Galactic Cosmic-Ray Manganese: ULYSSES High Energy Telescope Results

Details Galactic Cosmic-Ray Manganese: ULYSSES High Energy Telescope Results Galactic Cosmic-Ray Manganese: ULYSSES High Energy Telescope Results

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...481..241d&link_type=abstract

Astrophysical Journal v.481, p.241

Astronomy and Astrophysics

Astronomy

20

Ism: Cosmic Rays, Galaxy: Abundances, Ism: Abundances

Scientific paper

The Ulysses High Energy Telescope (HET) allows for a study of Galactic cosmic-ray manganese because of the telescope's excellent mass resolution and large collecting area. The manganese isotopes in the cosmic rays provide a means of studying the parameters of the cosmic-ray propagation in the Galaxy. Each of the isotopes probes a separate aspect of the propagation model. 53Mn, a long-lived electron capture species, measures the time between the nucleosynthesis and acceleration of the cosmic rays. There is no evidence found for a source of 53Mn, but sensitivity to this is limited. The isotope 54Mn decays in the laboratory with tau 1/2 = 312 days by electron capture, but in the cosmic rays, it has a beta - decay mode with an unmeasured partial half-life. From the HET data, this partial half-life is found to be near 1 Myr, if the iron-group cosmic rays propagate like the lighter cosmic rays. This measurement raises the lower limit on the 54Mn beta - partial half-life by a factor of ~3. The iron-group escape time from the Galaxy, even if the iron-group cosmic rays do not propagate as the lower charge cosmic rays, is found to be ~18 tau _{ beta ^-} . Finally, the stable 55Mn is found to have a source abundance, relative to iron, consistent with a solar system abundance at the source.

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