develop a fitting procedure to make automatic fitting to B/C
ratio, CR spectra and abundances Develop a dedicated Web-site:
– Controlled changes in GALPROP: tests +documentation +…– Allow for communication with users– Post relevant information: best models, gas maps, ISRF, nuclear
cross sections…– Ability to run GALPROP on-line…
![Page 29: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/29.jpg)
Igor V. Moskalenko 29 November 17, 2005 GALPROP manual/Rome2, Italy
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)
Radioactive isotopes:Galactic halo size Zh Zh increase
B/C
Be10/Be9
Inters
tellar
Ek, MeV/nucleon
Ek, MeV/nucleon
![Page 30: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/30.jpg)
Igor V. Moskalenko 30 November 17, 2005 GALPROP manual/Rome2, Italy
Peak in the Secondary/Primary Ratio
• Leaky-box model: fitting path-length distribution -> free function
B/C
• Diffusion models: Diffusive reacceleration Convection Damping of interstellar
turbulence Etc.
Accurate measurements in a wide energy range may help to distinguish between the models
EEkk, MeV/nucleon, MeV/nucleon
too sharp max?
![Page 31: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/31.jpg)
Igor V. Moskalenko 31 November 17, 2005 GALPROP manual/Rome2, Italy
Distributed Stochastic Reacceleration
Fermi 2-nd order mechanism
BB
Scattering on magnetic turbulences Dpp~ p2Va
2/DD ~ vR1/3 - Kolmogorov spectrum
Icr
E
strongreaccelerati
onweakreacceleration
ΔE
Simon et al. 1986Seo & Ptuskin
1994
1/3
Dxx = 5.2x1028 (R/3 GV)1/3cm-2 s-1
Va = 36 km s-1
γ ~ R-δ, δ=1.8/2.4 below/above 4 GV
![Page 32: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/32.jpg)
Igor V. Moskalenko 32 November 17, 2005 GALPROP manual/Rome2, Italy
Convection
Galactic wind
Escape length
Xe
E
v R-0.6
wind orturbulentdiffusion
resonantdiffusion
Jones 1979
problem: too broad sec/prim peak
D~R0.
6
Dxx = 2.5x1028 (R/4 GV)0.6cm-2 s-1
dV/dz = 10 km s-1 kpc-1
γ ~ R-δ, δ=2.46/2.16 below/above 20 GV
![Page 33: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/33.jpg)
Igor V. Moskalenko 33 November 17, 2005 GALPROP manual/Rome2, Italy
Damping of Interstellar Turbulence
p
l(p)
Iroshnikov-Kraichnan cascade:
Kolmogorov cascade:
W(k)
k
dissipation
1/1012cm1/1020cm
Simplified case:
• 1-D diffusion• No energy losses
Mean free pathnonlinearcascade
Ptuskin et al. 2003, 2005
![Page 34: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/34.jpg)
Igor V. Moskalenko 34 November 17, 2005 GALPROP manual/Rome2, Italy
Dxx – Diffusion Coefficient
Plain diffusion
Diffusivereacceleration
Reaccelerationwith damping
~R0.6
~β-3
![Page 35: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/35.jpg)
Igor V. Moskalenko 35 November 17, 2005 GALPROP manual/Rome2, Italy
• Positrons/electrons p+p->π,K->e± (MS 1998)– Dermer 1986 method: LE –Stecker Δ-isobar model (isotropic
decay), HE –scaling (inv. x-section: Stephens & Badhwar 1981), plus interpolation in between
– Pion decay “includes” polarization of muons– Kaon decay – scaling (Stephens & Badhwar 1981)
• Antiprotons (M et al. 2002)– pp Inclusive production x-section (Tan & Ng 1983)– pA, AA-> pbar –scaling using Gaisser & Schaeffer 1992 or
Simon et al. 1998 –results similar– Total inelastic x-section (p: TN’83, A: Moiseev & Ormes 1997)– p+pbar annihilation x-section = (p+pbar)tot – (p+p)tot (LE:
TN’83, HE: PDG’00 –Regge parameterization)
How It Is Really Done: Secondary Particles
![Page 36: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/36.jpg)
Igor V. Moskalenko 36 November 17, 2005 GALPROP manual/Rome2, Italy
Elemental Abundances: CR vs. Solar System
CR abundances: ACE
Solar system abundances
LiBeB
CNO
F
Fe
ScTiV
CrMn
Si
Cl
Al
O
Na
S
“input”
“output”
![Page 37: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/37.jpg)
Igor V. Moskalenko 37 November 17, 2005 GALPROP manual/Rome2, Italy
Fitting to Measured CR Abundances (ACE vs HEAO-3)
Fitting to measured CR abundances in the wide energy range (~0.1 – 30 GeV) is problematic: May indicate systematic or cross-calibration errors
![Page 38: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/38.jpg)
Igor V. Moskalenko 38 November 17, 2005 GALPROP manual/Rome2, Italy
Total Nuclear Cross Sections
Ekin, MeV/nucleonWellisch & Axen 1996
![Page 39: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/39.jpg)
Igor V. Moskalenko 39 November 17, 2005 GALPROP manual/Rome2, Italy
Isotopic Production Cross Sections of LiBeB
Semi-empirical systematics are not always correct.
Results obtained by different groups are often inconsistent and hard to test.
Very limited number of nuclear measurements:
Evaluating the cross section is very laborious and can’t be done without modern nuclear codes.
Use LANL nuclear database and modern computer codes.
![Page 40: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/40.jpg)
Igor V. Moskalenko 40 November 17, 2005 GALPROP manual/Rome2, Italy
LiBeB: Major Production Channels
Propagated Abundance * Cross-sectionPropagated Abundance * Cross-section
Be B
C
LiN
OLi6
7 9 1011
1315
14
•Well defined (65%):C12, O16 ->LiBeBN14 -> Be7
(see Moskalenko & Mashnik 28 ICRC, 2003)
•Few measurements:C13,N -> LiBeBB -> BeB•Unknown:LiBeB,C13,N -> LiBeB
“Tertiary” reactions also important! -35%
12 16
A=
![Page 41: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/41.jpg)
Igor V. Moskalenko 41 November 17, 2005 GALPROP manual/Rome2, Italy
Effect of Cross Sections: Radioactive Effect of Cross Sections: Radioactive SecondariesSecondaries
Different Different size from different ratios…size from different ratios…
Zhalo,kpc
STST
WW
2727Al+pAl+p2626AlAl
•ErrorsErrors in CR measurements (HE & LE) in CR measurements (HE & LE)•ErrorsErrors in production cross sections in production cross sections•ErrorsErrors in the lifetime estimates in the lifetime estimates•DifferentDifferent origin of elements (Local origin of elements (Local Bubble ?)Bubble ?)
natnatSi+pSi+p2626AlAl
WW
STST
TT1/21/2==??
Ek, MeV/nucleon
![Page 42: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/42.jpg)
Igor V. Moskalenko 42 November 17, 2005 GALPROP manual/Rome2, Italy
How It Is Really Done: Nucleons
• Calculated for p+A reactions and scaled for α+A (Ferrando et al. 1988)
• Calculation of total nuclear cross sections– Letaw et al. 1983– Wellisch & Axen 1996 (corrected), Z>5– Barashenkov & Polanski 2001
• Calculation of isotopic production cross sections– Webber et al. 1993 (non-renormalized, renormalized); E>200
MeV/nucleon, essentially flat– Silberberg & Tsao 2000 (non-renormalized, renormalized); claim that it
works at all energies, but is problematic sometimes– Fits to the available data (LANL, Webber et al., etc.) in the form of a
function or a table (see .dat files), but data may not be always available– Use the best of all three, but very time consuming work
• Nuclear reaction network– Nuclear Data Tables (includes several decay channels + branching)– Standard β± -decay, emission of p, n– K-capture isotopes can be treated separately
![Page 43: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/43.jpg)
Igor V. Moskalenko 43 November 17, 2005 GALPROP manual/Rome2, Italy
Interstellar Gas► Extend CO surveys to high latitudes
– newly-found small molecular clouds will otherwise be interpreted as unidentified sources, and clearly limit dark matter studies
► C18O observations (optically thin tracer) of special directions (e.g. Galactic center, arm tangents)
– assess whether velocity crowding is affecting calculations of molecular column density, and for carefully pinning down the diffuse emission
20
0
-20
-40
Gal
actic
Lat
itude
220 200 180 160 140 120 100 80 60 40 20 0
CfA 1.2mGalactic Longitude
Dam
e, Hartm
ann, & Thaddeus (2001)
Dam
e & Thaddeus (2004)
![Page 44: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/44.jpg)
Igor V. Moskalenko 44 November 17, 2005 GALPROP manual/Rome2, Italy
Distribution of Interstellar Gas
• Neutral interstellar medium– 21-cm H I & 2.6-mm CO (stand in for H2)
• Near-far distance ambiguity, rotation curve, optical depth effects, …
Dame et al.(1987)
Hartmann &Burton (1997)
(25°, 0°)
W. Keel
CO
H IG.C.
25°
Seth Digel
![Page 45: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/45.jpg)
Igor V. Moskalenko 45 November 17, 2005 GALPROP manual/Rome2, Italy
Seth Digel’05
![Page 46: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/46.jpg)
Igor V. Moskalenko 46 November 17, 2005 GALPROP manual/Rome2, Italy
Gas Distribution
Sun
Molecular hydrogen H2 is traced using J=1-0 transition of 12CO, concentrated mostly in the plane (z~70 pc, R<10 kpc)
Atomic hydrogen H I (radio 21 cm) has a wider distribution (z~1 kpc, R~30 kpc)
Ionized hydrogen H II (visible, UV, X) small proportion, but exists even in halo (z~1 kpc)
Z=0,0.1,0.2 kpc
![Page 47: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/47.jpg)
Igor V. Moskalenko 47 November 17, 2005 GALPROP manual/Rome2, Italy
Gas Rings: HI (Inner & Outer Galaxy)
Seth Digel’05
![Page 48: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/48.jpg)
Igor V. Moskalenko 48 November 17, 2005 GALPROP manual/Rome2, Italy
Seth Digel’05
Gas Rings: HI (Our Neighborhood)
![Page 49: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/49.jpg)
Igor V. Moskalenko 49 November 17, 2005 GALPROP manual/Rome2, Italy
• Bremsstrahlung (Koch & Motz 1959, SMR2000) –many different regimes:– LE: 0.01 < Ekin < 0.07 MeV –nonrelativistic non-screened brems– Intermediate: 0.07 < Ekin <2 MeV– HE: Ekin > 2 MeV arbitrary screening: unshielded charge, 1-, 2-
electron atoms (form factors, Hylleraas, Hertree-Fock wave functions)
– Fano-Sauter limit: k->Ekin • “Anisotropic” IC (MS2000)
– Takes into account the anisotropic angular distribution of background photons
• Neutral pion decay (see “secondary positrons/electrons”)• Synchrotron radiation (Ginzburg 1979, Ghisellini et al. 1988)
– Averaging over pitch angle– Uses total magnetic field (regular + random)
• Emissivities: uses “real” H2, H I gas column densities (“rings”)• Skymap calculations: integration over the line of sight
How It Is Really Done: Gammas
![Page 50: GALPROP tutorial](https://reader036.vdocument.in/reader036/viewer/2022081507/56815df5550346895dcc2cf6/html5/thumbnails/50.jpg)
Igor V. Moskalenko 50 November 17, 2005 GALPROP manual/Rome2, Italy
Uncertainties in the Propagation Models• Production cross sections of isotopes and pbars
Typical errors ~50% Fitting to B/C ratio may introduce errors in Dxx
• Propagation models and parameters Gas distribution in the Galaxy
Ambient spectrum of CR (solar modulation, GeV excess in γ’s !) Current knowledge of CR diffusion
• Heliospheric modulation Depends on rigidity Similar for all nuclei A/Z~ +2
Different for protons A/Z=+1 and pbars A/Z=-1 • Systematic errors of measurements
Difficult to account for
Simultaneous measurements of Li, Be, B, C, secondary e+, p in a wide energy range ~100 MeV/nucleon – 100 GeV/nucleon are needed to understand CR propagation and distinguish between the models: looking forward to Pamela launch!
_