Supernova Luminosity Powered by Magnetar–Disk System

Lin, Weili; Wang, Lingjun; Dai, Z. G.

doi:10.3847/2041-8213/ac004a

Cited by 15 publications

(17 citation statements)

References 59 publications

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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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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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“…Comparing to stellar fragment fallback determined accretion (e.g., Lin et al 2021), the MHD instability induced periodic accretion process have a shorter time interval for two successive accretion, for this scenario, the inner disk ram pressure can be released timely. 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).…”

Section: Conclusion and Discussionmentioning

confidence: 88%

“…A corotating magnetosphere of the magnetized NS preventing the plasma accretion and throwing away the accreting materials were figured as propeller (Illarionov & Sunyaev 1975;Campana et al 1998). A competing process of accretion and propeller was figured in the recent studies (e.g., Eks ¸i et al 2005;Gompertz et al 2014;Lin et al 2021). However, the coexistence of accretion and outflow was also suggested by some of the magnetohydrodynamic (MHD) simulative studies (e.g., Goodson et al 1997;Romanova et al 2005Romanova et al , 2009Romanova et al , 2018Ustyugova et al 2006).…”

Section: Introductionmentioning

confidence: 99%

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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“…After fallback accretion has slowed, the magnetar would subsequently spin down via the propellor mechanism and/or dipole radiation, driving a type Ic-BL SN. In this scenario, Ic-BL can be produced by events with large magnetic fields of B ∼ 10 15 G and short fallback times of t fb ∼ 100 s, while SLSNe Ic can be produced by events with lower magnetic fields of B ∼ 10 14 G and long fallback times of t fb ∼ 10 4 s (Lin et al 2020(Lin et al , 2021.…”

Section: Magnetar Central Enginesmentioning

confidence: 99%

The spins of compact objects born from helium stars in binary systems

Fuller,

2022

Preprint

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The angular momentum (AM) content of massive stellar cores helps to determine the natal spin rates of neutron stars and black holes. Asteroseismic measurements of low-mass stars have proven that stellar cores rotate slower than predicted by most prior work, so revised models are necessary. In this work, we apply an updated AM transport model based on the Tayler instability to massive helium stars in close binaries, in which tidal spin-up can greatly increase the star's AM. Consistent with prior work, these stars can produce highly spinning black holes upon core-collapse if the orbital period is less than P orb 1 day. For neutron stars, we predict a strong correlation between the pre-explosion mass and the neutron star rotation rate, with millisecond periods (P NS 5 ms) only achievable for massive (M 10 M ) helium stars in tight (P orb 1 day) binaries. Finally, we discuss our models in relation to type Ib/c supernovae, superluminous supernove, gamma-ray bursts, and LIGO measurements of black hole spins. Our models are roughly consistent with the rates and energetics of these phenomena, with the exception of broad-lined Ic supernovae, whose high rates and ejecta energies are difficult to explain.

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Supernova Luminosity Powered by Magnetar–Disk System

Cited by 15 publications

References 59 publications

Long-period Pulsars as Possible Outcomes of Supernova Fallback Accretion

Long-period Pulsars as Possible Outcomes of Supernova Fallback Accretion

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

The spins of compact objects born from helium stars in binary systems

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