2018
DOI: 10.18820/23099089/actat.sup26.4
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The חֵרֶם in Joshua 6 and 7, influenced by P?

Abstract: The article engages with the old question of Priestly influence in the book of Joshua and is, to a large extent, a response to Dozeman's most recent commentary on Joshua 1-12. The article focusses specifically on the ‫ם‬ ֶ ‫ר‬ ‫חֵ‬ and argues that there are more intertextual links between the understanding of ‫ם‬ ֶ ‫ר‬ ‫חֵ‬ in Joshua 6 and 7 and texts from Deuteronomy and the Former Prophets than with Priestly texts. 1 Under "P literature", Dozeman seems to understand many other texts that could be regarded as… Show more

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“…However, this gap would be filled up by taking into account the dependence of acceleration efficiency on the first ionization potential (FIP). Meyer shows how the overabundance of elements in Galactic CRs with respect to local interstellar medium could be related to their FIPs [54]. According to his results, the abundance of sodium, whose FIP is ∼ 5 eV, in the Galactic CRs is similar to that in the interstellar medium, while the abundance of hydrogen, whose FIP is ∼ 13 eV, in the Galactic CRs is a factor of ∼ 0.03 smaller than that in the interstellar medium.…”
Section: Resultsmentioning
confidence: 99%
“…However, this gap would be filled up by taking into account the dependence of acceleration efficiency on the first ionization potential (FIP). Meyer shows how the overabundance of elements in Galactic CRs with respect to local interstellar medium could be related to their FIPs [54]. According to his results, the abundance of sodium, whose FIP is ∼ 5 eV, in the Galactic CRs is similar to that in the interstellar medium, while the abundance of hydrogen, whose FIP is ∼ 13 eV, in the Galactic CRs is a factor of ∼ 0.03 smaller than that in the interstellar medium.…”
Section: Resultsmentioning
confidence: 99%
“…The contribution from fragmentation of heavier nuclei is negligible. In all reactions, kinetic energy per nucleon is approximately conserved except for the p+p reaction, which peaks at a proton energy of ∼ 600 MeV/n and produces deuterons within a narrow energy range around 150 MeV/n (Meyer 1972). Hence, these deuterons experience DSA acceleration similarly to primary components with non-zero Y -factor, i.e., to a power-law spectrum ∼ p −α .…”
Section: Calculationsmentioning
confidence: 99%