scholarly journals Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

2019 ◽  
Vol 872 (1) ◽  
pp. 31 ◽  
Author(s):  
Jayant Bhalerao ◽  
Sangwook Park ◽  
Andrew Schenck ◽  
Seth Post ◽  
John P. Hughes
Keyword(s):  
Supernova Remnant ◽  
Core Collapse ◽  
X Ray ◽  
Core Collapse Supernova ◽  
Circumstellar Medium

scholarly journals X-RAY EJECTA KINEMATICS OF THE GALACTIC CORE-COLLAPSE SUPERNOVA REMNANT G292.0+1.8

2015 ◽  
Vol 800 (1) ◽  
pp. 65 ◽  
Author(s):  
Jayant Bhalerao ◽  
Sangwook Park ◽  
Daniel Dewey ◽  
John P. Hughes ◽  
Koji Mori ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Core Collapse ◽  
X Ray ◽  
Core Collapse Supernova

THE PUZZLING JET AND PULSAR WIND NEBULA OF IGR J11014-6103

2014 ◽  
Vol 28 ◽  
pp. 1460172 ◽  
Author(s):  
LUCIA PAVAN ◽  
POL BORDAS ◽  
GERD PÜHLHOFER ◽  
MIROSLAV D. FILIPOVIC ◽  
AIN DE HORTA ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Helical Structure ◽  
Core Collapse ◽  
Radio Observations ◽  
X Ray ◽  
Core Collapse Supernova ◽  
The Core ◽  
Pulsar Wind

IGR J11014-6103 is a hard X-ray source discovered by INTEGRAL. Follow-up X-ray and radio observations revealed an elongated pulsar wind nebula formed by a neutron star escaping supersonically its parent supernova remnant SNR MSH 11-61A. The pulsar also emits highly collimated jets extending perpendicularly to the direction of motion. The jet has a continuous helical structure extending up to more than 10 parsecs. IGR J11014-6103 is a laboratory to study jet ejection in the wind of a pulsar and to constrain the core collapse supernova mechanism responsible for the observed pulsar kick velocity in excess of 1000 km/s.

scholarly journals 60Fe in core-collapse supernovae and prospects for X-ray and gamma-ray detection in supernova remnants

2019 ◽  
Vol 485 (3) ◽  
pp. 4287-4310 ◽  
Author(s):  
Samuel W Jones ◽  
Heiko Möller ◽  
Chris L Fryer ◽  
Christopher J Fontes ◽  
Reto Trappitsch ◽  
...  
Keyword(s):  
Cross Section ◽  
Supernova Remnants ◽  
Gamma Ray ◽  
Flux Ratio ◽  
Core Collapse ◽  
Line Broadening ◽  
X Ray ◽  
Core Collapse Supernova ◽  
Structure Line ◽  
Solar Metallicity

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.

scholarly journals X-Ray Absorption in Young Core-collapse Supernova Remnants

2018 ◽  
Vol 864 (2) ◽  
pp. 175 ◽  
Author(s):  
Dennis Alp ◽  
Josefin Larsson ◽  
Claes Fransson ◽  
Michael Gabler ◽  
Annop Wongwathanarat ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Core Collapse ◽  
X Ray ◽  
Core Collapse Supernova ◽  
X Ray Absorption

scholarly journals DENSE IRON EJECTA AND CORE-COLLAPSE SUPERNOVA EXPLOSION IN THE YOUNG SUPERNOVA REMNANT G11.2-0.3

2009 ◽  
Vol 703 (1) ◽  
pp. L81-L85 ◽  
Author(s):  
Dae-Sik Moon ◽  
Bon-Chul Koo ◽  
Ho-Gyu Lee ◽  
Keith Matthews ◽  
Jae-Joon Lee ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Supernova Explosion ◽  
Core Collapse ◽  
Core Collapse Supernova ◽  
Young Supernova Remnant

scholarly journals A THREE-STAGE MODEL FOR THE INNER ENGINE OF GRBs: PROMPT EMISSION AND EARLY AFTERGLOW

2008 ◽  
Vol 17 (09) ◽  
pp. 1383-1389 ◽  
Author(s):  
J. STAFF ◽  
B. NIEBERGAL ◽  
R. OUYED
Keyword(s):  
Black Hole ◽  
Gamma Ray ◽  
Surrounding Medium ◽  
Core Collapse ◽  
Stage Model ◽  
Quark Star ◽  
X Ray ◽  
Core Collapse Supernova ◽  
Stage 1 ◽  
Prompt Emission

We describe a model within the "quark-nova" scenario to interpret the recent observations of early X-ray afterglows of long gamma-ray bursts (GRBs) with the Swift satellite. This is a three-stage model within the context of a core-collapse supernova. STAGE 1 is an accreting (proto-) neutron star leading to a possible delay between the core collapse and the GRB. STAGE 2 is accretion onto a quark star, launching an ultrarelativistic jet generating the prompt GRB. This jet also creates the afterglow as the jet interacts with the surrounding medium creating an external shock. Slower shells ejected from the quark star (during accretion), can re-energize the external shock leading to a flatter segment in the X-ray afterglow. STAGE 3, which occurs only if the quark star collapses to form a black hole, consists of an accreting black hole. The jet launched in this accretion process interacts with the preceding quark star jet, and could generate the flaring activity frequently seen in early X-ray afterglows. Alternatively, a STAGE 2b can occur in our model if the quark star does not collapse to a black hole. The quark star in this case can then spin down due to magnetic braking, and the spin down energy may lead to flattening in the X-ray afterglow as well. This model seems to account for both the energies and the timescales of GRBs, in addition to the newly discovered early X-ray afterglow features.

scholarly journals Impact of sterile neutrino dark matter on core-collapse supernovae

2016 ◽  
Vol 31 (25) ◽  
pp. 1650137 ◽  
Author(s):  
Mackenzie L. Warren ◽  
Grant J. Mathews ◽  
Matthew Meixner ◽  
Jun Hidaka ◽  
Toshitaka Kajino
Keyword(s):  
Dark Matter ◽  
Sterile Neutrino ◽  
Core Collapse ◽  
Observable Effect ◽  
Sterile Neutrinos ◽  
X Ray ◽  
Core Collapse Supernova ◽  
Electron Neutrinos ◽  
Supernova Explosions ◽  
The Impact

We summarize the impact of sterile neutrino dark matter on core-collapse supernova explosions. We explore various oscillations between electron neutrinos or mixed [Formula: see text] neutrinos and right-handed sterile neutrinos that may occur within a core-collapse supernova. In particular, we consider sterile neutrino masses and mixing angles that are consistent with sterile neutrino dark matter candidates as indicated by recent X-ray flux measurements. We find that the interpretation of the observed 3.5 keV X-ray excess as due to a decaying 7 keV sterile neutrino that comprises 100% of the dark matter would have almost no observable effect on supernova explosions. However, in the more realistic case in which the decaying sterile neutrino comprises only a small fraction of the total dark matter density due to the presence of other sterile neutrino flavors, WIMPs, etc. a larger mixing angle is allowed. In this case a 7 keV sterile neutrino could have a significant impact on core-collapse supernovae. We also consider mixing between [Formula: see text] neutrinos and sterile neutrinos. We find, however, that this mixing does not significantly alter the explosion and has no observable effect on the neutrino luminosities at early times.

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