scholarly journals A Key to Pulsar Wind Bubble Morphologies: Hydrodynamical Simulations

2004 ◽  
Vol 218 ◽  
pp. 175-178
Author(s):  
Eric van der Swaluw ◽  
Turlough P. Downes
Keyword(s):  
High Velocity ◽  
Supernova Remnant ◽  
Bow Shock ◽  
Shock Interaction ◽  
Reverse Shock ◽  
Supersonic Expansion ◽  
Expansion Stage ◽  
Pulsar Wind ◽  
Hydrodynamical Simulations

We present a model of a pulsar-driven supernova remnant, by using a hydrodynamics code, which simulates the evolution of a pulsar wind nebula when the pulsar is moving at a high velocity through its expanding supernova remnant. The simulation shows four different stages of the pulsar wind nebula: the supersonic expansion stage, the reverse shock interaction stage, the subsonic expansion stage and ultimately the bow shock stage. Due to the high velocity of the pulsar, the position of the pulsar is located at the head of the pulsar wind bubble, after the passage of the reverse shock. The resulting morphology of the pulsar wind bubble is therefore similar to the morphology of a bow shock pulsar wind nebulA. We show how to distinguish these two different stages, and apply this method to the SNR G327.1–1.1, for which we argue that there is no bow shock around its pulsar wind nebulA.

scholarly journals Deciphering the nature of the pulsar wind nebula CTB 87 with XMM–Newton

2019 ◽  
Vol 491 (2) ◽  
pp. 3013-3021 ◽  
Author(s):  
B Guest ◽  
S Safi-Harb ◽  
A MacMaster ◽  
R Kothes ◽  
B Olmi ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Thermal Emission ◽  
Plasma Temperature ◽  
Evolutionary Stage ◽  
Reverse Shock ◽  
X Ray ◽  
Upper Limit ◽  
Supernova Shell ◽  
Pulsar Wind ◽  
Hydrodynamical Simulations

ABSTRACT CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM–Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm−3 for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations.

scholarly journals Hubble Space TelescopeObservations of High‐Velocity Lyα and Hα Emission from Supernova Remnant 1987A: The Structure and Development of the Reverse Shock

2003 ◽  
Vol 593 (2) ◽  
pp. 809-830 ◽  
Author(s):  
Eli Michael ◽  
Richard McCray ◽  
Roger Chevalier ◽  
Alexei V. Filippenko ◽  
Peter Lundqvist ◽  
...  
Keyword(s):  
High Velocity ◽  
Supernova Remnant ◽  
Reverse Shock ◽  
Hα Emission ◽  
Supernova Remnant 1987A

scholarly journals Revisiting the evolution of nonradiative supernova remnants: A hydrodynamical-informed parameterization of the shock positions

2021 ◽  
Author(s):  
R Bandiera ◽  
N Bucciantini ◽  
J Martín ◽  
B Olmi ◽  
D F Torres
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Structural Features ◽  
Pulsar Wind Nebulae ◽  
Reverse Shock ◽  
Self Similar ◽  
Pulsar Wind ◽  
The One ◽  
Similar Solutions

Abstract Understanding the evolution of a supernova remnant shell in time is fundamental. Such understanding is critical to build reliable models of the dynamics of the supernova remnant shell interaction with any pulsar wind nebula it might contain. Here, we perform a large study of the parameter space for the one-dimensional spherically symmetric evolution of a supernova remnant, accompanying it by analytical analysis. Assuming, as is usual, an ejecta density profile with a power-law core and an envelope, and a uniform ambient medium, we provide a set of highly-accurate approximations for the evolution of the main structural features of supernova remnants, such as the reverse and forward shocks and the contact discontinuity. We compare our results with previously adopted approximations, showing that existing simplified prescriptions can easily lead to large errors. In particular, in the context of pulsar wind nebulae modelling, an accurate description for the supernova remnant reverse shock is required. We also study in depth the self-similar solutions for the initial phase of evolution, when the reverse shock propagates through the envelope of the ejecta. Since these self-similar solutions are exact, but not fully analytical, we here provide highly-accurate approximations as well.

scholarly journals On the origin of jet-like features in bow shock pulsar wind nebulae

2019 ◽  
Vol 490 (3) ◽  
pp. 3608-3615 ◽  
Author(s):  
B Olmi ◽  
N Bucciantini
Keyword(s):  
Supernova Remnant ◽  
High Energy ◽  
Field Structure ◽  
Bow Shock ◽  
Pulsar Wind Nebulae ◽  
Magnetic Field Structure ◽  
X Ray ◽  
Class A ◽  
Pulsar Wind ◽  
High Energy Particles

ABSTRACT Bow shock pulsar wind nebulae are a large class of non-thermal synchrotron sources associated to old pulsars that have emerged from their parent supernova remnant and are directly interacting with the interstellar medium. Within this class a few objects show extended X-ray features, generally referred as ‘jets’, that defies all the expectations from the canonical MHD models, being strongly misaligned respect to the pulsar direction of motion. It has been suggested that these jets might originate from high energy particles that escape from the system. Here we investigate this possibility, computing particle trajectories on top of a 3D relativistic MHD model of the flow and magnetic field structure, and we show not only that beamed escape is possible, but that it can easily be asymmetric and charge separated, which as we will discuss are important aspects to explain known objects.

scholarly journals Disentangling hadronic from leptonic emission in the composite SNR G326.3-1.8

2017 ◽  
Vol 12 (S331) ◽  
pp. 320-324
Author(s):  
Justine Devin ◽  
Fabio Acero ◽  
Jean Ballet
Keyword(s):  
Spectral Analysis ◽  
Supernova Remnant ◽  
Angular Resolution ◽  
Middle Aged ◽  
Reverse Shock ◽  
Data Release ◽  
Γ Ray ◽  
Pulsar Wind ◽  
Aged Composite

AbstractG326.3-1.8 (also known as MSH 15-56) has been detected in radio as a middle-aged composite supernova remnant (SNR) consisting of a SNR shell and a pulsar wind nebula (PWN) which has been crushed by the reverse shock. With the recent Fermi-LAT data release Pass 8 providing increased acceptance and angular resolution, we investigate the morphology of this SNR to disentangle the PWN from the SNR contributions and understand the nature of the γ-ray emission. We thus perform a morphological and spectral analysis from 300 MeV to 300 GeV which highlights the contributions from these two components. The simplest interpretation is hadronic emission from the SNR and harder leptonic emission from the PWN.

scholarly journals An X-ray Pulsar, Metal-rich Ejecta, and Shocked Ambient Medium in the Supernova Remnant G292.0+1.8

2004 ◽  
Vol 218 ◽  
pp. 199-202
Author(s):  
John P. Hughes ◽  
Robert B. Friedman ◽  
Patrick Slane ◽  
Sangwook Park
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Ambient Medium ◽  
Compact Object ◽  
Optical Counterpart ◽  
Reverse Shock ◽  
X Ray ◽  
Pulsar Wind ◽  
Circumstellar Medium

We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the Galactic supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period is consistent with the extrapolation of the radio period and spindown rate of PSR J1124−5916. The X-ray pulse is single peaked and broad. There is no optical counterpart to a limit of MV ∼ 26. The pressure in the pulsar wind nebula is considerably less than that in the reverse-shock-heated ejecta and circumstellar medium, indicating that the reverse shock has not yet begun to interact with the nebula.

scholarly journals High-velocity gas associated with the supernova remnant S147

1981 ◽  
Vol 195 (3) ◽  
pp. 485-495 ◽  
Author(s):  
A. P. Phillips ◽  
P. M. Gondhalekar ◽  
J. C. Blades
Keyword(s):  
High Velocity ◽  
Supernova Remnant

scholarly journals Interaction of high-velocity pulsars with supernova remnant shells

2003 ◽  
Vol 397 (3) ◽  
pp. 913-920 ◽  
Author(s):  
E. van der Swaluw ◽  
A. Achterberg ◽  
Y. A. Gallant ◽  
T. P. Downes ◽  
R. Keppens
Keyword(s):  
High Velocity ◽  
Supernova Remnant
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