Microstructure Crosscorrelation in Pulses Simultaneously Observed at Frequencies Separated by up to 1 GHz

Symposium - International Astronomical Union ◽

10.1017/s007418090009286x ◽

1981 ◽

Vol 95 ◽

pp. 191-196

Author(s):

Valentin Boriakoff ◽

Dale C. Ferguson

Keyword(s):

Component Separation ◽

Pulse Profile ◽

Double Peak ◽

Arecibo Observatory

Microstructure crosscorrelation of pulses observed simultaneously at various separations in frequency in the range of 196 to 1420 MHz was done for PSR 0950+08 and PSR 1133+16 at the Arecibo Observatory. Microstructure and subpulse components were identified in the crosscorrelations, and their behaviour vs. pulse longitude was studied. Drastic differences in the subpulse and micropulse behaviour are noted, related in particular to component separation in the double peak average pulse profile of PSR 1133+16. Here the subpulses follow the average pulse profile component separation but the microstructure does not. Interpretation and constraints in terms of some current theories are also presented.

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Pulsar Discovery by Global Volunteer Computing: Fig. 1

Science ◽

10.1126/science.1195253 ◽

2010 ◽

Vol 329 (5997) ◽

pp. 1305-1305 ◽

Cited By ~ 38

Author(s):

B. Knispel ◽

B. Allen ◽

J. M. Cordes ◽

J. S. Deneva ◽

D. Anderson ◽

...

Keyword(s):

Survey Data ◽

Large Data ◽

Large Data Sets ◽

Volunteer Computing ◽

Data Sets ◽

Pulse Profile ◽

Computing Power ◽

Spin Period ◽

Arecibo Observatory ◽

Computer Power

Einstein@Home aggregates the computer power of hundreds of thousands of volunteers from 192 countries to mine large data sets. It has now found a 40.8-hertz isolated pulsar in radio survey data from the Arecibo Observatory taken in February 2007. Additional timing observations indicate that this pulsar is likely a disrupted recycled pulsar. PSR J2007+2722’s pulse profile is remarkably wide with emission over almost the entire spin period; the pulsar likely has closely aligned magnetic and spin axes. The massive computing power provided by volunteers should enable many more such discoveries.

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On the radio frequency dependence of the pulse delay phenomenon in PSR B0943+10

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab472 ◽

2021 ◽

Author(s):

S A Suleymanova ◽

A N Kazantsev ◽

J M Rankin ◽

S V Logvinenko

Keyword(s):

Amplitude Ratio ◽

Wide Frequency Range ◽

Special Method ◽

Pulse Profile ◽

Pulse Delay ◽

Pulse Phase ◽

Exponential Change ◽

Arecibo Observatory ◽

Delay Phenomenon ◽

Vacuum Gap

Abstract We report the result of measurements of a gradual shift of the integrated pulses towards later spin phase of the anomalous pulsar B0943+10 at the high radio frequencies. We have used observations from the Arecibo Observatory and the GMRT at 327 and 325 MHz correspondingly. For the measurements we have proposed a special method for calculating the correct positions of the partially merged two components of the pulse profile shape with significant temporal changes in their amplitude ratio. The exponential change in the pulse phase with an amplitude of 4 ms and characteristic time of about 1 hour has been found. Comparison of our measurements at 325 and 327 MHz with those at the lower frequencies of 25–80, 62 and 112 MHz have shown that the character of the process does not depend on frequency across a wide frequency range. The result is very important for constraining the nature of the delay. It supports the assumption that the process results from changes in the vacuum gap near the surface of the pulsar. The further correlation between changes in the pulse phase and its intensity is discussed.

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Geodetic Precession and the Binary Pulsar B1913+16

International Astronomical Union Colloquium ◽

10.1017/s0252921100059236 ◽

2000 ◽

Vol 177 ◽

pp. 125-126 ◽

Cited By ~ 1

Author(s):

A. Karastergiou ◽

M. Kramer ◽

N. Wex ◽

A. von Hoensbroech

Keyword(s):

Component Separation ◽

Testing Model ◽

Binary Pulsar ◽

Geodetic Precession ◽

Additional Information ◽

New Information ◽

Model Predictions ◽

Arecibo Observatory ◽

First Time ◽

System Geometry

AbstractA change of the component separation in the profiles of the binary pulsar PSR B1913+16 has been observed for the first time (Kramer 1998) as expected by geodetic precession. In this work we extend the previous work by accounting for recent data from the Effelsberg 100-m telescope and Arecibo Observatory and testing model predictions. We demonstrate how the new information will provide additional information on the solutions of the system geometry.

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