The Evolution of a Newborn Millisecond Magnetar with a Propeller-recycling Disk

Li, Shao-Ze; Yu, Yun-Wei; Zhang, Bing

doi:10.3847/1538-4357/abcc70

Cited by 14 publications

(12 citation statements)

References 58 publications

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“…Furthermore, the observed periodic accretion process may imply the disk has reached a quasi-steady state (The disk may erratic when it born in the collapse of a massive star). Just as the simulation in Li et al (2021), after a significant accretion, the fastness parameter keeps close to 1, the propeller and the accretion effect is comparable. In this scenario, the MHD instability leads the oscillation of disk and triggers the short-duration accretion.…”

Section: Conclusion and Discussionsupporting

confidence: 55%

X-ray Flares Raising upon Magnetar Plateau as an Implication of a Surrounding Disk of Newborn Magnetized Neutron Star

Zheng,

Li,

Zou

et al. 2021

Preprint

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The X-ray flares have usually been ascribed to long-lasting activities of the central engine of gamma-ray bursts (GRBs), e.g., fallback accretion. The GRB X-ray plateaus, however, favor a millisecond magnetar central engine. The fallback accretion can be significantly suppressed due to the propeller effect of a magnetar. Therefore, if the propeller regime cannot resist the mass flow onto the surface of the magnetar efficiently, the X-ray flares raise upon the magnetar plateau would be hinted. In this work, such peculiar cases are connected to the accretion process of a magnetar, and an implication for magnetar-disc structure is given. We investigate the repeating accretion process with multi-flare GRB 050730, and give a discussion for the accreting induced variation of the magnetic field in GRB 111209A. Two or more flares exhibit in the GRB 050730, GRB 060607A, and GRB 140304A; by adopting magnetar mass M = 1.4 M ⊙ and radius R = 12 km, the average mass flow rates of the corresponding surrounding disk are 3.53 × 10 −4 M ⊙ s −1 , 4.23 × 10 −4 M ⊙ s −1 , and 4.33 × 10 −4 M ⊙ s −1 , and the corresponding average sizes of the magnetosphere are 5.01 × 10 6 cm, 6.45 × 10 6 cm, and 1.09 × 10 7 cm, respectively. A statistic analysis that contains 8 GRBs within 12 flares shows that the total mass loading in single flare is ∼ 2 × 10 −5 M ⊙ . In the lost mass of a disk, there are about 0.1% used to feed a collimated jet.

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Section: Conclusion and Discussionsupporting

confidence: 55%

X-ray Flares Raising upon Magnetar Plateau as an Implication of a Surrounding Disk of Newborn Magnetized Neutron Star

Zheng,

Li,

Zou

et al. 2021

Preprint

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“…For such high fallback rates, the accretion flow is likely able to penetrate and squeeze the proto-neutron star magnetosphere, causing an initial phase of direct accretion onto the surface. This might also result in the burial of the magnetic field (see for example Taam & van den Heuvel 1986;Li et al 2021;Lin et al 2021), a scenario that (combined with the subsequent secular re-emergence of the magnetic field) has been invoked to explain the observed properties of Central Compact Objects (CCOs) (Halpern & Gotthelf 2010;Fu & Li 2013;Ho 2015;Zhong et al 2021); a class of young, generally weak-field neutron stars found close to the centers of supernova remnants. After this initial direct accretion phase, as the fallback rate decreases in time, the neutron star could enter a propeller phase that could cause the star to spin-down as in the disk scenario.…”

Section: Accretion From Spherical Fall-backmentioning

confidence: 99%

Long-period Pulsars as Possible Outcomes of Supernova Fallback Accretion

Ronchi¹,

Rea²,

Graber³

et al. 2022

Preprint

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For about half a century the radio pulsar population was observed to spin in the ∼ 0.002-12 s range, with different pulsar classes having spin-period evolution that differs substantially depending on their magnetic fields or past accretion history. The recent detection of several slowly rotating pulsars has re-opened the long-standing question of the exact physics, and observational biases, driving the upper bound of the period range of the pulsar population. In this work, we study the spin-period evolution of pulsars interacting with supernova fallback matter and specifically look at the fallback accretion disk scenario using general assumption for the pulsar spin period and magnetic field at birth, as well as fallback accretion rates. We show that this evolution can differ substantially from the typical dipolar spin-down, and can be very dependent on the ranges of initial parameters at formation, resulting in pulsars that show spin periods longer than their coeval peers. In addition, we study the case of the recently discovered radio transient GLEAM-X J162759.5-523504.3 (P = 1091 s). Long-period isolated pulsars might be more common than expected, being the natural result of supernova fallback accretion, and necessarily having a strong magnetic field.

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“…Thus, most LGRBs are not expected to be associated with SLSNe I in the isolated magnetar-powered scenario. However, their association, if observed in the future, can be explained in the context of magnetar-disk system where the magnetic field of the nascent magnetar could decay significantly due to fallback accretion, since the magnetar-disk scenario is also favored for some LGRB afterglows (e.g., Dai & Liu 2012;Li et al 2021).…”

Section: Resultsmentioning

confidence: 99%

“…where B NS,0 is the initial magnetic field. As for the uncertain characteristic mass M c , we follow Li et al (2021) to adopt M c = 10 −3 M . The magnetic field will rediffuse to the surface of NS due to Ohmic diffusion and Hall drift after a relatively long timescale (e.g., Geppert et al 1999;Fu & Li 2013).…”

Section: Evolution Of a Magnetar With A Diskmentioning

confidence: 99%

“…Outflow could be also generated from the inner disk during the propeller regime. However, as Li et al (2021) pointed out, the kinetic energy of the propeller outflow could be reduced because of (1) low acceleration efficiency, (2) internal dissipation inside the outflow, and (3) interaction between the outflows and the in-falling matter from the outer disk. Thus, the propeller outflow is not considered here.…”

Section: Sn Luminosity Powered By Magnetar-disk Systemmentioning

confidence: 99%

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Supernova luminosity powered by magnetar-disk system

Lin,

Wang,

Wang

et al. 2021

Preprint

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Magnetars are one of the potential power sources for some energetic supernova explosions such as type I superluminous supernovae (SLSNe I) and broad-lined type Ic supernovae (SNe Ic-BL). In order to explore the possible link between these two subclasses of supernovae (SNe), we study the effect of fallback accretion disk on magnetar evolution and magnetar-powered SNe. In this scenario, the interaction between a magnetar and a fallback accretion disk would accelerate the spin of the magnetar in the accretion regime but could result in substantial spin-down of the magnetars in the propeller regime. Thus, the initial rotation of the magnetar plays a less significant role in the spin evolution. Such a magnetar-disk interaction scenario can explain well the light curves of both SNe Ic-BL and SLSNe I, for which the observed differences are sensitive to the initial magnetic field of the magnetar and the fallback mass and timescale for the disk. Compared to the magnetars powering the SNe Ic-BL, those accounting for more luminous SNe usually maintain faster rotation and have relatively lower effective magnetic fields around peak time. In addition, the association between SLSNe I and long gamma-ray bursts, if observed in the future, could be explained in the context of magnetar-disk system.

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The Evolution of a Newborn Millisecond Magnetar with a Propeller-recycling Disk

Cited by 14 publications

References 58 publications

X-ray Flares Raising upon Magnetar Plateau as an Implication of a Surrounding Disk of Newborn Magnetized Neutron Star

X-ray Flares Raising upon Magnetar Plateau as an Implication of a Surrounding Disk of Newborn Magnetized Neutron Star

Long-period Pulsars as Possible Outcomes of Supernova Fallback Accretion

Supernova luminosity powered by magnetar-disk system

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