scholarly journals The Peculiar X-ray Morphology of the SNR G292.0+1.8 : Evidence for an Asymmetric Supernova Explosion

1983 ◽  
Vol 101 ◽  
pp. 153-158
Author(s):  
D. H. Clark ◽  
I. R. Tuohy
Keyword(s):  
Surface Brightness ◽  
Supernova Remnant ◽  
Supernova Explosion ◽  
Morphological Properties ◽  
Type Ii ◽  
X Ray ◽  
Young Supernova Remnant ◽  
Rich Material ◽  
Einstein Observatory ◽  
Shell Characteristic

A high resolution X-ray image from the Einstein Observatory of the young supernova remnant G292.0+1.8 (MSH11–54), previously noted as peculiar in terms of its spectral and morphological properties at optical and radio wavelengths, also shows an unusual X-ray morphology. Instead of a limb-brightened X-ray shell characteristic of most SNRs, the remnant consists of a central bar-like feature superposed on an ellipsoidal disc of approximately uniform surface brightness. We attribute the bar emission to a ring of oxygen-rich material ejected in the equatorial plane of a massive rotating progenitor, and the uniform disc component to emission from material with roughly cosmic composition heated by the accompanying blast wave. This interpretation provides observational support for the rotating precursor model of a Type II supernova discussed by Bodenheimer and Woosley.

X-Ray, Optical and UV Observations of the Young Supernova Remnant in the Irregular Galaxy NGC 4449

1983 ◽  
pp. 579-582
Author(s):  
W. P. Blair ◽  
R. P. Kirshner ◽  
P. F. Winkler ◽  
J. C. Raymond ◽  
R. A. Fesen ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Irregular Galaxy ◽  
X Ray ◽  
Young Supernova Remnant

scholarly journals The X-ray Structure of the Supernova Remnant G78.2+2.1

1983 ◽  
Vol 101 ◽  
pp. 281-286
Author(s):  
L. A. Higgs ◽  
T. L. Landecker ◽  
F. D. Seward
Keyword(s):  
Supernova Remnant ◽  
The South ◽  
X Ray ◽  
South Eastern ◽  
Einstein Observatory

The south-eastern portion of the supernova remnant G78.2+2.1, in Cygnus, has been detected as a weak X-ray source by the Einstein Observatory. The X-ray structure is similar to that of the radio filaments in this region, and confirms that X-ray emission in this portion of the “Cygnus super-bubble” does originate in a known supernova remnant. Marginally significant variations in X-ray hardness across the mapped area have been detected and can be related to known radio and optical features of the remnant. In its X-ray properties, G78.2+2.1 resembles IC443.

scholarly journals Non-Equilibrium Ionization in Puppis A

1983 ◽  
Vol 101 ◽  
pp. 245-252
Author(s):  
P. F. Winkler ◽  
C. R. Canizares ◽  
B. C. Bromley
Keyword(s):  
High Resolution ◽  
Spectroscopic Data ◽  
Supernova Remnant ◽  
Optical Data ◽  
Equilibrium Conditions ◽  
X Ray ◽  
Flux Measurements ◽  
Far From Equilibrium ◽  
Einstein Observatory ◽  
Non Equilibrium

High resolution X-ray spectroscopy of the brightest knot of emission in the Puppis A supernova remnant shows that it is made up of ionizing plasma, far from equilibrium. Flux measurements in several X-ray lines enable us to determine the non-equilibrium conditions: electron temperature, ion populations, and time since the knot was heated by the supernova shock. Imaging and spectroscopic data from the Einstein Observatory together suggest that this knot is a cloud of density about 10 cm−3 which has recently been shocked to a temperature 7 × 106 K. Radio and optical data on the region appear consistent with this picture.

The X-ray surface brightness of Kepler's supernova remnant

1983 ◽  
Vol 264 ◽  
pp. 196 ◽  
Author(s):  
R. L. White ◽  
K. S. Long
Keyword(s):  
Surface Brightness ◽  
Supernova Remnant ◽  
X Ray

scholarly journals The Mass and Structure of the Remnant of Tycho's Supernova

1983 ◽  
Vol 101 ◽  
pp. 1-15 ◽  
Author(s):  
Paul Gorenstein ◽  
Frederick Seward ◽  
Wallace Tucker
Keyword(s):  
Total Mass ◽  
Column Density ◽  
Supernova Remnant ◽  
Average Density ◽  
Equilibrium Calculation ◽  
Free Expansion ◽  
X Ray ◽  
Upper Limit ◽  
Interstellar Material ◽  
Einstein Observatory

A high resolution X-ray image of Tycho's supernova remnant obtained from the Einstein Observatory reveals three components of X-ray emission that we identify with shocked interstellar material, diffuse ejecta, and clumpy ejecta. This picture is applied to derive the mass of X-ray emitting material. Assuming a distance of 3 kpc, an absorbing column density of 3 × 1021 atoms/cm2, and using an ion-electron non-equilibrium calculation for the emissivity, we find the average density of the ISM is 0.4 atoms/cm3, and the energy contained in the remnant is 1.4 × 1051 ergs. The total mass of X-ray emitting material in the remnant is ≈4 M⊙, ≈2 M⊙ ejecta and ≈2 M⊙ swept up, putting the remnant at an intermediate state between a free expansion and the Sedov phase. There is no evidence for neutron star. The upper limit on the surface temperature is in the range 1.1 to 1.8 × 106K.

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 Two Types of Pulsars

1987 ◽  
Vol 125 ◽  
pp. 425-437
Author(s):  
J.H. Huang
Keyword(s):  
Neutron Stars ◽  
Supernova Explosion ◽  
Type I ◽  
Type Ii ◽  
Emission Mechanism ◽  
X Ray ◽  
Origin And Evolution ◽  
Binary Pulsars ◽  
Self Consistent ◽  
Evolutionary Mode

To sort out the whole sample of pulsars with measured P and P into two types has much something to do with the origin and evolution of neutron stars. Under the configuration of two types of pulsars with different spindown mechanism, we have discussed a variety of their properties, including their radio emission mechanism, space velocities, interior structures and evolutionary modes. The fact that different type of pulsars does have quite different properties indicates that the processes to create neutron stars may have two distinct types, say, Type II supernova explosion and the collapse of accreting white dwarfs. The evolutionary mode for our Type I pulsars provides such a key link between binary pulsars and X-ray binary pulsars that we may propose a self-consistent scenario for binary pulsars, X-ray binary pulsars, fast pulsars as well as Type I pulsars.

scholarly journals Differential Imaging of [Fe X] in IC 443

1988 ◽  
Vol 101 ◽  
pp. 407-410
Author(s):  
Larry Brown ◽  
Bruce E. Woodgate ◽  
Robert Petre
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Temperature Region ◽  
Supernova Remnant ◽  
Coronal Line ◽  
X Ray ◽  
Imaging Camera ◽  
Differential Imaging ◽  
Einstein Observatory ◽  
Gas Pressures

AbstractThis paper presents images of two areas of the supernova remnant IC443 showing emission from the [Fe X] 6374Å red coronal line taken with an emission line differential imaging camera. The areas are in the vicinity of strong soft X-ray emission as observed with the Einstein Observatory. The [Fe X] emission is patchy on the scale of seconds of arc. For the highest emission regions we find an electron density of approximately 100 cm−3 and gas pressures of 108cm−3K. No correlation is found between the X-ray and [Fe X] knots, and the results support a clumpy, multi-temperature region where the [Fe X] knots are balanced between collapse and evaporation.

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