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The GRB-SLSN Connection: mis-aligned magnetars, weak jet emergence, and observational signatures
High Energy Astrophysical Phenomena · Submitted 2 May 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We propose a new unifying model for magnetar thermalization and jet formation: misalignment between the rotation (${\bf \Omega}$) and magnetic dipole (${\bf \mu}$) axes thermalizes a fraction of the spindown power by reconnection in the striped equatorial wind, providing a guaranteed source of "thermal" emission to power the supernova.
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The abstract, sentence by sentence
Multiple observational lines of evidence support a connection between hydrogen-poor superluminous supernovae (SLSNe) and long duration gamma-ray bursts (GRBs). Both events require a powerful central energy source, usually attributed to a millisecond magnetar or an accreting black hole. The GRB-SLSN link raises several theoretical questions: What distinguishes the engines responsible for these different phenomena? Can a single engine power both a GRB and a luminous SN in the same event? We propose a new unifying model for magnetar thermalization and jet formation: misalignment between the rotation (${\bf \Omega}$) and magnetic dipole (${\bf \mu}$) axes thermalizes a fraction of the spindown power by reconnection in the striped equatorial wind, providing a guaranteed source of "thermal" emission to power the supernova. The remaining un-thermalized power energizes a relativistic jet. In this picture, the GRB-SLSN dichotomy is directly linked to ${\bf \Omega \cdot \mu}$. We extend earlier work to show that even weak relativistic jets of luminosity $\sim10^{46}$ erg s$^{-1}$ can escape the expanding SN ejecta hours after the explosion, implying that escaping relativistic jets may accompany many SLSNe. We calculate the observational signature of these jets. We show that they may produce transient UV cocoon emission lasting a few hours when the jet breaks out of the ejecta surface. A longer-lived optical/UV signal may originate from a mildly-relativistic wind driven from the interface between the jet and the ejecta walls. This provides a new explanation for the secondary early-time maximum observed in some SLSNe light curves, such as LSQ14bdq. This scenario also predicts a population of GRB from on-axis jets with extremely long durations, potentially similar to the population of "jetted tidal disruption events", in coincidence with a small subset of SLSNe.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Multiple observational lines of evidence support a connection between hydrogen-poor superluminous supernovae (SLSNe) and long duration gamma-ray bursts (GRBs). | background 1.00 | 0.06 | 0.04 | asserted 0.98 |
| s1 | Both events require a powerful central energy source, usually attributed to a millisecond magnetar or an accreting black hole. | background 1.00 | 0.04 | 0.02 | asserted 0.68 |
| s2 | The GRB-SLSN link raises several theoretical questions: What distinguishes the engines responsible for these different phenomena? | gap 0.71 | 0.06 | 0.02 | asserted 0.81 |
| s3 | Can a single engine power both a GRB and a luminous SN in the same event? | gap 0.79 | 0.04 | 0.03 | unclear 0.66 |
| s4 | We propose a new unifying model for magnetar thermalization and jet formation: misalignment between the rotation (${\bf \Omega}$) and magnetic dipole (${\bf \mu}$) axes thermalizes a fraction of the spindown power by reconnection in the striped equatorial wind, providing a guaranteed source of "thermal" emission to power the supernova. | contribution 0.94 | 0.76 | 0.56 | asserted 0.74 |
| s5 | The remaining un-thermalized power energizes a relativistic jet. | contribution 0.52 | 0.41 | 0.08 | asserted 1.00 |
| s6 | In this picture, the GRB-SLSN dichotomy is directly linked to ${\bf \Omega \cdot \mu}$. | interpretation 0.83 | 0.48 | 0.34 | asserted 1.00 |
| s7 | We extend earlier work to show that even weak relativistic jets of luminosity $\sim10^{46}$ erg s$^{-1}$ can escape the expanding SN ejecta hours after the explosion, implying that escaping relativistic jets may accompany many SLSNe. | result 0.80 | 0.88 | 0.20 | asserted 0.56 |
| s8 | We calculate the observational signature of these jets. | contribution 0.69 | 0.90 | 0.03 | asserted 0.78 |
| s9 | We show that they may produce transient UV cocoon emission lasting a few hours when the jet breaks out of the ejecta surface. | result 0.99 | 0.84 | 0.11 | hedged possibility 0.95 |
| s10 | A longer-lived optical/UV signal may originate from a mildly-relativistic wind driven from the interface between the jet and the ejecta walls. | result 0.77 | 0.74 | 0.07 | hedged possibility 0.98 |
| s11 | This provides a new explanation for the secondary early-time maximum observed in some SLSNe light curves, such as LSQ14bdq. | interpretation 0.93 | 0.65 | 0.10 | asserted 0.73 |
| s12 | This scenario also predicts a population of GRB from on-axis jets with extremely long durations, potentially similar to the population of "jetted tidal disruption events", in coincidence with a small subset of SLSNe. | interpretation 0.64 | 0.62 | 0.13 | hedged possibility 0.50 |
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The paper
Original abstract
Multiple observational lines of evidence support a connection between hydrogen-poor superluminous supernovae (SLSNe) and long duration gamma-ray bursts (GRBs). Both events require a powerful central energy source, usually attributed to a millisecond magnetar or an accreting black hole. The GRB-SLSN link raises several theoretical questions: What distinguishes the engines responsible for these different phenomena? Can a single engine power both a GRB and a luminous SN in the same event? We propose a new unifying model for magnetar thermalization and jet formation: misalignment between the rotation (${\bf \Omega}$) and magnetic dipole (${\bf \mu}$) axes thermalizes a fraction of the spindown power by reconnection in the striped equatorial wind, providing a guaranteed source of "thermal" emission to power the supernova. The remaining un-thermalized power energizes a relativistic jet. In this picture, the GRB-SLSN dichotomy is directly linked to ${\bf \Omega \cdot \mu}$. We extend earlier work to show that even weak relativistic jets of luminosity $\sim10^{46}$ erg s$^{-1}$ can escape the expanding SN ejecta hours after the explosion, implying that escaping relativistic jets may accompany many SLSNe. We calculate the observational signature of these jets. We show that they may produce transient UV cocoon emission lasting a few hours when the jet breaks out of the ejecta surface. A longer-lived optical/UV signal may originate from a mildly-relativistic wind driven from the interface between the jet and the ejecta walls. This provides a new explanation for the secondary early-time maximum observed in some SLSNe light curves, such as LSQ14bdq. This scenario also predicts a population of GRB from on-axis jets with extremely long durations, potentially similar to the population of "jetted tidal disruption events", in coincidence with a small subset of SLSNe.
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References
How the literature uses it
8 arXiv papers cite this in 17 sentences
Papers citing it · 11 sentences without a confident label
Uses its method or tool 1 paper
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Assuming the analytic density profile from equation 12 of [ref] , and that the characteristic velocity can be well approximated by , the kinetic energy is given by $=1/2$ $^2$ (a similar result is obtained if we instead assume that the ejecta mass is entirely concentrated in a thin shell).
The magnetar model for Type I superluminous supernovae I: Bayesian analysis of the full multicolour light curve sample with MOSFiT · Modules: physical constraints · 0.90
Cites it as background 4 papers
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Magnetic dissipation inside the tenuous wind bubble with radius $R_w$ has been considered in the context of magnetar models for SNe Ibc-BL, SLSNe and rapidly rising optical transients [ref] .
Quasithermal GeV neutrinos from neutron-loaded magnetized outflows in core-collapse supernovae: spectra and light curves · Neutrino-driven winds and neutron decoupling · 0.92
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This has been variously interpreted as shock cooling in low-density extended material around the progenitor [ref] , a second shock breakout driven by the hydrodynamic impact of a central engine [ref] , or a sign of an off-axis jet driving a mildly relativistic wind [ref] .
The magnetar model for Type I superluminous supernovae I: Bayesian analysis of the full multicolour light curve sample with MOSFiT · SLSN sample · 0.83
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The origin of these bumps is currently unknown, although several theoretical explanations have been posed (e.g., [ref] ).
Theoretical Models of Optical Transients. I. A Broad Exploration of the Duration-Luminosity Phase Space · Specific Engine Insights · 0.97
What it cites · 24 sentences without a confident label
Cites as support 4 papers
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Further indirect evidence for a connection between SLSNe, GRB, and magnetar birth was provided by the recent localization of the repeating fast radio burst (FRB) FRB 121102 [ref] in a dwarf irregular galaxy [ref] with properties of mass, metallicity, and star formation remarkably similar to the hosts of SLSNe and GRB [ref] .
The direct localization of a fast radio burst and its host · Introduction · 0.96
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Further indirect evidence for a connection between SLSNe, GRB, and magnetar birth was provided by the recent localization of the repeating fast radio burst (FRB) FRB 121102 [ref] in a dwarf irregular galaxy [ref] with properties of mass, metallicity, and star formation remarkably similar to the hosts of SLSNe and GRB [ref] .
The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102 · Introduction · 0.96
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Further indirect evidence for a connection between SLSNe, GRB, and magnetar birth was provided by the recent localization of the repeating fast radio burst (FRB) FRB 121102 [ref] in a dwarf irregular galaxy [ref] with properties of mass, metallicity, and star formation remarkably similar to the hosts of SLSNe and GRB [ref] .
Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long Duration Gamma-ray Bursts · Introduction · 0.96
Cites as background 2 papers
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The process by which this “friction” occurs is left unspecified, but it could plausibly be related to intrinsic variability of the central engine [ref] , conical recollimation shocks between the jet and confining (evacuated) funnel [ref] , Kelvin-Helmholtz instabilities at the jet-ejecta interface, or some other unspecified process.
Three-dimensional Simulations of AGN Jets: Magnetic Kink Instability versus Conical Shocks · Thermal Wind from Jet-Ejecta Interface · 0.90
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The latter might be produced by pre-explosion stellar mass loss (as in Type IIn supernovae; [ref] ), pulsational pair instability (e.g. [ref] ), or a relic proto-stellar disk ( [ref] ).
Pulsational Pair-Instability Supernovae · Introduction · 0.85
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