The Characteristics of Millisecond Pulsar Emission. III. From Low to High Frequencies

1999 ◽  
Vol 526 (2) ◽  
pp. 957-975 ◽  
Author(s):  
Michael Kramer ◽  
Christoph Lange ◽  
Duncan R. Lorimer ◽  
Donald C. Backer ◽  
Kiriaki M. Xilouris ◽  
...  
Keyword(s):  
Millisecond Pulsar ◽  
Pulsar Emission ◽  
High Frequencies

The Characteristics of Millisecond Pulsar Emission. I. Spectra, Pulse Shapes, and the Beaming Fraction

1998 ◽  
Vol 501 (1) ◽  
pp. 270-285 ◽  
Author(s):  
Michael Kramer ◽  
Kiriaki M. Xilouris ◽  
Duncan R. Lorimer ◽  
Oleg Doroshenko ◽  
Axel Jessner ◽  
...  
Keyword(s):  
Millisecond Pulsar ◽  
Pulsar Emission

The Characteristics of Millisecond Pulsar Emission. II. Polarimetry

1998 ◽  
Vol 501 (1) ◽  
pp. 286-306 ◽  
Author(s):  
Kiriaki M. Xilouris ◽  
Michael Kramer ◽  
Axel Jessner ◽  
Alexis von Hoensbroech ◽  
Duncan R. Lorimer ◽  
...  
Keyword(s):  
Millisecond Pulsar ◽  
Pulsar Emission

scholarly journals Toward an Empirical Theory of Pulsar Emission. XII. Exploring the Physical Conditions in Millisecond Pulsar Emission Regions

2017 ◽  
Vol 845 (1) ◽  
pp. 23 ◽  
Author(s):  
Joanna M. Rankin ◽  
Anne Archibald ◽  
Jason Hessels ◽  
Joeri van Leeuwen ◽  
Dipanjan Mitra ◽  
...  
Keyword(s):  
Millisecond Pulsar ◽  
Empirical Theory ◽  
Pulsar Emission ◽  
Physical Conditions

scholarly journals Triplicity of Pulsar Profiles and Orthogonal Polarization Modes

1987 ◽  
Vol 125 ◽  
pp. 58-58
Author(s):  
J. A. Gil
Keyword(s):  
Inner Core ◽  
Emission Region ◽  
Radius Of Curvature ◽  
Orthogonal Polarization ◽  
Pulsar Emission ◽  
Pulsar Radio ◽  
High Frequencies ◽  
The Mean ◽  
Radio Frequencies ◽  
Field Lines

A mechanism for generation of two concentric pulsar beams corresponding to the core and conal pulsar emission is proposed. The inner beam originates close to the star, where the radius of curvature of the dipolar magnetic field lines is suitable for coherent curvature emission at pulsar radio frequencies. Further from the star where the outer beam originates, the radius of curvature of dipolar lines is probably too large, but the actual curvature can be dominated by the toroidal component of field lines twisted back due to the pulsar rotation. One can show that for even moderate twisting the actual radius of curvature leads again to pulsar radio frequencies. Thus, the pulsar emission is a superposition of two beams originating at widely radially separated locations. When the observer's line-of-sight cuts both beams, a three-component profile should be observed. Because of the retardational time delay, the inner (core) component should appear late with respect to the profile midpoint, that is, closer to the traling component. Such an asymmetry is indeed observed in complex profile pulsars. In pulsar magnetosphere, the radius of curvature of dipolar field lines depends on the radius of the emission region in the opposite way than that of the toroidal lines. This explains why core and conal components dominate the mean profile at low and high frequencies, respectively.

scholarly journals PROBING MILLISECOND PULSAR EMISSION GEOMETRY USING LIGHT CURVES FROM THEFERMI/LARGE AREA TELESCOPE

2009 ◽  
Vol 707 (1) ◽  
pp. 800-822 ◽  
Author(s):  
C. Venter ◽  
A. K. Harding ◽  
L. Guillemot
Keyword(s):  
Light Curves ◽  
Millisecond Pulsar ◽  
Large Area ◽  
Pulsar Emission

Quasi-Periodic Oscillations in Dwarf Novae

1979 ◽  
Vol 46 ◽  
pp. 77-88
Author(s):  
Edward L. Robinson
Keyword(s):  
Binary Systems ◽  
Outer Edge ◽  
Light Curves ◽  
Close Binary ◽  
Bright Spot ◽  
Dwarf Novae ◽  
Periodic Oscillations ◽  
High Frequencies ◽  
Short Period ◽  
Typical Time

Three distinct kinds of rapid variations have been detected in the light curves of dwarf novae: rapid flickering, short period coherent oscillations, and quasi-periodic oscillations. The rapid flickering is seen in the light curves of most, if not all, dwarf novae, and is especially apparent during minimum light between eruptions. The flickering has a typical time scale of a few minutes or less and a typical amplitude of about .1 mag. The flickering is completely random and unpredictable; the power spectrum of flickering shows only a slow decrease from low to high frequencies. The observations of U Gem by Warner and Nather (1971) showed conclusively that most of the flickering is produced by variations in the luminosity of the bright spot near the outer edge of the accretion disk around the white dwarf in these close binary systems.

Determination of developmental stage to obtain high frequencies of embryogenic microspores in Brassica napus

1992 ◽  
Vol 84 (3) ◽  
pp. 417-424 ◽  
Author(s):  
Cheryl A. Telmer ◽  
Daina H. Simmonds ◽  
William Newcomb
Keyword(s):  
Brassica Napus ◽  
Developmental Stage ◽  
High Frequencies

Hydrodynamics of a normal fluid up to high frequencies and small wavelengths

1976 ◽  
Vol 37 (11) ◽  
pp. 1255-1266 ◽  
Author(s):  
B. Quentrec
Keyword(s):  
Normal Fluid ◽  
High Frequencies
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