High-Energy Neutrinos from Gamma-Ray-Faint Accretion-Powered Hypernebulae
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| Formato: | Preprint |
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2022
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| _version_ | 1866916077210959872 |
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| author | Sridhar, Navin Metzger, Brian D. Fang, Ke |
| author_facet | Sridhar, Navin Metzger, Brian D. Fang, Ke |
| contents | Hypernebulae are inflated by accretion-powered winds accompanying hyper-Eddington mass transfer from an evolved post-main sequence star onto a black hole or neutron star companion. The ions accelerated at the termination shock -- where the collimated fast disk winds/jet collide with the slower, wide-angled wind-fed shell -- can generate high-energy neutrinos via hadronic ($pp$) reactions, and photohadronic ($pγ$) interactions with the disk thermal and Comptonized nonthermal background photons. It has been suggested that some fast radio bursts (FRBs) may be powered by such short-lived jetted hyper-accreting engines. Although neutrino emission associated with the ms-duration bursts themselves is challenging to detect, the persistent radio counterparts of some FRB sources -- if associated with hypernebulae -- could contribute to the high energy neutrino diffuse background flux. If the hypernebula birth rate follows that of steller-merger transients and common envelope events, we find that their volume-integrated neutrino emission -- depending on the population-averaged mass-transfer rates -- could explain up to $\sim25\%$ of the high-energy diffuse neutrino flux observed by the IceCube Observatory and the Baikal-Gigaton Volume Detector (GVD) Telescope. The time-averaged neutrino spectrum from hypernebula -- depending on the population parameters -- can also reproduce the observed diffuse neutrino spectrum. The neutrino emission could in some cases furthermore extend to >100 PeV, detectable by future ultra-high-energy neutrino observatories. The large optical depth through the nebula to Breit-Wheeler ($γγ$) interaction attenuates the escape of GeV-PeV gamma-rays co-produced with the neutrinos, rendering these gamma-ray-faint neutrino sources, consistent with the \textit{Fermi} observations of the isotropic gamma-ray background. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2212_11236 |
| institution | arXiv |
| publishDate | 2022 |
| record_format | arxiv |
| spellingShingle | High-Energy Neutrinos from Gamma-Ray-Faint Accretion-Powered Hypernebulae Sridhar, Navin Metzger, Brian D. Fang, Ke High Energy Astrophysical Phenomena High Energy Physics - Experiment High Energy Physics - Phenomenology Plasma Physics Hypernebulae are inflated by accretion-powered winds accompanying hyper-Eddington mass transfer from an evolved post-main sequence star onto a black hole or neutron star companion. The ions accelerated at the termination shock -- where the collimated fast disk winds/jet collide with the slower, wide-angled wind-fed shell -- can generate high-energy neutrinos via hadronic ($pp$) reactions, and photohadronic ($pγ$) interactions with the disk thermal and Comptonized nonthermal background photons. It has been suggested that some fast radio bursts (FRBs) may be powered by such short-lived jetted hyper-accreting engines. Although neutrino emission associated with the ms-duration bursts themselves is challenging to detect, the persistent radio counterparts of some FRB sources -- if associated with hypernebulae -- could contribute to the high energy neutrino diffuse background flux. If the hypernebula birth rate follows that of steller-merger transients and common envelope events, we find that their volume-integrated neutrino emission -- depending on the population-averaged mass-transfer rates -- could explain up to $\sim25\%$ of the high-energy diffuse neutrino flux observed by the IceCube Observatory and the Baikal-Gigaton Volume Detector (GVD) Telescope. The time-averaged neutrino spectrum from hypernebula -- depending on the population parameters -- can also reproduce the observed diffuse neutrino spectrum. The neutrino emission could in some cases furthermore extend to >100 PeV, detectable by future ultra-high-energy neutrino observatories. The large optical depth through the nebula to Breit-Wheeler ($γγ$) interaction attenuates the escape of GeV-PeV gamma-rays co-produced with the neutrinos, rendering these gamma-ray-faint neutrino sources, consistent with the \textit{Fermi} observations of the isotropic gamma-ray background. |
| title | High-Energy Neutrinos from Gamma-Ray-Faint Accretion-Powered Hypernebulae |
| topic | High Energy Astrophysical Phenomena High Energy Physics - Experiment High Energy Physics - Phenomenology Plasma Physics |
| url | https://arxiv.org/abs/2212.11236 |