Simulations show magnetar giant flares produce nuclei near r-process peaks whose decays create bright MeV gamma-ray lines from 88Kr and 92Sr with fluxes above 10^-8 erg cm^-2 s^-1.
An exceptionally bright flare from SGR1806-20 and the origins of short-duration gamma-ray bursts
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abstract
Soft-gamma-ray repeaters (SGRs) are galactic X-ray stars that emit numerous short-duration (about 0.1 s) bursts of hard X-rays during sporadic active periods. They are thought to be magnetars: strongly magnetized neutron stars with emissions powered by the dissipation of magnetic energy. Here we report the detection of a long (380 s) giant flare from SGR 1806-20, which was much more luminous than any previous transient event observed in our Galaxy. (In the first 0.2 s, the flare released as much energy as the Sun radiates in a quarter of a million years.) Its power can be explained by a catastrophic instability involving global crust failure and magnetic reconnection on a magnetar, with possible large-scale untwisting of magnetic field lines outside the star. From a great distance this event would appear to be a short-duration, hard-spectrum cosmic gamma-ray burst. At least a significant fraction of the mysterious short-duration gamma-ray bursts therefore may come from extragalactic magnetars.
fields
astro-ph.HE 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
Magnetic inclination alignment with timescale proportional to B to the minus two suppresses observed numbers of strong-field neutron stars, unifying pulsars and magnetars under one log-uniform initial B distribution.
citing papers explorer
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MeV Gamma-Ray Lines from Radioactive Nuclei in Magnetar Giant Flares
Simulations show magnetar giant flares produce nuclei near r-process peaks whose decays create bright MeV gamma-ray lines from 88Kr and 92Sr with fluxes above 10^-8 erg cm^-2 s^-1.
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A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment
Magnetic inclination alignment with timescale proportional to B to the minus two suppresses observed numbers of strong-field neutron stars, unifying pulsars and magnetars under one log-uniform initial B distribution.