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Author Komiya, Yutaka ♦ Shigeyama, Toshikazu
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ ACCELERATION ♦ COSMIC RADIATION ♦ ELEMENT ABUNDANCE ♦ ENERGY LOSSES ♦ ENERGY SPECTRA ♦ FLUCTUATIONS ♦ METEORITES ♦ NEUTRON STARS ♦ NUCLEOSYNTHESIS ♦ R PROCESS ♦ SOLAR SYSTEM ♦ SPALLATION ♦ SUPERNOVA REMNANTS ♦ TRANSPORT THEORY ♦ UNIVERSE
Abstract Neutron star mergers (NSMs) are one of the most plausible sources of r -process elements in the universe. Therefore, NSMs can also be a major source of ultra-heavy elements in cosmic rays. In this paper, we first estimate the contribution of r -process elements synthesized in NSMs to the ultra-heavy element cosmic rays (UHCRs) by calculating transport equations that take into account energy loss processes and spallations. We show that the flux of UHCRs accelerated by the NSMs themselves fluctuates by many orders of magnitude on a timescale of several million years and can overwhelm UHCRs accelerated by supernova remnants (SNRs) after an NSM takes place within a few kiloparsec from the solar system. Experiments with very long exposure times using meteorites as UHCR detectors can detect this fluctuation. As a consequence, we show that if NSMs are the primary source of UHCRs, future experiments using meteorites may be able to reveal the event history of NSMs in the solar vicinity. We also describe a possible difference in the abundance pattern and energy spectrum of UHCRs between NSM and SNR accelerations.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-09-10
Publisher Place United States
Journal Astrophysical Journal
Volume Number 846
Issue Number 2


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