X-Ray Absorption in Young Core-collapse Supernova Remnants

Abstract We investigate 60Fe in massive stars and core-collapse supernovae focussing on uncertainties that influence its production in 15, 20, and 25 M$\odot$ stars at solar metallicity. We find that the 60Fe yield is a monotonic increasing function of the uncertain 59Fe(n, γ)60Fe cross-section and that a factor of 10 reduction in the reaction rate results in a factor of 8–10 reduction in the 60Fe yield, while a factor of 10 increase in the rate increases the yield by a factor of 4–7. We find that none of the 189 simulations we have performed are consistent with a core-collapse supernova triggering the formation of the Solar system, and that only models using 59Fe(n, γ)60Fe cross-section that is less than or equal to that from NON-SMOKER can reproduce the observed 60Fe/26Al line flux ratio in the diffuse interstellar medium. We examine the prospects of detecting old core-collapse supernova remnants (SNRs) in the Milky Way from their gamma-ray emission from the decay of 60Fe, finding that the next generation of gamma-ray missions could be able to discover up to ∼100 such old SNRs as well as measure the 60Fe yields of a handful of known Galactic SNRs. We also predict the X-ray spectrum that is produced by atomic transitions in 60Co following its ionization by internal conversion and give theoretical X-ray line fluxes as a function of remnant age as well as the Doppler and fine-structure line broadening effects. The X-ray emission presents an interesting prospect for addressing the missing SNR problem with future X-ray missions.

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Plerion model of the X-ray plateau in short gamma-ray bursts

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1648 ◽

2019 ◽

Vol 487 (4) ◽

pp. 5010-5018 ◽

Cited By ~ 3

Author(s):

L C Strang ◽

A Melatos

Keyword(s):

Light Curve ◽

Supernova Remnants ◽

Gamma Ray ◽

Electron Energy Spectrum ◽

Gamma Ray Bursts ◽

Time Dependent ◽

Core Collapse ◽

X Ray ◽

Surface Magnetic Field ◽

Core Collapse Supernova

Abstract Many short gamma-ray bursts (sGRBs) exhibit a prolonged plateau in the X-ray light curve following the main burst. It is shown that an X-ray plateau at the observed luminosity emerges naturally from a plerion-like model of the sGRB remnant, in which the magnetized, relativistic wind of a millisecond magnetar injects shock-accelerated electrons into a cavity confined by the sGRB blast wave. A geometry-dependent fraction of the plerionic radiation is also intercepted and reprocessed by the optically thick merger ejecta. The relative contributions of the plerion and ejecta to the composite X-ray light curve are estimated approximately with the aid of established ejecta models. The plerionic component of the electron energy spectrum is evolved under the action of time-dependent, power-law injection and adiabatic and synchrotron cooling in order to calculate the X-ray light curve analytically. The model yields an anticorrelation between the luminosity and duration of the plateau as well as a sudden cut-off in the X-ray flux, if the decelerating magnetar collapses to form a black hole. Both features are broadly consistent with the data and can be related to the surface magnetic field of the magnetar and its angular velocity at birth. The analogy with core-collapse supernova remnants is discussed briefly.

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The contribution of young core-collapse supernova remnants to the X-ray emission near quiescent supermassive black holes

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stv2799 ◽

2015 ◽

Vol 456 (3) ◽

pp. 2537-2549 ◽

Cited By ~ 1

Author(s):

A. Rimoldi ◽

E. M. Rossi ◽

E. Costantini ◽

S. Portegies Zwart

Keyword(s):

Black Holes ◽

Supernova Remnants ◽

Supermassive Black Holes ◽

Core Collapse ◽

X Ray ◽

Core Collapse Supernova

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Using X-ray Emission from Core-Collapse Supernova Shocks to Probe Circumstellar Environments

10.1063/1.3682942 ◽

2007 ◽

Author(s):

Mike Koss ◽

Stefan Immler ◽

Kurt Weiler

Keyword(s):

Core Collapse ◽

X Ray ◽

Core Collapse Supernova ◽

Circumstellar Environments

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Observing the Nucleosynthesis from Core Collapse Supernovae

International Astronomical Union Colloquium ◽

10.1017/s0252921100094136 ◽

1988 ◽

Vol 108 ◽

pp. 383-393

Author(s):

Claes Fransson

Keyword(s):

Supernova Remnants ◽

Direct Evidence ◽

Optical Observations ◽

Core Collapse ◽

Valuable Insight ◽

Sources Of Information ◽

X Ray ◽

Stellar Nucleosynthesis ◽

Plasma Effects ◽

Indirect Sources

Since the appearance of the classical papers on stellar nucleosynthesis in the 1950’s most of the observational tests have been through indirect sources of information. Even though this has been rather successful (cf. various contributions in this volume), it represents only an average over all sources, yielding little information about specific stars. The most direct evidence comes from observations of young galactic supernova remnants (age less than ∼103 years). Unfortunately, the analysis of X-ray data are hampered by a lack of understanding of the detailed physics, eg. non-equilibrium and plasma effects, as well as by observational problems (Itoh and Nomoto, 1987). Optical observations (cf. Raymond, 1984) have given some valuable insight of eg. the oxygen-rich remnants. The analysis of these are, however, suffering from the fact that only a small fraction of the mass is seen in the optical.

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