Distributed Radioactivities

Diehl, R.; Hartmann, D. H.; Prantzos, Nikos

doi:10.1007/978-3-319-91929-4_7

Cited by 3 publications

(2 citation statements)

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“…The 26 Al mass estimate was revised and refined, as better geometrical models for the assumed source distribution in the Galaxy could be developed, also to account for foreground emission from more-nearby massive-star groups, which reduces the estimated mass of 26 Al in the Galaxy. The total mass of 26 Al in the Galaxy is now estimated to be between 1.8 and 2 M [40,41]. The value of the Galactic corecollapse supernova rate therefore was updated with better estimates of the 26 Al mass and of model yields to 1.4±1.1 century −1 [40,41], or one such supernova in our Galaxy every 71 years.…”

Section: Astrophysical Studies Using Radioactivitymentioning

confidence: 99%

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Radioactive Decay

Diehl¹

2022

Preprint

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Radioactive decay of unstable atomic nuclei leads to liberation of nuclear binding energy in the forms of gamma-ray photons and secondary particles (electrons, positrons); their energy then energises surrounding matter. Unstable nuclei are formed in nuclear reactions, which can occur either in hot and dense extremes of stellar interiors or explosions, or from cosmic-ray collisions. In high-energy astronomy, direct observations of characteristic gamma-ray lines from the decay of radioactive isotopes are important tools to study the process of cosmic nucleosynthesis and its sources, as well as tracing the flows of ejecta from such sources of nucleosynthesis. These observations provide a valuable complement to indirect observations of radioactive energy deposits, such as the measurement of supernova light in the optical. Here we present basics of radioactive decay in astrophysical context, and how gamma-ray lines reveal details about stellar interiors, about explosions on stellar surfaces or of entire stars, and about the interstellar-medium processes that direct the flow and cooling of nucleosynthesis ashes once having left their sources. We address radioisotopes such as 56 Ni, 44 Ti, 26 Al, 60 Fe, 22 Na, 7 Be, and also how characteristic gamma-ray emission from the annihilation of positrons is connected to these. Basics of Radioactivity DiscoveryIn the nineteenth century, various efforts aimed to bring order into the elements encountered in nature. The inventory of the elements assembled by the Russian

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Section: Astrophysical Studies Using Radioactivitymentioning

confidence: 99%

“…The total mass of 26 Al in the Galaxy is now estimated to be between 1.8 and 2 M [40,41]. The value of the Galactic corecollapse supernova rate therefore was updated with better estimates of the 26 Al mass and of model yields to 1.4±1.1 century −1 [40,41], or one such supernova in our Galaxy every 71 years.…”

Section: Astrophysical Studies Using Radioactivitymentioning

confidence: 99%