scholarly journals N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

1983 ◽  
Vol 101 ◽  
pp. 573-577
Author(s):  
G. Pizzichini ◽  
T. L. Cline ◽  
U. D. Desai ◽  
B. J. Teegarden ◽  
W. D. Evans ◽  
...  
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Large Magellanic Cloud ◽  
X Rays ◽  
Radio Image ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Preliminary Results ◽  
Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

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.

scholarly journals X-Ray Astronomy Satellite Ginga

1990 ◽  
Vol 123 ◽  
pp. 41-48
Author(s):  
F. Makino
Keyword(s):  
Gamma Ray ◽  
Effective Area ◽  
X Rays ◽  
Scientific Instruments ◽  
Large Area ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Proportional Counters ◽  
Main Instrument

AbstractThe X-ray astronomy satellite Ginga carries three scientific instruments, the Large Area proportional Counters (LAC), All Sky X-ray Monitor (ASM) and Gamma-ray Burst Detector (GBD). The LAC is the main instrument with an effective area of 4000 cm2 giving it the highest sensitivity to hard X-rays so far achieved. Ginga observed about 250 targets up to the end of 1989.

scholarly journals Radio imaging of the supernova remnant N132D in the Large Magellanic Cloud

1991 ◽  
Vol 148 ◽  
pp. 349-350
Author(s):  
John R. Dickel ◽  
D. K. Milne
Keyword(s):  
High Resolution ◽  
Shell Structure ◽  
Supernova Remnant ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Radio Image ◽  
Radio Imaging

The first high resolution radio image of the supernova remnant N132D shows a complex shell structure.

scholarly journals Australia Telescope observations of the supernova remnant N49 in the LMC

1991 ◽  
Vol 148 ◽  
pp. 347-348
Author(s):  
Norbert Junkes
Keyword(s):  
High Resolution ◽  
Shell Structure ◽  
Supernova Remnant ◽  
Radio Image ◽  
Southeastern Part ◽  
X Ray ◽  
Northern Edge

We present the first high-resolution radio image of the supernova remnant N49 near the northern edge of the LMC. These observations with the Australia Telescope at 6cm wavelength (4 arcsec resolution) show a distinct radio shell. The shell structure of N49 is similar in radio and X-ray emission, with the maximum of the emission found in the southeastern part of the SNR.

scholarly journals AN X-RAY STUDY OF SUPERNOVA REMNANT N49 AND SOFT GAMMA-RAY REPEATER 0526-66 IN THE LARGE MAGELLANIC CLOUD

2012 ◽  
Vol 748 (2) ◽  
pp. 117 ◽  
Author(s):  
Sangwook Park ◽  
John P. Hughes ◽  
Patrick O. Slane ◽  
David N. Burrows ◽  
Jae-Joon Lee ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Gamma Ray ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
X Ray

N49: The Site of a Gamma-Ray Burst. Preliminary Results from X-Ray Observations.

1983 ◽  
pp. 573-577
Author(s):  
G. Pizzichini ◽  
T. L. Cline ◽  
U. D. Desai ◽  
B. J. Teegarden ◽  
W. D. Evans ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Preliminary Results

scholarly journals Einstein X-ray Observations of Planetary Nebulae and their Implications

1989 ◽  
Vol 131 ◽  
pp. 304-304
Author(s):  
S. P. Tarafdar ◽  
K.M. V. Apparao
Keyword(s):  
High Resolution ◽  
Point Source ◽  
Planetary Nebulae ◽  
Central Star ◽  
Heavy Elements ◽  
X Rays ◽  
X Ray ◽  
Einstein Observatory ◽  
Central Stars

Central stars of nineteen planetary nebulae were observed for X-ray emission using the Einstein Observatory and four of them were detected. High resolution observations with the Einstein Observatory indicates that the X-ray source in NGC 246 is a point source. These planetary nebulae with positive observations turn out to be the nearest, have the least extinction and also have the largest size of the nebulae around them. It is possible that X-ray emission is observed from these planetary nebulae with larger ages because of the smaller extinction by the nebulae and also due to the settling of heavy elements in the central star which otherwise prevents escape of X-rays by providing opacity.

Studies of gamma-ray transitions in 146Eu

1976 ◽  
Vol 54 (2) ◽  
pp. 197-204 ◽  
Author(s):  
P. Sen ◽  
M. Kingman ◽  
H. Bakhru ◽  
N. Cue
Keyword(s):  
High Resolution ◽  
Level Scheme ◽  
Gamma Ray ◽  
X Rays ◽  
Accurate Evaluation ◽  
X Ray ◽  
Correlation Studies ◽  
Γ Rays ◽  
Γ Ray

The decay of 146Gd to levels of 146Eu has been studied using high resolution X-ray and γ-ray detectors. γ–γ directional correlation studies, using X and γ-ray Ge(Li) detectors, were made to assign the spins of the low lying states in 146Eu. γ–γ coincidence experiments with two Ge(Li) detectors and between Eu X rays and γ rays were performed to pin down the levels of 146Eu. On the basis of these measurements, Jπ of 4−, 3−, 2−, and 1− have been assigned respectively to the ground, 115.66, 230.51, and 385.11 keV states in 146Eu. More accurate evaluation of the E2 admixtures in the M1 transitions, 114.85, 115.66, and 154.60 keV, have been obtained. Based on the above results a tentative level scheme for 146Eu has been proposed.

High-resolution X-ray observations of the Cassiopeia A supernova remnant with the Einstein Observatory

1979 ◽  
Vol 234 ◽  
pp. L69 ◽  
Author(s):  
S. S. Murray ◽  
G. Fabbiano ◽  
A. Epstein ◽  
R. Giacconi ◽  
A. C. Fabian
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
X Ray ◽  
Cassiopeia A ◽  
Einstein Observatory

scholarly journals Luminous Supersoft X-ray Sources

1996 ◽  
Vol 165 ◽  
pp. 415-424
Author(s):  
S. Rappaport ◽  
R. Di Stefano
Keyword(s):  
Accretion Disks ◽  
Large Magellanic Cloud ◽  
High Energy ◽  
Magellanic Cloud ◽  
Emission Lines ◽  
Time Variability ◽  
X Rays ◽  
X Ray ◽  
Significant Time ◽  
Einstein Observatory

Supersoft X-ray sources exhibit spectra that are remarkably steep, in that the ratio of low-to-high energy X rays is much larger than is characteristic of the spectra associated with the previously known classes of luminous X-ray sources. The first supersoft sources were discovered during a survey of the Large Magellanic Cloud with the EINSTEIN Observatory (Longet al.1981). The all-sky X-ray survey carried out with ROSAT has now established that luminous supersoft X-ray sources constitute a distinct astronomical class (see, e.g., Hasinger 1994). A number of the identified optical counterparts of the supersoft X-ray sources exhibit blue continua with emission lines of H and He II (Smaleet al.1988; Pakullet al.1988; Cowleyet al.1990), which are characteristic of accretion disks. The X-ray emission of some sources is steady, while others exhibit significant time variability. Table 1 briefly summarizes what is known thus far about the numbers and characteristics of supersoft X-ray sources (see Hasinger 1994, and references therein).

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