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The recent observations of an approximately linear relationship
between both Be and B and
iron in metal-poor stars has led to a reassessment of the origin of the
light elements in the early Galaxy. In addition to standard secondary
production of BeB, it is necessary to introduce a
production mechanism which is independent of the interstellar
metallicity (primary), and in which freshly synthesized C, O and
He are accelerated by supernova shock waves. Primary mechanisms are
expected to be dominant at low metallicity. At metallicities higher than
[{\rm O/H}] \ga -1.75,
some existing data indicate that secondary production is
dominant. In this paper, we focus on
the secondary process, related to the standard Galactic cosmic
rays, and
we examine the cosmic ray energy requirements
for both present and past epochs.
We find the
power input to maintain
the present-day Galactic cosmic ray
flux is about
1.5 1041 erg/s = 5 1050 erg/century;
this estimate includes energy losses from
both the escape of
high-energy particle and ionization losses from low-energy
particles.
This implies that, if supernovae are the sites of
cosmic ray acceleration, the fraction of explosion energy
going to accelerated particles
is about ~30% , a value which we obtain consistently
both from considering the present cosmic ray flux and confinement
and from the present 9Be and 6Li abundances.
Using the abundances of 9Be (and 6Li) in metal-poor halo stars,
we extend the analysis to show the effect of the interstellar
gas mass on the standard Galactic cosmic ray
energetic constraints on
models of Li, Be, and B evolution.
The efficiency of the beryllium production per erg
may be enhanced in the past
by a factor of about 10; thus the energetic requirement by itself
cannot be used to rule out a secondary origin of light elements.
Only a
clear and indisputable observational determination
of the O-Fe relation in the halo will discriminate between the two
processes
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