MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503Citation formats

  • External authors:
  • Andrzej Szary
  • Joeri van Leeuwen
  • Geoffrey Wright
  • Caterina Tiburzi
  • Yogesh Maan

Standard

MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503. / Szary, Andrzej; van Leeuwen, Joeri; Wright, Geoffrey; Weltevrede, Patrick; Agar, Crispin; Tiburzi, Caterina; Maan, Yogesh; Keith, Michael.

In: The Astrophysical Journal, 03.06.2022.

Research output: Contribution to journalArticlepeer-review

Harvard

Szary, A, van Leeuwen, J, Wright, G, Weltevrede, P, Agar, C, Tiburzi, C, Maan, Y & Keith, M 2022, 'MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503', The Astrophysical Journal.

APA

Szary, A., van Leeuwen, J., Wright, G., Weltevrede, P., Agar, C., Tiburzi, C., Maan, Y., & Keith, M. (Accepted/In press). MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503. The Astrophysical Journal.

Vancouver

Szary A, van Leeuwen J, Wright G, Weltevrede P, Agar C, Tiburzi C et al. MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503. The Astrophysical Journal. 2022 Jun 3.

Author

Szary, Andrzej ; van Leeuwen, Joeri ; Wright, Geoffrey ; Weltevrede, Patrick ; Agar, Crispin ; Tiburzi, Caterina ; Maan, Yogesh ; Keith, Michael. / MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503. In: The Astrophysical Journal. 2022.

Bibtex

@article{0636791fb16e46c0abae96df254f8848,
title = "MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503",
abstract = "We present an analysis of the subpulse drift in PSR J1750-3503, which is characterized by abrupt transitions of drift direction. As the pulsar does not exhibit other mode changes or clear nulling, it is an ideal candidate system for studying the phenomenon of drift direction change. For ∼80% of the time the subpulses are characterized by positive drift - from early to later longitudes - while the drift direction is negative in the other ∼20%. The subpulse separation for single pulses with positive drift, P2=(18.8±0.1)∘, is higher then for single pulses with negative drift, P2=(17.5±0.2)∘. When the drift is stable, the measured repetition time of the drift pattern is Pobs3=(43.5±0.4)P, where P is pulsar period. We show that the observed data can be reproduced by a carousel models with subpulse rotation around the magnetic axis using purely dipolar configuration of surface magnetic field. The observed drift characteristics can be modeled assuming that the actual repetition time P3<2P, such that we observe its aliased value. A small variation in P3, of the order of 6% (or less assuming higher alias orders), is enough to reproduce the characteristic drift direction changes we observe.",
author = "Andrzej Szary and {van Leeuwen}, Joeri and Geoffrey Wright and Patrick Weltevrede and Crispin Agar and Caterina Tiburzi and Yogesh Maan and Michael Keith",
year = "2022",
month = jun,
day = "3",
language = "English",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",

}

RIS

TY - JOUR

T1 - MEERKAT OBSERVATIONS OF THE REVERSING DRIFTING SUBPULSES IN PSR J1750-3503

AU - Szary, Andrzej

AU - van Leeuwen, Joeri

AU - Wright, Geoffrey

AU - Weltevrede, Patrick

AU - Agar, Crispin

AU - Tiburzi, Caterina

AU - Maan, Yogesh

AU - Keith, Michael

PY - 2022/6/3

Y1 - 2022/6/3

N2 - We present an analysis of the subpulse drift in PSR J1750-3503, which is characterized by abrupt transitions of drift direction. As the pulsar does not exhibit other mode changes or clear nulling, it is an ideal candidate system for studying the phenomenon of drift direction change. For ∼80% of the time the subpulses are characterized by positive drift - from early to later longitudes - while the drift direction is negative in the other ∼20%. The subpulse separation for single pulses with positive drift, P2=(18.8±0.1)∘, is higher then for single pulses with negative drift, P2=(17.5±0.2)∘. When the drift is stable, the measured repetition time of the drift pattern is Pobs3=(43.5±0.4)P, where P is pulsar period. We show that the observed data can be reproduced by a carousel models with subpulse rotation around the magnetic axis using purely dipolar configuration of surface magnetic field. The observed drift characteristics can be modeled assuming that the actual repetition time P3<2P, such that we observe its aliased value. A small variation in P3, of the order of 6% (or less assuming higher alias orders), is enough to reproduce the characteristic drift direction changes we observe.

AB - We present an analysis of the subpulse drift in PSR J1750-3503, which is characterized by abrupt transitions of drift direction. As the pulsar does not exhibit other mode changes or clear nulling, it is an ideal candidate system for studying the phenomenon of drift direction change. For ∼80% of the time the subpulses are characterized by positive drift - from early to later longitudes - while the drift direction is negative in the other ∼20%. The subpulse separation for single pulses with positive drift, P2=(18.8±0.1)∘, is higher then for single pulses with negative drift, P2=(17.5±0.2)∘. When the drift is stable, the measured repetition time of the drift pattern is Pobs3=(43.5±0.4)P, where P is pulsar period. We show that the observed data can be reproduced by a carousel models with subpulse rotation around the magnetic axis using purely dipolar configuration of surface magnetic field. The observed drift characteristics can be modeled assuming that the actual repetition time P3<2P, such that we observe its aliased value. A small variation in P3, of the order of 6% (or less assuming higher alias orders), is enough to reproduce the characteristic drift direction changes we observe.

M3 - Article

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

ER -