Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Tamborra, Irene; Ando, Shinʼichiro

doi:10.1088/1475-7516/2015/09/036

Cited by 33 publications

(30 citation statements)

References 87 publications

(208 reference statements)

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“…The above relation for a typical HL-GRB with Γ = 300 gives an opening angle of θ j = 6 • , consistent with observations (Goldstein et al 2016). The break at Γ = 100 is taken from Cenko et al (2011);Ackermann et al (2011);Dermer et al (2014); Tamborra & Ando (2015). Measurements of the jet opening angle for LL-GRBs are more uncertain.…”

Section: Properties Of the Astrophysical Jetsupporting

confidence: 78%

Exploring the Properties of Choked Gamma-ray Bursts with IceCube’s High-energy Neutrinos

Denton

Tamborra

2018

ApJ

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Long duration gamma-ray bursts (GRBs) have often been considered as the natural evolution of some corecollapse supernova (CCSN) progenitors. However, the fraction of CCSNe linked to astrophysical jets and their properties are still poorly constrained. While any successful astrophysical jet harbored in a CCSN should produce high energy neutrinos, photons may be able to successfully escape the stellar envelope only for a fraction of progenitors, possibly leading to the existence of high-luminosity, low-luminosity and notelectromagnetically bright ("choked") GRBs. By postulating a CCSN-GRB connection, we accurately model the jet physics within the internal-shock GRB model and assume scaling relations for the GRB parameters that depend on the Lorentz boost factor Γ. The IceCube high energy neutrino flux is then employed as an upper limit of the neutrino background from electromagnetically bright and choked GRBs to constrain the jet and the progenitor properties. The current IceCube data set is compatible with up to 1% of all CCSNe harboring astrophysical jets. Interestingly, those jets are predominantly choked. Our findings suggest that neutrinos can be powerful probes of the burst physics and can provide major insights on the CCSN-GRB connection.

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Section: Properties Of the Astrophysical Jetsupporting

confidence: 78%

Exploring the Properties of Choked Gamma-ray Bursts with IceCube’s High-energy Neutrinos

Denton

Tamborra

2018

ApJ

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“…We also show the effects of meson and muon cooling on the all-flavour neutrino spectra (compare dashed blue and dashdotted red lines). Above the peak energy of the neutrino spectrum, the flux decreases because pions and muons cool before they decay (see also Baerwald et al 2011;Petropoulou 2014;Tamborra & Ando 2015). A comparison of the numerical and semi-analytical results for the neutrino emission is presented in Fig.…”

Section: Numerical Resultsmentioning

confidence: 99%

“…However, a fraction of their populations can cool by emitting synchrotron photons before their decay (for more details, see Appendix A). Pion and muon synchrotron cooling can affect both the photon and neutrino spectra (Baerwald et al 2011;Petropoulou et al 2014b;Tamborra & Ando 2015). Neutrons do not typically interact with soft photons before they escape the source (i.e., the source is optically thin to neutron-photon interactions), and neutrinos escape the source without any interactions on a light-crossing time.…”

Section: Numerical Codementioning

confidence: 99%

“…If Fε v,obs ∝ ε χ v,obs , we approximately account for the cooling effects by describing the neutrino flux as Fε v,obs ∝ ε χ−2 v,obs above an energy that corresponds to that of a pion with equal synchrotron cooling and decay timescales (this is indicated with a diamond in the figure). While this is a rough approximation (for a detailed analytical treatment of cooling effects, see e.g., He et al 2012;Tamborra & Ando 2015;Pitik et al 2021), it is sufficient for the purposes of this study. More details on the neutrino flux predicted by this model will be presented elsewhere (Pitik et al 2021).…”

Section: Below)mentioning

confidence: 99%

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A marginally fast-cooling proton-synchrotron model for prompt GRBs

Florou,

Petropoulou,

Mastichiadis

2021

Preprint

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A small fraction of GRBs with available data down to soft X-rays (∼ 0.5 keV) have been shown to feature a spectral break in the low-energy part (∼1-10 keV) of their prompt emission spectrum. The overall spectral shape is consistent with optically thin synchrotron emission from a population of particles that have cooled on a timescale comparable to the dynamic time to energies that are still much higher than their rest mass energy (marginally fast cooling regime). We consider a hadronic scenario and investigate if the prompt emission of these GRBs can originate from relativistic protons that radiate synchrotron in the marginally fast cooling regime. Using semi-analytical methods, we derive the source parameters, such as magnetic field strength and proton luminosity, and calculate the high-energy neutrino emission expected in this scenario. We also investigate how the emission of secondary pairs produced by photopion interactions and γγ pair production affect the broadband photon spectrum. We support our findings with detailed numerical calculations. Strong modification of the photon spectrum below the break energy due to the synchrotron emission of secondary pairs is found, unless the bulk Lorentz factor is very large (Γ 10 3 ). Moreover, this scenario predicts unreasonably high Poynting luminosities because of the strong magnetic fields (10 6 −10 7 G) that are necessary for the incomplete proton cooling. Our results strongly disfavor marginally fast cooling protons as an explanation of the low-energy spectral break in the prompt GRB spectra.

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“…Neutrino emission from classical gamma-ray bursts (e.g., [32][33][34][35][36][37][38][39][40][41][42][43][44][45]) has already been strongly constrained by IceCube via a lack of time/directional coincidence with known GRBs [46,47]. There are a variety of alternative models that suggest neutrino emission within the > ∼ TeV range (e.g., [48][49][50][51][52][53][54]).…”

Section: Introductionmentioning

confidence: 99%

Peeking into the Origins of IceCube Neutrinos: I. Buried Transient TeV Miniburst Rates

Kistler,

Yuksel

2017

Preprint

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Any interpretation of the astrophysical neutrinos discovered by IceCube must accommodate a variety of multimessenger constraints. We address implications of these neutrinos being produced in transient sources, principally if buried within supernovae so that gamma rays are absorbed by the star. This would alleviate tension with the isotropic Fermi GeV background that > ∼ 10 TeV neutrinos rival in detected energy flux. We find that IceCube data constrain transient properties, implying buried GeV-TeV electromagnetic emission near or exceeding canonical SN explosion energies of ∼ 10 51 erg, indicative of an origin within superluminous SNe. TeV neutrino bursts with dozens of IceCube events -which would be of great use for understanding r-process nucleosynthesis and more -may be just around the corner if they are a primary component of the flux.

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Diffuse emission of high-energy neutrinos from gamma-ray burst fireballs

Cited by 33 publications

References 87 publications

Exploring the Properties of Choked Gamma-ray Bursts with IceCube’s High-energy Neutrinos

Exploring the Properties of Choked Gamma-ray Bursts with IceCube’s High-energy Neutrinos

A marginally fast-cooling proton-synchrotron model for prompt GRBs

Peeking into the Origins of IceCube Neutrinos: I. Buried Transient TeV Miniburst Rates

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