Effect of the excited states of a bleachable agent on the dynamics of the development of giant-pulse emission in a laser with a passive shutter

1976 ◽  
Vol 24 (3) ◽  
pp. 309-313
Author(s):  
A. A. Kovalev ◽  
V. A. Pilipovich ◽  
Yu. V. Razvin
1969 ◽  
Vol 10 (2) ◽  
pp. 171-173 ◽  
Author(s):  
V. I. Malyshev ◽  
A. S. Markin ◽  
A. A. Sychev

2011 ◽  
Vol 741 (1) ◽  
pp. 53 ◽  
Author(s):  
Walid A. Majid ◽  
Charles J. Naudet ◽  
Stephen T. Lowe ◽  
Thomas B. H. Kuiper

2004 ◽  
Vol 218 ◽  
pp. 315-318
Author(s):  
Simon Johnston ◽  
Roger W. Romani

We briefly review observational manifestations of pulsars with giant pulse emission and consider quasi-giant pulse phenomena in other pulsars. We argue that power-law statistics give the best definition of giant pulses. Finally, we speculate as to the origin of the giant pulses and a possible link with high energy emission.


2012 ◽  
Vol 144 (5) ◽  
pp. 155 ◽  
Author(s):  
Ashok K. Singal ◽  
Hari Om Vats
Keyword(s):  

2017 ◽  
Vol 13 (S337) ◽  
pp. 378-379
Author(s):  
Bradley W. Meyers ◽  
Steven E. Tremblay ◽  
N. D. Ramesh Bhat ◽  
Ryan M. Shannon

AbstractThe frequency dependence of normal pulsar radio emission is typically observed to be a power law, with some indications of a flattening or turnover at low frequencies (≲ 100 MHz). The spectrum of the Crab pulsar’s giant pulse emission has not been examined as closely. We conducted simultaneous wideband observations of the Crab pulsar, with the Parkes radio telescope and the Murchison Widefield Array, to study the spectral behaviour of its giant pulses. Our analysis shows that the mean spectral index of Crab giant pulses flattens at low frequencies, from −2.6 ± 0.5 between the Parkes bands, to −0.7 ± 1.4 between the lowest MWA subbands.


1968 ◽  
Vol 28 (6) ◽  
pp. 422-423 ◽  
Author(s):  
U. Deserno ◽  
D. Röss ◽  
G. Zeidler
Keyword(s):  

1988 ◽  
Vol 102 ◽  
pp. 239
Author(s):  
M.S.Z. Chaghtai

Using R.D. Cowan’s computations (1979) and parametric calculations of Meinders et al (1982), old analyses are thoroughly revised and extended at Aligarh, of Zr III by Khan et al (1981), of Nb IV by Shujauddin et Chaghtai (1985), of Mo V by Tauheed at al (1985). Cabeza et al (1986) confirmed the last one largely.Extensive studies have been reported of the 1–e spectra, Zr IV (Rahimullah et al 1980; Acquista and Reader 1980), Nb V (Shujauddin et al 1982; Kagan et al 1981) and Mo VI (Edlén et al 1985). Some interacting 4p54d2levels of these spectra have been reported from our laboratory, also.Detailed spectral analyses of transitions between excited states have furnished complete energy values for J ≠ 1 levels of these spectra during 1970s and 80s. Shujauddin et al (1982) have worked out Nb VI and Tauheed et al (1984) Mo VII from our lab, while Khan et al (1981) share the work on Zr V with Reader and Acquista (1979).


Physica ◽  
1952 ◽  
Vol 18 (2) ◽  
pp. 1101-1104
Author(s):  
B FLOWERS
Keyword(s):  

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