scholarly journals Investigations of Recently Discovered Supernova Remnants’ Spectral Plot: AT2019fya, SN2019fjp, SN2019fcc, SN2019fbv, SN2019ffi, and SN2019fce

2020 ◽  
Vol 84 ◽  
pp. 1-9
Author(s):  
Bjorn Jasper R. Raquel ◽  
Agnes C. Bantaculo ◽  
Shane Carlo B. Llemit ◽  
Eldrin P. Custodio
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Type Ii ◽  
Plot Analysis ◽  
The Individual ◽  
The Crab Nebula

This paper presents the spectroscopic graphs of recently discovered Supernova Remnants (AT2019fya, SN2019fjp, SN2019fcc, SN2019fce, SN2019fbv & SN2019ffi) for the determination of elements present. The researchers use the spectral plot analysis to analyze the presence of certain elements of the individual supernova remnants (SNR) for the assimilation, differentiation and classification of these SNR. Redshift and velocities of these SNR were also found using the observed wavelength and the rest wavelength ratio. Comparison suggests that AT2019fya is a Type II supernova remnant and some of the SNRs in this study exhibits an existence of krypton (Kr) on their composition which is recently discovered by M. Barlow (2013) to be present at the Crab Nebula. This might suggest that AT2019fya, SN2019fbv, SN2019fce, and SN2019ffi have a pulsar at their center.

scholarly journals Supernova Remnants Resembling the Crab Nebula

1983 ◽  
Vol 101 ◽  
pp. 299-320 ◽  
Author(s):  
K. W. Weiler
Keyword(s):  
Large Class ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Origin And Evolution ◽  
Class C ◽  
The Individual ◽  
The Crab Nebula

While reviewing and systematizing the properties of the class of supernova remnants resembling the Crab Nebula it has been found that supernova remnants can be split into three morphological groups – Class S (shells), Class P (plerions), and Class C (combinations) – where the Class C objects appear to represent a new and especially interesting classification. In this overview, the identifying properties of all three classes are defined. Because the large Class S has been studied in detail many times previously, it is not discussed further here. For the smaller Classes P and C, the individual members and suspected members are presented and their properties reviewed. Finally, an origin and evolution for each class is suggested.

Studies of the X-ray emission from supernova remnants

1974 ◽  
Vol 340 (1623) ◽  
pp. 423-437
Keyword(s):  
Supernova Remnants ◽  
Column Density ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Lower Intensity ◽  
X Ray ◽  
Cassiopeia A ◽  
Cygnus Loop ◽  
A Value ◽  
The Crab Nebula

Supernova remnants are now recognized as a class of soft X-ray emitting-objects. The evolution of a remnant’s X-ray emission is discussed and a number of possible X-ray emission mechanisms are described. The spectrum of the Crab Nebula has been studied with Copernicus. The data have been used to derive a value of the gas column density of the interstellar medium. The X-ray structure and spectrum of the remnant Cassiopeia. A have been investigated and the results are presented. A high resolution X-ray map of the Puppis A supernova remnant has been obtained and the interpretation of the X-ray structure is discussed. X-ray emission has been detected from the pulsar PSR 08 33-45. This observation is compared with data obtained from the Uhuru satellite in order to derive the gas column density to the source. Weak soft X-ray emission has been detected from the Cygnus Loop in the regions expected but a t a lower intensity – a search for regions of higher intensity is continuing. A programme to identify known radio remnants as X-ray emitters is in progress and the results obtained so far are reported.

scholarly journals A Newly-Recognised Galactic Supernova Remnant with Shell-Type and Filled-Centre Features

1988 ◽  
Vol 101 ◽  
pp. 347-350
Author(s):  
Peter J. Barnes ◽  
A.J. Turtle
Keyword(s):  
Spectral Index ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Dual Nature ◽  
Valuable Addition ◽  
Shell Type ◽  
The Crab Nebula ◽  
Galactic Object

While the number of galactic supernova remnants (SNRs) now known is fairly large (>150), the subset among these that are known to resemble the Crab Nebula is still distressingly small, about 15 or so (Green, 1984). Thus any object that can be unambiguously included in this exclusive club forms a valuable addition to our knowledge of this class. We report here observations of a newly recognised nonthermal galactic object, G18.94-l.06, having all the hallmarks of the classical shell-type SNRs, while also appearing to have a filled-centre component located inside the shell. Among the known Crab-like remnants, about one third show this dual nature (Green, 1984). This diagnosis of G18.94-1.06 is supported mainly by the variations in spectral index α (Sν∝ να) across the source, as seen between the two observation frequencies, 408 MHz and 5.0 GHz.

scholarly journals The Spectral Turnover of the “Filled-Center” Supernova Remnant 3C 58: Implications for When Acceleration Occurs

1994 ◽  
Vol 142 ◽  
pp. 817-821
Author(s):  
D. A. Green
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Crab Nebula ◽  
Injection Rate ◽  
Power Law Distribution ◽  
Radiation Mechanisms ◽  
Particle Injection ◽  
The Past ◽  
Upper Limits ◽  
The Crab Nebula

AbstractIRASobservations the “filled-center” supernova remnant 3C 58 are used to derived upper limits of 0.4, 0.4, 0.8, and 1.5 Jy for its infrared flux density at 12, 25, 60, and 100 μm, respectively. These values imply a break in the spectrum of 3C58 above a few tens of gigahertz—two orders of magnitude below the break in the spectrum of the Crab Nebula—with a change of spectral index across the break for 3C 58 of more than 0.5. This is similar to previous results for another “filled-center” remnant, G74.9+1.2, from radio observations alone. This implies that their emission isnotdominated by a constant injection rate of particles with a power-law distribution. Either the break is due to synchrotron losses in the past, with little particle injection in recent times or it is intrinsic to the acceleration mechanism at work (presumably from a central neutron star).Subject headings: acceleration of particles — ISM: individual (3C 58) — radiation mechanisms: nonthermal — supernova remnants

Classification of the Oxbow Lakes of the Hármas-Körös River and Determination of Ways for Further Exploiting the Various Water Regions in the Light of the Water Framework Directive

2017 ◽  
Author(s):  
Józsa Vilmos ◽  
Jacek Kozłowski ◽  
Anna Zróbek-Sokolnik ◽  
Krzysztof Kozłowski ◽  
Piotr Dynowski
Keyword(s):  
Fishery Management ◽  
Ecological Status ◽  
Anthropogenic Factors ◽  
Oxbow Lakes ◽  
Negative Effect ◽  
Juvenile Stages ◽  
The Individual ◽  
The City

Hármas-Koros river lies between the mouth of the Tisza and the city Békés. In the nineteenth century, the work of regulatory her bed was made, which resulted in 44 oxbow lakes were created, of which 36 still exist till today. In presented work 14 oxbow lakes was selected and the following objectives were carried out: 1. The classification of oxbow lakes based on selected criteria: the manner and intensity of water exchange, sediment thickness, redox potential, usage, ichtiofouna. 2. The assessment of the state of spawning and its impact on ichtiofauna. 3. Determination the best methods of water management in particular types of oxbow lakes, which could stop their further degradation. The obtained results led to the following conclusions: - Tested oxbow lakes belong to different categories - Anthropogenic factors had a negative effect on the conditions of fish reproduction and survival of their juvenile stages. - The management of fisheries was not a factor differentiating the individual water regions, but had an impact on the ecological status. - For the maintenance and/or improvement of the natural environment of the individual oxbow lakes significant impact may have fishery management, carried out in the following years.

scholarly journals Physical Processes and Parameters in the Magnetosphere of NP 0532

1971 ◽  
Vol 46 ◽  
pp. 394-406
Author(s):  
F. Pacini
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
General Relation ◽  
Energy Generation ◽  
Main Pulse ◽  
Physical Processes ◽  
X Ray ◽  
The Crab Nebula

The Crab Nebula pulsar conforms to the model of a rotating magnetised neutron star in the rate of energy generation and the exponent of the rotation law.It is suggested that the main pulse is due to electrons and the precursor to protons. Both must radiate in coherent bunches. Optical and X-ray radiation is by the synchrotron process.The wisps observed in the Nebula may represent the release of an instability storing about 1043 erg and 1047–48 particles.Finally, some considerations are made about the general relation between supernova remnants and rotating neutron stars.

scholarly journals The Galactic Sources G5.4-1.2 and G5.27-0.90

1987 ◽  
Vol 125 ◽  
pp. 129-129
Author(s):  
J.L. Caswell ◽  
M.J. Kesteven ◽  
R.F. Haynes ◽  
D.K. Milne ◽  
M.M. Komesaroff ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Stellar Core ◽  
Galactic Sources ◽  
The Crab Nebula

Long after a supernova event, the stellar core (neutron star) may continue to excite an extended remnant of ejecta surrounding it, as in the case of the Crab nebula. In contrast, the more common shell supernova remnants (SNRs) appear unaffected by any embedded neutron star.

DA 495 - an unusual supernova remnant with resemblances to the Crab nebula

1983 ◽  
Vol 88 ◽  
pp. 1810 ◽  
Author(s):  
T. L. Landecker ◽  
J. L. Caswell
Keyword(s):  
Supernova Remnant ◽  
Crab Nebula ◽  
The Crab Nebula

scholarly journals Peculiar Differences in Radio and X-ray Synchrotron Radiation from Pulsar Wind Nebulae

2004 ◽  
Vol 218 ◽  
pp. 221-224
Author(s):  
John R. Dickel ◽  
Shiya Wang
Keyword(s):  
Synchrotron Radiation ◽  
Radio Emission ◽  
Supernova Remnants ◽  
Crab Nebula ◽  
Pulsar Wind Nebulae ◽  
X Ray ◽  
Pulsar Wind ◽  
The Crab Nebula

Several Crab-type supernova remnants appear to have very bright non-thermal X-ray cores just around the pulsar or expected pulsar. This X-ray brightness is often not matched by a corresponding increase in radio emission. The best example of this phenomenon is in N157B in the LMC. G21.5−0.9 and possibly 3C 58 also show it while the Crab Nebula and 0540−69.3 do not. Some method to enhance the higher energy particles must be present in these objects.

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