Isotopic abundances of CR sources Igor V Moskalenko

Isotopic abundances of CR sources Igor V. Moskalenko (Stanford) Andrew W. Strong (MPE) Troy A. Porter (UCSC)

CR Interactions in the Interstellar Medium SNR RX J 1713 -3946 42 sigma (2003+2004 data) X, γ e PSF HESS ISM tron +- B P diffusion He energy losses CNO reacceleration + convection e etc. π +- ro synch Chandra IC ISRF s brems gas π0 GLAST gas _ P + π- p + e- Li. Be. B He CNO Flux GLAST LAT 20 Ge. V/n BESS PAMELA Igor V. Moskalenko 2 July 5, 2007 helio-modulation ACE CR species: Ø Only 1 location Ø modulation 30 th ICRC/Merida, Mexico

GLAST LAT CR Propagation: Milky Way Galaxy 1 kpc ~ 3 x 1018 cm pc Optical image: Cheng et al. 1992, Brinkman et al. 1993 Radio contours: Condon et al. 1998 AJ 115, 1693 10 0 NGC 891 Halo 0. 1 -0. 01/ccm 40 kp c Ga 1 - s, 10 so 0/ urc cc es m 4 - 12 kp c Sun R Band image of NGC 891 1. 4 GHz continuum (NVSS), 1, 2, … 64 m. Jy/ beam Igor V. Moskalenko 3 July 5, 2007 Intergalactic space “Flat halo” model (Ginzburg & Ptuskin 1976) 30 th ICRC/Merida, Mexico

GLAST LAT A Model of CR Propagation in the Galaxy Ø Gas distribution (energy losses, π0, brems) Ø Interstellar radiation field (IC, e± energy losses) Ø Nuclear & particle production cross sections Ø Transport equations for all CR species (H-Ni, pbars, e±) Ø Energy losses: ionization, Coulomb, brems, IC, synch Ø Fix propagation parameters Ø Gamma-ray production: brems, IC, π0; synchrotron Ø Astrophysics Igor V. Moskalenko 4 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT Transport Equations ~90 (no. of CR species) sources (SNR, nuclear reactions…) diffusion convection diffusive reacceleration (Galactic wind) (diffusion in the momentum space) E-loss radioactive decay fragmentation + boundary conditions Igor V. Moskalenko 5 July 5, 2007 ψ(r, p, t) – density per total momentum 30 th ICRC/Merida, Mexico

GLAST LAT Column densities of gas • Here are examples of the resulting ‘rings’ • For the local (7. 5 -9. 5 kpc) annulus we are incorporating new intermediate latitude CO survey data (Dame 2007) and additional coverage from the NANTEN survey in the south (Onishi, Mizuno, & Fukui 2004) WCO N(H I) Igor V. Moskalenko 6 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT How It Works: Fixing Propagation Parameters E 2 Flux B/C Carbon Ek, Ge. V/nucleon In te r st e lla r Radioactive isotopes: Galactic halo size Zh Be 10/Be 9 Ek, Me. V/nucleon Using secondary/primary nuclei ratio & flux: • Diffusion coefficient and its index • Propagation mode and its parameters (e. g. , reacceleration VA, convection Vz) Zh increase Ek, Me. V/nucleon Igor V. Moskalenko 7 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT ACE Isotopic Abundances vs SS Abundances ACE Solar System Wiedenbeck+2001 Igor V. Moskalenko 8 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT Fitting procedure Solar isotopic abundances Fine adjustment of the source abundances: Propagation (GALPROP) 64 Ni … 1 H Propagation parameters Solar modulation (force-field) Igor V. Moskalenko 9 July 5, 2007 NSA=OSA*δ*(ACE-propagated) NSA=new source abundance OSA=old source abundance δ~0. 01 -0. 001 Comparison with ACE data 30 th ICRC/Merida, Mexico

GLAST LAT Quality of the Fit problematic Xsections F Ti Reacceleration Plain diffusion V 5% Reminder: fitted are the isotopic abundances while shown are elemental abund. Example: Carbon: 12 C is fitted well, but 13 C is overproduced – Xsection problems Accuracy: generally better than 5% Igor V. Moskalenko 10 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT Source Isotopic Abundances vs SS Solar system: Anders & Grevesse’ 89 Lodders’ 03 Agrees remarkably well with the latest SS abundances by Lodder for many nuclei! Igor V. Moskalenko 11 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT Detailed comparison 20 Ne 32 S 40 Ca 22 Ne 53 Mn* 41 Ca* P 15 N F 55 Mn 33 S Good Sc. Ti. V Xsections Well-known Differences in models Igor V. Moskalenko 12 July 5, 2007 30 th ICRC/Merida, Mexico

GLAST LAT Conclusions • This is the first time that a `realistic' (i. e. full spatial- and energydependence) propagation model has been used to derive isotopic source abundances for a full range of nuclei • The results are encouraging! Igor V. Moskalenko 13 July 5, 2007 30 th ICRC/Merida, Mexico