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 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

scholarly journals Radio study of the extended TeV source VER J1907+062

2019 ◽  
Vol 491 (4) ◽  
pp. 5732-5739
Author(s):  
L Duvidovich ◽  
A Petriella ◽  
E Giacani
Keyword(s):  
Atomic Hydrogen ◽  
Molecular Clouds ◽  
Supernova Remnant ◽  
Molecular Gas ◽  
Radio Observations ◽  
Very Large Array ◽  
X Ray ◽  
New Radio ◽  
Γ Ray ◽  
Pulsar Wind

ABSTRACT This paper aims to provide new insights on the origin of the TeV source VER J1907+062 through new high-quality radio observations. We used the Karl G. Jansky Very Large Array (VLA) to observe the whole extension of VER J1907+062 at 1.5 GHz with a mosaicking technique and the PSR J1907+0602 in a single pointing at 6 GHz. These data were used together with 12CO and atomic hydrogen observations obtained from public surveys to investigate the interstellar medium in the direction of VER J1907+062. The new radio observations do not show any evidence of a pulsar wind nebula (PWN) driven by the pulsars present in the field and no radio counterpart to the proposed X-ray PWN powered by PSR J1907+0602 is seen in the new VLA image at 6 GHz down to a noise level of 10 $\mu$Jy beam−1. Molecular clouds were discovered over the eastern, southern, and western borders of the radio shell of G40.5−0.5, suggesting an association with this supernova remnant. We explored several scenarios for the origin of VER J1907+062. We propose as the most probable scenario one in which the TeV emission is produced by two separated γ-ray sources located at different distances: one of leptonic origin and associated with a PWN powered by PSR J1907+0602 at ∼3.2 kpc and another of hadronic origin and produced by the interaction between G40.5−0.5 and the surrounding molecular gas at ∼8.7 kpc.

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 The bubble-like interior of the core-collapse supernova remnant Cassiopeia A

Science ◽  
2015 ◽  
Vol 347 (6221) ◽  
pp. 526-530 ◽  
Author(s):  
D. Milisavljevic ◽  
R. A. Fesen
Keyword(s):  
Supernova Remnant ◽  
Core Collapse ◽  
Cassiopeia A ◽  
Core Collapse Supernova ◽  
The Core

scholarly journals Discovery of a jet-like structure with overionized plasma in the SNR IC 443

2018 ◽  
Vol 615 ◽  
pp. A157 ◽  
Author(s):  
Emanuele Greco ◽  
Marco Miceli ◽  
Salvatore Orlando ◽  
Giovanni Peres ◽  
Eleonora Troja ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Supernova Explosion ◽  
Original Position ◽  
Core Collapse ◽  
Complex Environment ◽  
Energy Bands ◽  
X Ray ◽  
Spatially Resolved ◽  
Pulsar Wind ◽  
The Relationship

Context. IC 443 is a supernova remnant (SNR) located in a quite complex environment since it interacts with nearby clouds. Indications for the presence of overionized plasma have been found though the possible physical causes of overionization are still debated. Moreover, because of its peculiar position and proper motion, it is not clear if the pulsar wind nebula (PWN) within the remnant is the relic of the IC 443 progenitor star or just a rambling one seen in projection on the remnant. Aims. Here we address the study of IC 443 plasma in order to clarify the relationship PWN-remnant, the presence of overionization and the origin of the latter. Methods. We analyzed two XMM-Newton observations producing background-subtracted, vignetting-corrected and mosaicked images in two different energy bands and we performed a spatially resolved spectral analysis of the X-ray emission. Results. We identified an elongated (jet-like) structure with Mg-rich plasma in overionization. The head of the jet is interacting with a molecular cloud and the jet is aligned with the position of the PWN at the instant of the supernova explosion. Interestingly, the direction of the jet of ejecta is somehow consistent with the direction of the PWN jet. Conclusions. Our discovery of a jet of ejecta in IC 443 enlarge the sample of core-collapse SNRs with collimated ejecta structures. IC 443’s jet is the first one which shows overionized plasma, possibly associated with the adiabatic expansion of ejecta. The match between the jet’s direction and the original position of the PWN strongly supports the association between the neutron star and IC 443.

scholarly journals A shallow water analogue of asymmetric core-collapse, and neutron star kick/spin

2011 ◽  
Vol 7 (S279) ◽  
pp. 134-137
Author(s):  
Thierry Foglizzo ◽  
Frédéric Masset ◽  
Jérôme Guilet ◽  
Gilles Durand
Keyword(s):  
Neutron Star ◽  
Shallow Water ◽  
Acoustic Waves ◽  
Large Scale ◽  
Massive Stars ◽  
Core Collapse ◽  
Hydraulic Jumps ◽  
Core Collapse Supernova ◽  
Accretion Shock

AbstractMassive stars end their life with the gravitational collapse of their core and the formation of a neutron star. Their explosion as a supernova depends on the revival of a spherical accretion shock, located in the inner 200km and stalled during a few hundred milliseconds. Numerical simulations suggest that the large scale asymmetry of the neutrino-driven explosion is induced by a hydrodynamical instability named SASI. Its non radial character is able to influence the kick and the spin of the resulting neutron star. The SWASI experiment is a simple shallow water analog of SASI, where the role of acoustic waves and shocks is played by surface waves and hydraulic jumps. Distances in the experiment are scaled down by a factor one million, and time is slower by a factor one hundred. This experiment is designed to illustrate the asymmetric nature of core-collapse supernova.

Supernova Remnant Searches at Molonglo

1984 ◽  
Vol 5 (4) ◽  
pp. 537-540 ◽  
Author(s):  
A. J. Turtle ◽  
B. Y. Mills
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Magellanic Clouds ◽  
Radio Observations ◽  
X Ray

A catalogue of 38 supernova remnants (SNRs) identified in the Large and Small Magellanic Clouds from X-ray, optical and radio observations has recently been presented by Mills et al. (1984). One important consideration is the completeness of this catalogue and of the Galactic catalogues with which it is compared. These are currently being investigated.

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.

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