A precessing magnetar model for GLEAM-X J162759.5-523504.3

Ekşi, K. Yavuz; Şaşmaz, Sinem

doi:10.48550/arxiv.2202.05160

Cited by 2 publications

(2 citation statements)

References 32 publications

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“…The corresponding period of free precession is P precession = P/ε ∼ 10 3 s. This may explain the pulsation period of GLEAM-X J1627 (Eksi & Sasmaz 2022).…”

Section: The 1091 S Period Is Unlikely To Be the Precession Periodmentioning

confidence: 87%

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Discussions on the Nature of GLEAM-X J162759.5–523504.3

Tong

2023

ApJ

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The nature of the long-period radio transient GLEAM-X J162759.5−523504.3 (hereafter GLEAM-X J1627) is discussed. We try to understand both its radio emission and pulsation in the neutron star scenario as an alternative to the white dwarf model. We think that (1) from the radio emission point of view, GLEAM-X J1627 can be a radio-loud magnetar; (2) from the rotational evolution point of view, GLEAM-X J1627 is unlikely to be an isolated magnetar; (3) the 1091 s period is unlikely to be the precession period; (4) GLEAM-X J1627 may be a radio-loud magnetar spun down by a fallback disk; (5) the pulsar death line is modified due to the presence of a fallback disk or a twisted magnetic field. In both cases, a higher maximum acceleration potential can be obtained. This may explain why GLEAM-X J1627 is still radioactive with such a long pulsation period; and (6) general constraints on the neutron star magnetic field and initial disk mass are given analytically. Possible ways to discriminate between different modelings are also discussed.

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“…The corresponding period of free precession is P precession = P/ε ∼ 10 3 s. This may explain the pulsation period of GLEAM-X J1627 (Eksi & Sasmaz 2022).…”

Section: The 1091 S Period Is Unlikely To Be the Precession Periodmentioning

confidence: 87%

“…It cannot be excluded that the long pulsation period of GLEAM-X J1627 is due to precession (Eksi & Sasmaz 2022). However, the exactness of periods may favor a rotational or orbital period (Hurley-Walker et al 2022).…”

Section: Comparison With Other Modelingsmentioning

confidence: 99%

Discussions on the Nature of GLEAM-X J162759.5–523504.3

Tong

2023

ApJ

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Evolutionary implications of a magnetar interpretation for GLEAM-X J162759.5–523504.3

Suvorov

Melatos

2023

Monthly Notices of the Royal Astronomical Society

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The radio pulsar GLEAM-X J162759.5–523504.3 has an extremely long spin period (P = 1091.17 s), and yet seemingly continues to spin down rapidly ($\dot{P} < 1.2 \times 10^{-9}\, \mbox{ss}^{-1}$). The magnetic field strength that is implied, if the source is a neutron star undergoing magnetic dipole braking, could exceed 1016 G. This object may therefore be the most magnetised neutron star observed to date. In this paper, a critical analysis of a magnetar interpretation for the source is provided. (i) A minimum polar magnetic field strength of B ∼ 5 × 1015 G appears to be necessary for the star to activate as a radio pulsar, based on conventional ‘death valley’ assumptions. (ii) Back-extrapolation from magnetic braking and Hall-plastic-Ohm decay suggests that a large angular momentum reservoir was available at birth to support intense field amplification. (iii) The observational absence of X-rays constrains the star’s field strength and age, as the competition between heating from field decay and Urca cooling implies a surface luminosity as a function of time. If the object is an isolated, young (∼10 kyr) magnetar with a present-day field strength of B ≳ 1016 G, the upper limit (≈1030 ergs−1) set on its thermal luminosity suggests it is cooling via a direct Urca mechanism.

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A precessing magnetar model for GLEAM-X J162759.5-523504.3

Cited by 2 publications

References 32 publications

Discussions on the Nature of GLEAM-X J162759.5–523504.3

Discussions on the Nature of GLEAM-X J162759.5–523504.3

Evolutionary implications of a magnetar interpretation for GLEAM-X J162759.5–523504.3

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