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:
UDK 52 Астрономия. Геодезия
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC 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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