Measurement of the Secondary Radionuclides 10Be, 26Al, 36Cl, 54Mn, and 14C and Implications for the Galactic Cosmic-Ray Age

Details Measurement of the Secondary Radionuclides 10Be, 26Al, 36Cl, 54Mn, and 14C and Implications for the Galactic Cosmic-Ray Age Measurement of the Secondary Radionuclides 10Be, 26Al, 36Cl, 54Mn, and 14C and Implications for the Galactic Cosmic-Ray Age

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...563..768y&link_type=abstract

The Astrophysical Journal, Volume 563, Issue 2, pp. 768-792.

Astronomy and Astrophysics

Astronomy

65

Ism: Cosmic Rays, Galaxy: General, Galaxy: Halo, Ism: Abundances

Scientific paper

We report on abundance measurements of 10Be, 26Al, 36Cl, and 54Mn in the Galactic cosmic rays (GCRs) using the Cosmic-Ray Isotope Spectrometer (CRIS) instrument aboard the Advanced Composition Explorer spacecraft at energies from ~70 to ~400 MeV nucleon-1. We also report an upper limit on the abundance of GCR 14C. The high statistical significance of these measurements allows the energy dependence of their relative abundances to be studied. A steady-state, leaky-box propagation model, incorporating observations of the local interstellar medium (ISM) composition and density and recent partial fragmentation cross section measurements, is used to interpret these abundances. Using this model, the individual galactic confinement times derived using data for each species are consistent with a unique confinement time value of τesc=15.0+/-1.6 Myr. The CRIS abundance measurements are consistent with propagation through an average ISM hydrogen number density nH=0.34+/-0.04 H atoms cm-3. The surviving fractions, f, for each radioactive species have been calculated. From predictions of the diffusion models of Ptuskin & Soutoul, the values of f indicate an interstellar cosmic-ray diffusion coefficient of D=(3.5+/-2.0)×1028 cm2 s-1.

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