Isotopic abundances of CR sources

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Presentation transcript:

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

CR Interactions in the Interstellar Medium 42 sigma (2003+2004 data) HESS SNR RX J1713-3946 PSF ISM X,γ e + - synchrotron Chandra B IC P He CNO ISRF diffusion energy losses reacceleration convection etc. bremss gas e + - π π + - GLAST gas P _ π + - p LiBeB Flux He CNO e + - 20 GeV/n BESS CR species: Only 1 location modulation PAMELA ACE helio-modulation

CR Propagation: Milky Way Galaxy 1 kpc ~ 3x1018 cm Optical image: Cheng et al. 1992, Brinkman et al. 1993 Radio contours: Condon et al. 1998 AJ 115, 1693 NGC891 100 pc Halo Gas, sources 40 kpc 0.1-0.01/ccm 1-100/ccm Sun 4-12 kpc Intergalactic space R Band image of NGC891 1.4 GHz continuum (NVSS), 1,2,…64 mJy/ beam “Flat halo” model (Ginzburg & Ptuskin 1976)

A Model of CR Propagation in the Galaxy Gas distribution (energy losses, π0, brems) Interstellar radiation field (IC, e± energy losses) Nuclear & particle production cross sections Transport equations for all CR species (H-Ni, pbars, e±) Energy losses: ionization, Coulomb, brems, IC, synch Fix propagation parameters Gamma-ray production: brems, IC, π0; synchrotron Astrophysics

Transport Equations ~90 (no. of CR species) sources (SNR, nuclear reactions…) diffusion convection (Galactic wind) diffusive reacceleration (diffusion in the momentum space) E-loss fragmentation radioactive decay ψ(r,p,t) – density per total momentum + boundary conditions

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)

How It Works: Fixing Propagation Parameters E2 Flux B/C Carbon Radioactive isotopes: Galactic halo size Zh Interstellar Ek, GeV/nucleon Be10/Be9 Ek, MeV/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, MeV/nucleon

ACE Isotopic Abundances vs SS Abundances Solar System Wiedenbeck+2001

Fitting procedure Solar isotopic abundances Propagation (GALPROP) 64Ni … 1H Comparison with ACE data Fine adjustment of the source abundances: NSA=OSA*δ*(ACE-propagated) Solar modulation (force-field) Propagation parameters NSA=new source abundance OSA=old source abundance δ~0.01-0.001

Quality of the Fit problematic Xsections F V Ti 5% Reminder: Reacceleration Plain diffusion Ti 5% Reminder: fitted are the isotopic abundances while shown are elemental abund. Example: Carbon: 12C is fitted well, but 13C is overproduced – Xsection problems Accuracy: generally better than 5%

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!

Detailed comparison 20Ne 32S 53Mn* 40Ca 41Ca* 22Ne P F 55Mn 15N 33S Good Xsections Well-known Differences in models ScTiV

Conclusions This is the first time that a `realistic' (i.e. full spatial- and energy-dependence) propagation model has been used to derive isotopic source abundances for a full range of nuclei The results are encouraging!