scholarly journals Mode Changing and Giant Pulses in the Millisecond Pulsar PSR B1957+20

2018 ◽  
Vol 867 (1) ◽  
pp. L2 ◽  
Author(s):  
Nikhil Mahajan ◽  
Marten H. van Kerkwijk ◽  
Robert Main ◽  
Ue-Li Pen
Keyword(s):  
Millisecond Pulsar ◽  
Giant Pulses

scholarly journals Statistical and polarization properties of giant pulses of the millisecond pulsar B1937+21

2013 ◽  
Vol 430 (4) ◽  
pp. 2815-2821 ◽  
Author(s):  
V. I. Zhuravlev ◽  
M. V. Popov ◽  
V. A. Soglasnov ◽  
V. I. Kondrat’ev ◽  
Y. Y. Kovalev ◽  
...  
Keyword(s):  
Millisecond Pulsar ◽  
Giant Pulses

scholarly journals Observations of Giant Pulses from Pulsar PSR B1937+21

1996 ◽  
Vol 160 ◽  
pp. 209
Author(s):  
S. E. Thorsett ◽  
J. A. Shrauner ◽  
I. Cognard ◽  
J. H. Taylor
Keyword(s):  
Power Law ◽  
Millisecond Pulsar ◽  
Power Law Distribution ◽  
Sampling System ◽  
Giant Pulse ◽  
Circularly Polarized ◽  
Giant Pulses ◽  
Interstellar Scattering ◽  
The Mean ◽  
The Individual

AbstractWe discuss observations of giant pulses from the millisecond pulsar PSR B1937+21 at 430 MHz, with a baseband sampling system at Arecibo (Shrauner et al., these proceedings) and coherent dedispersion techniques. About one pulse or interpulse per hundred thousand is stronger than 100 times the mean flux density, and the giant pulse strengths follow a power law distribution somewhat shallower than that of the Crab giant pulses. The individual giant pulses appear consistent with impulses shorter than a few microseconds, convolved with an exponential due to interstellar scattering. They are systematically delayed with respect to the average emission, and many are nearly 100% circularly polarized.

scholarly journals Are Giant Pulses Evidence of Self-Organized Criticality?

1996 ◽  
Vol 160 ◽  
pp. 179-180 ◽  
Author(s):  
Matthew D. T. Young ◽  
Brian G. Kenny
Keyword(s):  
Power Laws ◽  
Crab Pulsar ◽  
Statistical Distributions ◽  
Millisecond Pulsar ◽  
Recent Discussion ◽  
Scale Invariant ◽  
Giant Pulse ◽  
Self Organized ◽  
Giant Pulses ◽  
Self Organized Criticality

The statistical distributions of certain giant pulse (GP) properties appear to be well described by power laws. This suggests that the emission mechanism that produces giant pulses is a scale-invariant one. In turn this may indicate that the source of the GPs is in a state of self-organized criticality (SOC). For a recent discussion of SOC see Sornetteet al. (1995).Prior to this conference, the only pulsars reported to exhibit GPs were the Crab pulsar, PSR B0531+21 (Lundgrenet al. 1995), and the millisecond pulsar PSR B1937+21 (Cognardet al. 1996). However, at the conference it was reported that giantmicropulseshad recently been observed from PSR J0437–4715 (Ables and McConnell, this volume). In all cases the statistical distributions of observed GP heights and/or fluxes are found to be well described by simple power laws. The arguments in this note apply to all these pulsars.

Giant pulses from the millisecond pulsar PSR B1937+214

2002 ◽  
Vol 28 (1) ◽  
pp. 21-23 ◽  
Author(s):  
A. D. Kuzmin ◽  
B. Ya. Losovsky
Keyword(s):  
Millisecond Pulsar ◽  
Giant Pulses

scholarly journals Giant Pulses from the Millisecond Pulsar B1821−24

2001 ◽  
Vol 557 (2) ◽  
pp. L93-L96 ◽  
Author(s):  
Roger W. Romani ◽  
Simon Johnston
Keyword(s):  
Millisecond Pulsar ◽  
Giant Pulses

Millisecond Pulsar Alignment: PSR J0437−4715

1998 ◽  
Vol 493 (1) ◽  
pp. 397-403 ◽  
Author(s):  
Kaiyou Chen ◽  
Malvin Ruderman ◽  
Tianhua Zhu
Keyword(s):  
Millisecond Pulsar

scholarly journals Afterglow light curve modulated by a highly magnetized millisecond pulsar

2002 ◽  
Vol 381 (1) ◽  
pp. L5-L8 ◽  
Author(s):  
H.-Y. Chang ◽  
C.-H. Lee ◽  
I. Yi
Keyword(s):  
Light Curve ◽  
Millisecond Pulsar

scholarly journals Millisecond Pulsars

1989 ◽  
Vol 8 ◽  
pp. 161-165
Author(s):  
J.H. Krolik
Keyword(s):  
Neutron Star ◽  
Stellar Evolution ◽  
Close Binary ◽  
Millisecond Pulsar ◽  
Millisecond Pulsars ◽  
Physical Conditions ◽  
Cast Doubt ◽  
Standard Picture ◽  
The Universe ◽  
New System

AbstractMillisecond pulsars are intrinsically interesting because they illustrate some of the most extreme physical conditions to be found anywhere in the Universe, and because their evolution exhibits several stages of great drama. It had been widely believed for several years that spin-up of an old neutron star by accretion from a close stellar companion explained their fast rotation, but the absence of companions in several cases cast doubt on that picture. This spring a millisecond pulsar in a close binary was discovered in which the companion appears to be evaporating, thus reconciling the existence of lone millisecond pulsars with the standard picture. Ongoing observations of this new system, and complementary calculations, promise to answer many of the questions remaining about this dramatic phase in stellar evolution.

A planetary system around the millisecond pulsar PSR1257 + 12

Nature ◽  
1992 ◽  
Vol 355 (6356) ◽  
pp. 145-147 ◽  
Author(s):  
A. Wolszczan ◽  
D. A. Frail
Keyword(s):  
Planetary System ◽  
Millisecond Pulsar
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