A possible feedback mechanism of outflows from a black hole hyperaccretion disk in the center of jet-driven iPTF14hls

Liu, Tong; Song, Cui-Ying; Yi, Tuan; Gu, Wei‐Min

doi:10.1016/j.jheap.2019.02.001

Cited by 20 publications

(14 citation statements)

References 62 publications

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“…After a massive star collapses, a rotating stellar-mass BH surrounded by a hyperaccretion disk might form. Using the density profiles of the pre-SN model (for details, see Paper I), we can calculate the mass supply rate of the progenitors (see, e.g., Suwa & Ioka 2011;Woosley & Heger 2012;Matsumoto et al 2015;Liu et al 2018Liu et al , 2019…”

Section: Progenitor Modelmentioning

confidence: 99%

“…Such case is not considered in this work. In the initial hundreds of seconds of the accretion process, the jets are generally choked in the envelope of a collapsar, so no electromagnetic counterparts of the central engine can be observed (see, e.g., Kashiyama et al 2013;Nakauchi et al 2013;Liu et al 2018Liu et al , 2019. Whether the jets can breakout out depends on the activity timescale of the central engine, the scale and density of the dense circumstellar medium (CSM) and the properties of the jets.…”

Section: Progenitor Modelmentioning

confidence: 99%

“…Whether the jets can breakout out depends on the activity timescale of the central engine, the scale and density of the dense circumstellar medium (CSM) and the properties of the jets. If the activity of the central engine lasts long enough to allow the jets to break out of the envelope and CSM, an energetic LGRB will be triggered (e.g., Liu et al 2018Liu et al , 2019.…”

Section: Progenitor Modelmentioning

confidence: 99%

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Black Hole Hyperaccretion in Collapsars. II. Gravitational Waves

Wei¹,

Liu

2020

ApJ

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As progenitors of gamma-ray bursts (GRBs), core collapse of massive stars and coalescence of compact object binaries are believed to be powerful sources of gravitational waves (GWs). In the collapsar scenario, a rotating stellar-mass black hole (BH) surrounded by a hyperaccretion disk might be running in the center of a massive collapsar, which is one of the plausible central engines of long GRBs. Such a BH hyperaccretion disk would be in a state of a neutrino-dominated accretion flow (NDAF) at the initial stage of the accretion process; meanwhile, the jets attempt to break out from the envelope and circumstellar medium to power GRBs. In addition to collapsars, the BH hyperaccretion systems are important sources of neutrinos and GWs. In this paper, we investigated the GW emission generated by the anisotropic neutrino emission from NDAFs in the collapsar scenarios. As the results indicate, the typical frequency of GWs is ∼ 1-100 Hz, and the masses and metallicities of the progenitor stars have slight effects on the GW strains. The GWs from NDAFs might be detected by operational or planned detectors at the distance of 10 kpc. Moreover, comparisons of the detectable GWs from collapsars, NDAFs, and GRB jets (internal shocks) are displayed. By combining the electromagnetic counterparts, neutrinos, and GWs, one may constrain the characteristics of collapsars and central BH accretion systems.

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Section: Progenitor Modelmentioning

confidence: 99%

Section: Progenitor Modelmentioning

confidence: 99%

Section: Progenitor Modelmentioning

confidence: 99%

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Black Hole Hyperaccretion in Collapsars. II. Gravitational Waves

Wei¹,

Liu

2020

ApJ

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“…It is widely believed that they originate from massive collapsars (e.g., Woosley 1993;MacFadyen & Woosley 1999) and binary compact object mergers (e.g., Paczyński 1986;Eichler et al 1989;Narayan et al 1992). Currently, GRB central engines are still uncertain, but there are two leading models, i.e., the stellar-mass black hole (BH) hyperaccretion model (e.g., Woosley 1993;Popham et al 1999;Narayan et al 2001;Yi et al 2017;Liu et al 2018Liu et al , 2019 and for a review see Liu et al (2017) and the model of a rapidly rotating neutron star (NS) with a strong magnetic field of ∼ 10 15 G, et al 2007;Dainotti et al 2008Dainotti et al , 2010Dainotti et al , 2011aDainotti et al , 2013aDainotti et al , 2016Du 2020) and for a review see Dainotti & Del Vecchio (2017). A similar shallow decay also occurs in the optical light curves (e.g., Si et al 2018;Dainotti et al 2020) and Fermi -LAT GRBs (e.g., Dainotti et al 2021).…”

mentioning

confidence: 99%

Statistical analyses on the energies of X-ray plateaus and flares in gamma-ray bursts

Yi,

Du,

Liu

2021

Preprint

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Distinct X-ray plateau and flare phases have been observed in the afterglows of gamma-ray bursts (GRBs), and most of them should be related to central engine activities. In this paper, we collect 174 GRBs with X-ray plateau phases and 106 GRBs with X-ray flares. There are 51 GRBs that overlap in the two selected samples. We analyze the distributions of the proportions of the plateau energy E plateau and the flare energy E flare relative to the isotropic prompt emission energy E γ,iso . The results indicate that they well meet the Gaussian distributions and the medians of the logarithmic ratios are ∼ −0.96 and −1.39 in the two cases. Moreover, strong positive correlations between E plateau (or E flare ) and E γ,iso with slopes of ∼ 0.95 (or ∼ 0.80) are presented. For the overlapping sample, the slope is ∼ 0.80. We argue that most of X-ray plateaus and flares might have the same physical origin but appear with different features because of the different circumstances and radiation mechanisms. We also test the applicabilities of two models, i.e., black holes surrounded by fractured hyperaccretion disks and millisecond magnetars, on the origins of X-ray plateaus and flares.

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“…Some models (e.g. Quataert et al 2019;Liu et al 2019;Gilkis et al 2019) have been proposed, but mostly dealing with the light curve behavior.…”

mentioning

confidence: 99%

A Wind-Driven Model: Application to Peculiar Transients AT2018cow and iPTF14hls

Uno,

Maeda

2020

Preprint

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We propose a wind-driven model for peculiar transients, and apply the model to AT2018cow and iPTF14hls. In the wind-driven model, we assume that a continuous outflow like a stellar wind is injected from a central system. While these transients have different observational properties, this unified model can explain their photometric properties which are not reproduced by a supernova-like instantaneous explosion. Furthermore, the model predicts characteristic spectral features and evolution, which are well in line with those of AT2018cow and iPTF14hls. Despite the different observational properties, the wind model shows that they have some common features; the large mass-loss rates (up to ∼ 20M yr −1 for AT2018cow and ∼ 30M yr −1 for iPTF14hls), the characteristic radii of ∼ 10 13 cm for the launch of the wind, and the kinetic energies of ∼ 10 51 erg. It would indicate that both may be related to events involving a red super giant (RSG), in which the RSG envelope is rapidly ejected by an event at a stellar core scale. On the other hand, the main differences are time scales and the total ejected mass. We then suggests that iPTF14hls may represent a dynamical common-envelope evolution induced by massive binary systems (∼ 50M each). AT2018cow may be either a tidal disruption event of a low-mass RSG by a black hole (BH), or a BH-forming failed supernova.

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A possible feedback mechanism of outflows from a black hole hyperaccretion disk in the center of jet-driven iPTF14hls

Cited by 20 publications

References 62 publications

Black Hole Hyperaccretion in Collapsars. II. Gravitational Waves

Black Hole Hyperaccretion in Collapsars. II. Gravitational Waves

Statistical analyses on the energies of X-ray plateaus and flares in gamma-ray bursts

A Wind-Driven Model: Application to Peculiar Transients AT2018cow and iPTF14hls

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