THE IMPACT OF TECHNICAL CONSTRAINTS ON THE POSSIBILITY OF RESOLVING THE PULSAR MAGNETOSPHERE BY OBSERVING ITS SCINTILLATIONS
Section: ASTRONOMICAL INSTRUMENTS AND METHODS
Authors:
1.
Lebedev Physical Institute, Astro Space Center
2.
Lebedev Physical Institute, Astro Space Center
3.
Lebedev Physical Institute, Astro Space Center
4.
Lebedev Physical Institute, Astro Space Center
5.
Lebedev Physical Institute, Astro Space Center
6.
Lebedev Physical Institute, Pushchino Radio Astronomy Observatory
7.
Lebedev Physical Institute, Astro Space Center
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDC 52
UDC 53
UDC 520
UDC 521
UDC 523
UDC 524
UDC 52-1
UDC 52-6
CSCSTI 41.00
CSCSTI 29.35
CSCSTI 29.31
CSCSTI 29.33
CSCSTI 29.27
CSCSTI 29.05
Russian Classification of Professions by Education 03.06.01
Russian Classification of Professions by Education 03.05.01
Russian Classification of Professions by Education 03.04.03
Russian Library and Bibliographic Classification 2
Russian Library and Bibliographic Classification 223
Russian Trade and Bibliographic Classification 614
Russian Trade and Bibliographic Classification 6135
BISAK SCI004000 Astronomy
BISAK SCI005000 Physics / Astrophysics
UDC 53
UDC 520
UDC 521
UDC 523
UDC 524
UDC 52-1
UDC 52-6
CSCSTI 41.00
CSCSTI 29.35
CSCSTI 29.31
CSCSTI 29.33
CSCSTI 29.27
CSCSTI 29.05
Russian Classification of Professions by Education 03.06.01
Russian Classification of Professions by Education 03.05.01
Russian Classification of Professions by Education 03.04.03
Russian Library and Bibliographic Classification 2
Russian Library and Bibliographic Classification 223
Russian Trade and Bibliographic Classification 614
Russian Trade and Bibliographic Classification 6135
BISAK SCI004000 Astronomy
BISAK SCI005000 Physics / Astrophysics
Language:
English
Keywords:
scattering; pulsars: individual: B1237+25; ISM: general; techniques: high angular resolution; methods: data analysis
Abstract (English):
Variation in the pulsar dynamic spectra with pulse longitude had in the past been interpreted as a result of the spatial motion of the pulsar emission region and led to some conclusions about the altitude of the emission regions or the magnetosphere structure. Motivated by this research, we used the VLBI observations of PSR B1237+25 with the Arecibo and Green Bank radio telescopes at 324 MHz, performed as part of a RadioAstron observing program, and analyzed scintillations at separate longitudes of the pulse profile. We have found that the fringe phase characteristics of the visibility function vary quasi-sinusoidally as a function of longitude. Also, the dynamic spectra from each of the telescopes shift in frequency as a function of longitude. However, we have found that these shifts arise from the low-level digitizing of the pulsar signal. After correcting for these digital effects, the frequency shifts have largely disappeared. The residual effects may be of instrumental origin or indicate the pulse emission altitudes well below the pulsar light cylinder radius.
Variation in the pulsar dynamic spectra with pulse longitude had in the past been interpreted as a result of the spatial motion of the pulsar emission region and led to some conclusions about the altitude of the emission regions or the magnetosphere structure. Motivated by this research, we used the VLBI observations of PSR B1237+25 with the Arecibo and Green Bank radio telescopes at 324 MHz, performed as part of a RadioAstron observing program, and analyzed scintillations at separate longitudes of the pulse profile. We have found that the fringe phase characteristics of the visibility function vary quasi-sinusoidally as a function of longitude. Also, the dynamic spectra from each of the telescopes shift in frequency as a function of longitude. However, we have found that these shifts arise from the low-level digitizing of the pulsar signal. After correcting for these digital effects, the frequency shifts have largely disappeared. The residual effects may be of instrumental origin or indicate the pulse emission altitudes well below the pulsar light cylinder radius.
Keywords:
scattering; pulsars: individual: B1237+25; ISM: general; techniques: high angular resolution; methods: data analysis
scattering; pulsars: individual: B1237+25; ISM: general; techniques: high angular resolution; methods: data analysis
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