Chemical stratification in a long gamma-ray burst cocoon and early-time spectral signatures of supernovae associated with gamma-ray bursts

Suzuki, Akihiro; Maeda, Keiichi

doi:10.48550/arxiv.2111.12914

Cited by 2 publications

(2 citation statements)

References 106 publications

(141 reference statements)

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“…In all cases the central engine launches a relativistic jet which is accompanied by a cocoon. As the cocoon pierces the stellar envelope, it expands adiabatically and powers a quasi-thermal cooling emission signal (Nakar & Piran 2017;Gottlieb et al 2018a;Gottlieb & Loeb 2020;Suzuki & Maeda 2021). We motivate the cocoon model in the view of current observational data, because FBOTs in our model: i) are associated with the deaths of massive stars, as suggested by the host star-forming galaxies, and the somewhat higher event rate of FBOTs compared to GRBs.…”

Section: Introductionmentioning

confidence: 83%

Shocked jets in CCSNe can power the zoo of fast blue optical transients

Gottlieb,

Tchekhovskoy,

Margutti

2022

Preprint

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Evidence is mounting that recent multi-wavelength detections of fast blue optical transients (FBOTs) in star-forming galaxies comprise a new class of transients, whose origin is yet to be understood. We show that hydrogen-rich collapsing stars that launch relativistic jets near the central engine can naturally explain the entire set of FBOT observables. The jet-star interaction forms a mildly-relativistic shocked jet (inner cocoon) component, which powers cooling emission that dominates the high velocity optical signal during the first few weeks, with a typical energy of ∼ 10 50 − 10 51 erg. During this time, the cocoon radial energy distribution implies that the optical lightcurve exhibits a fast decay of L ∝ ∼ t −2.4 . After a few weeks, when the velocity of the emitting shell is ∼ 0.01 c, the cocoon becomes transparent, and the cooling stellar envelope governs the emission. During this transition, discontinuities may emerge in the lightcurve and spectra, as have been observed in a few FBOTs, such as AT2018cow. The interaction between the cocoon forward shock and the dense circumstellar winds generates synchrotron selfabsorbed emission in the radio bands, featuring a steady rise on a month timescale. After a few months, if the jet successfully pierces the stellar envelope, it decelerates, enters the observer's line of sight, and powers the peak of the radio lightcurve, which rapidly decays thereafter. The jet (and the inner cocoon) become optically thin to X-rays ∼ day after the collapse, allowing X-ray photons to diffuse from the central engine that launched the jet to the observer. Cocoon cooling emission is expected at higher volumetric rates than gamma-ray bursts (GRBs) by a factor of a few, similar to FBOTs. We rule out uncollimated outflows, however both GRB jets and failed collimated jets are compatible with all observables.

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Section: Introductionmentioning

confidence: 83%

Shocked jets in CCSNe can power the zoo of fast blue optical transients

Gottlieb,

Tchekhovskoy,

Margutti

2022

Preprint

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“…There were also a couple of authors that considered a twocomponent explosion that contains a spherical source of energy at the core as well as a relativistic jet. Suzuki & Maeda (2021) considered the effect of the jet on the explosive nucleosynthesis and on the chemical mixing of newly synthesized heavy elements into high velocity outer layers of the ejecta. They found that the jet deposits a large amount of heavy metals in the high velocity layers, which is compatible with observations of Ic-BL SNe.…”

Section: Introductionmentioning

confidence: 99%

Observational signatures of stellar explosions driven by relativistic jets

Eisenberg,

Gottlieb,

Nakar

2022

Preprint

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The role of relativistic jets in unbinding the stellar envelope during a supernova (SN) associated with a gamma-ray burst (GRB) is unclear. To study that, we explore observational signatures of stellar explosions that are driven by jets. We focus on the final velocity distribution of the outflow in such explosions and compare its observational imprints to SN/GRB data. We find that jet driven explosions produce an outflow with a flat distribution of energy per logarithmic scale of proper velocity. The flat distribution seems to be universal as it is independent of the jet and the progenitor properties that we explored. The velocity range of the flat distribution for typical GRB parameters is γβ ≈ 0.03 − 3, where γ is the outflow Lorentz factor and β is its dimensionless velocity. A flat distribution is seen also for collimated choked jets where the highest outflow velocity decreases with the depth at which the jet is choked. Comparison to observations of SN/GRBs rules out jets as the sole explosion source in these events. Instead, in SN/GRB the collapsing star must deposit its energy into two channels -a quasi-spherical (or wide angle) channel and a narrowly collimated one. The former carries most of the energy and is responsible for the SN sub-relativistic ejecta while the latter carries 0.01-0.1 of the total outflow energy and is the source of the GRB. Intriguingly, the same two channels, with a similar energy ratio, were seen in the binary neutron star merger GW170817, suggesting that similar engines are at work in both phenomena.

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Chemical stratification in a long gamma-ray burst cocoon and early-time spectral signatures of supernovae associated with gamma-ray bursts

Cited by 2 publications

References 106 publications

Shocked jets in CCSNe can power the zoo of fast blue optical transients

Shocked jets in CCSNe can power the zoo of fast blue optical transients

Observational signatures of stellar explosions driven by relativistic jets

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