IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

Fang, Ke; Kotera, Kumiko; Murase, Kohta; Olinto, Angela V.

doi:10.1088/1475-7516/2016/04/010

Cited by 26 publications

(21 citation statements)

References 117 publications

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“…This is because for UHECRs crossing the supernova ejecta surrounding neutron stars, the effective optical depth to hadronic interactions is larger than unity, and so even in the most pessimistic case we expect fluxes of neutrinos in the energy range 10 8 E ν /GeV 10 9 [100]. Indeed, upper limits on the diffuse neutrino flux from IceCube [101,102] and the Pierre Auger Observatory [103] already constrain models of UHECR acceleration in the core of starburst galaxies [104,105]. Note, however, that if highenergy cosmic rays are re-accelerated to ultrahigh energies at the terminal shock of the starburst superwind, we expect the neutrino emission from starbursts to cutoff somewhat above 10 7 GeV, as entertained in [106].…”

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confidence: 99%

Acceleration of ultrahigh-energy cosmic rays in starburst superwinds

Anchordoqui

2018

Phys. Rev. D

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The sources of ultrahigh-energy cosmic rays (UHECRs) have been stubbornly elusive. However, the latest report of the Pierre Auger Observatory provides a compelling indication for a possible correlation between the arrival directions of UHECRs and nearby starburst galaxies. We argue that if starbursts are sources of UHECRs, then particle acceleration in the large-scale terminal shock of the superwind that flows from the starburst engine represents the best known concept model in the market. We investigate new constraints on the model and readjust free parameters accordingly. We show that UHECR acceleration above about 10 11 GeV remains consistent with observation. We also show that the model could accommodate hard source spectra as required by Auger data. We demonstrate how neutrino emission can be used as a discriminator among acceleration models.

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confidence: 99%

Acceleration of ultrahigh-energy cosmic rays in starburst superwinds

Anchordoqui

2018

Phys. Rev. D

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“…Furthermore, we assume that 0.2 of the energy of a given UHECR can be converted to the energy of a pion, and 0.25 of the pion energy then goes into the neutrino (as was done in Fang et al 2016). This provides us with an overall conversion factor ofñ f 0.05 from a given UHECR to a neutrino.…”

Section: Constraints From High-energy Neutrinosmentioning

confidence: 99%

“…Thus, for the same reason that we are able to efficiently produce UHECRs, we are also able to not overproduce high-energy neutrinos. We note that there may also be photo-hadronic interactions within the nebula that may also produce neutrinos (Lemoine et al 2015;Fang et al 2016). Since this process is stronger for protons than heavy nuclei, and since our main focus here is on the heavy nuclei as UHECRs, we save such a calculation for future work where the spectra of UHECRs and the non-thermal radiation is computed in more detail.…”

Section: Constraints From High-energy Neutrinosmentioning

confidence: 99%

Ultrahigh-Energy Cosmic Rays From the “En Caul” Birth of Magnetars*

Piro

Kollmeier

2016

ApJ

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Rapidly spinning magnetars can potentially form through the accretion induced collapse of a white dwarf or by neutron star (NS) mergers if the equation of state of the nuclear density matter is such that two low-mass NSs can form a massive NS rather than a black hole. In either case, the newborn magnetar is an attractive site for the production of ultrahigh-energy cosmic rays (particles with individual energies exceeding 10 eV; 18 UHECRs). The short-period spin and strong magnetic field are able to accelerate particles up to appropriate energies, and the composition of material on and around the magnetar may naturally explain recent inferences of heavy elements in UHECRs. We explore whether the small amount of natal debris surrounding these magnetars allows UHECRs to escape easily. We also investigate the impact on the UHECRs of the unique environment around the magnetar, which consists of a bubble of relativistic particles and magnetic field within the debris. The rates and energetics of UHECRs are consistent with such an origin, even though the rates of events that produce rapidly spinning magnetars remain very uncertain. The low ejecta mass also helps the high-energy neutrino background associated with this scenario to be below current IceCube constraints over most of the magnetar parameter space. A unique prediction is that UHECRs may be generated in old stellar environments without strong star formation, in contrast to what would be expected for other UHECR scenarios, such as active galactic nuclei or long gamma-ray bursts.

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“…Furthermore, we assume that 0.2 of the energy of a given UHECR can be converted to the energy of a pion, and 0.25 of the pion energy then goes into the neutrino (as was done in Fang et al 2016). This gives an overall conversion factor of f ν ∼ 0.05 from a given UHECR to a neutrino.…”

Section: Intergalactic Propagationmentioning

confidence: 99%

Ultrahigh-Energy Cosmic Rays from the "En Caul" Birth of Magnetars

Piro,

Kollmeier

2016

Preprint

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Rapidly-spinning magnetars can potentially form by the accretion induced collapse of a white dwarf or by neutron star mergers if the equation of state of nuclear density matter is such that two low mass neutron stars can sometimes form a massive neutron star rather than a black hole. In either case, the newly born magnetar is an attractive site for producing ultrahigh-energy cosmic rays (particles with individual energies exceeding 10 18 eV; UHECRs). The short-period spin and strong magnetic field are able to accelerate particles up to the appropriate energies, and the composition of material on and around the magnetar may naturally explain recent inferences of heavy elements in UHECRs. We explore whether the small amount of natal debris surrounding these magnetars allows the UHECRs to easily escape. We also investigate the impact on the UHECRs of the unique environment around the magnetar, which consists of a bubble of relativistic particles and magnetic field within the debris. Rates and energetics of UHECRs are consistent with such an origin even though the rates of events that produce rapidly-spinning magnetars remain very uncertain. The low ejecta mass also helps limit the high-energy neutrino background associated with this scenario to be below current IceCube constraints over most of the magnetar parameter space. A unique prediction is that UHECRs may be generated in old stellar environments without strong star formation in contrast to what would be expected for other UHECR scenarios, such as active galactic nuclei or long gamma-ray bursts.

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IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

Cited by 26 publications

References 117 publications

Acceleration of ultrahigh-energy cosmic rays in starburst superwinds

Acceleration of ultrahigh-energy cosmic rays in starburst superwinds

Ultrahigh-Energy Cosmic Rays From the “En Caul” Birth of Magnetars*

Ultrahigh-Energy Cosmic Rays from the "En Caul" Birth of Magnetars

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