Gamma-ray line measurements from supernova explosions

Abstract

Abstract. Gamma ray lines are expected to be emitted as part of the afterglow of supernova explosions, because radioactive decay of freshly synthesised nuclei occurs. Significant radioactive gamma ray line emission is expected from 56 Ni and 44 Ti decay on time scales of the initial explosion ( 56 Ni, τ ∼days) and the young supernova remnant ( 44 Ti,τ ∼90 years ). Less specific, and rather informative for the supernova population as a whole, are lessons from longer lived isotopes such as 26 Al and 60 Fe. From isotopes of elements heavier than iron group elements, any interesting gamma-ray line emission is too faint to be observable. Measurements with space-based gamma-ray telescopes have obtained interesting gamma ray line emissions from two core collapse events, Cas A and SN1987A, and one thermonuclear event, SN2014J. We discuss INTEGRAL data from all above isotopes, including all line and continuum signatures from these two objects, and the surveys for more supernovae, that have been performed by gamma ray spectrometry. Our objective here is to illustrate what can be learned from gamma-ray line emission properties about the explosions and their astrophysics.

Supernova explosions of massive stars and cosmic rays

“…Using the 26 Al line at 1809 keV we can estimate the piston mass: The observed lines have a half width of about 300 km/s (Diehl 2017; full width 593 km/s). In our picture we interpret this number as momentum conservation of the ejecta, so that Assuming then the same piston mass for the conditions for a RSG star wind, with a density about 100 times higher, implies that equality is reached far below 3 pc:…”

The Origin of the Most Energetic Galactic Cosmic Rays: Supernova Explosions into Massive Star Plasma Winds

“…Some recent relevant reviews and books are Aharonian (2004) [23], Stanev (2010) [24], Kotera and Olinto (2011) [25], Letessier-Selvon and Stanev (2011) [26], Bykov et al (2012) [27], Diehl (2013Diehl ( , 2017 [28,29], Blasi (2013) [30], Gaisser et al (2016) [31], Kronberg (2016) [32], Amato and Blasi (2018) [33], Biermann et al (2018), cited as ASR18 [34], Aartsen et al (2018c) [35], these latter articles all part of a collection of reviews on CR physics, edited by Moskalenko and Seo 2018 [36]. Many further tests can now be done with newer results from the Pierre Auger Observatory, the Telescope Array, IceCube, AMS, HAWC, H.E.S.S., MAGIC, PAMELA, Fermi-LAT, CALET, DAMPE, and VERITAS, further balloon flights, such as TIGER, and other experiments in space, on balloons, and on the ground.…”

The Origin of the Most Energetic Galactic Cosmic Rays: Supernova Explosions into Massive Star Plasma Winds

“…Some recent relevant reviews and books are Aharonian (2004) [19], Stanev (2010) [133], Kotera & Olinto (2011) [87], Letessier-Selvon & Stanev (2011) [99], Bykov et al (2012) [49], Diehl (2013Diehl ( , 2017 [60,61], Blasi (2013) [47], Gaisser et al (2016) [68], Kronberg (2016) [94], Amato & Blasi (2017) [27], and Biermann et al (2018) [43], referred to as ASR18. Many further tests can now be done with new results from Auger, the Telescope Array, IceCube, AMS, HAWC, HESS, MAGIC, CALET, DAMPE, and Veritas, further balloon flights, such as TIGER, and other experiments in space, on balloons, and on the ground.…”