Neutrino emission by the pair, plasma, and photo processes in the Weinberg-Salam model

Schinder, P. J.; Schramm, David N.; Wiita, Paul J.; Margolis, S. H.; Tubbs, D. L.

doi:10.1086/164993

Cited by 87 publications

(78 citation statements)

References 14 publications

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“…To check whether neutrino X p 0.1 C cooling is energetically important, we follow the thermal evolution in our one-zone model. With the neutrino cooling rates of Schinder et al (1987), we find that the neutrino cooling timescale at the peak of the burst, , is ≈ s. In-4 t p C T/e 2 # 10 n V n tegrating over the cooling tail, we find that 20% of the burst energy is emitted as neutrinos. This can be regarded as an upper limit as the exponential burst timescale of our simulation is somewhat longer (4 hr) than typical.…”

Section: Model and Initial Conditionsmentioning

confidence: 83%

“…For C V the electron contribution to , we use a modified version of C V the fit of Paczyński (1983), and for the ions include Coulomb corrections according to Potekhin & Chabrier (2000) using the linear mixing rule to sum over ion species (Chabrier & Potekhin 1998). Our code includes energy losses e cool due to neutrino emission (Schinder et al 1987) and a rough estimate of radiative cooling following Bildsten (1998). However, we find that the rise in temperature is so rapid that all cooling processes are negligible and have no impact on the peak temperature or the nuclear reactions powering the burst rise.…”

Section: Model and Initial Conditionsmentioning

confidence: 99%

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Photodisintegration-triggered Nuclear Energy Release in Superbursts

Schatz

Bildsten

Cumming

2003

The Astrophysical Journal

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Superbursts from accreting neutron stars present a unique opportunity to probe nuclear processes at densities g cm Ϫ3 and temperatures . Cumming & Bildsten showed that these 10 42 erg bursts are most 9 9r ≈ 10 T 1 10 K likely triggered by unstable ignition of a small amount of carbon in a sea of heavy nuclei made during prior rpprocess burning of hydrogen and helium. We show here that the high temperatures reached during superbursts lead to photodisintegration reactions, which trigger conversion of these heavy nuclei into iron group elements. The neutron richness of the heavy nuclei allow (g, n) reactions to trigger the photodisintegration runaway. Because the heavy elements are initially far from the minimum in binding energy, the nuclear energy release in this process can easily dominate that from the fusion of carbon. To our knowledge, this is the only cosmic phenomenon where the destruction of heavy nuclei into lighter nuclei represents the main source of energy.

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Section: Model and Initial Conditionsmentioning

confidence: 83%

Section: Model and Initial Conditionsmentioning

confidence: 99%

Photodisintegration-triggered Nuclear Energy Release in Superbursts

Schatz

Bildsten

Cumming

2003

The Astrophysical Journal

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“…Observations have determined that the ejecta of a typical SNIa are, by mass, 18% oxygen, 15% silicon, 13% iron, and 49% nickel (almost all in the unstable form 56 Ni which decays radioactively to 56 Fe), along with smaller amounts of carbon, calcium, sulphur and magnesium [37]. Elements emerge from SNIa in strata, with the lightest occupying the outermost layers.…”

Section: Abundancementioning

confidence: 99%

“…Special attention will be drawn here to the 4s electrons of iron as targets for mutually annihilating electron neutrinos and antineutrinos belonging to a dark matter halo. Stellar nucleosynthesis remains exothermic up until nickel but 56 Ni radioactively decays via 56 Co to 56 Fe, the most stable of all nuclides. Thus, iron is already and will continue to be an abundant element.…”

Section: Introductionmentioning

confidence: 99%

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

Spivey¹

2013

JMP

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The potential cosmological and astrobiological implications of neutrinos are considered. Dark energy drives the current phase of accelerating cosmic expansion. Like inflation, it may decay in time to matter and radiation. However, since its energy density is minuscule in comparison, decay would be unlikely to inject such a rich variety of particles into the universe, and may instead be limited to the lowest energy fermions. Nonrelativistic neutrinos have the capacity to form stable, galaxy-engulfing haloes supported by degeneracy pressure, much like white dwarves and neutron stars. Conversely, bodies of mass 100M   can indefinitely rely on Coulomb forces for weight support. Opportunities for the mutual annihilation of electron neutrinos are largely confined to planets containing iron in the hcp phase. If dark energy decays primarily to neutrinos in 40 ~ 100 Gyr, then oceanic planets orbiting within the resulting haloes could provide long-term habitats for aquatic life with only lax constraints on the neutrino mass, 6 1 4 0m m  e V   . Various considerations now favour the possibility that neutrinos are Majorana particles with an inverted mass hierarchy and an electron neutrino mass in the vicinity of 50 meV. Sterile neutrinos of eV-mass may already be a significant component of dark matter, and could enhance planetary heating when active neutrino haloes become heavily depleted. An intriguing mechanism capable of regulating oceanic heat flux over a wide range of planetary masses is also described.

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“…The neutrino cooling is computed using the interpolation formulas given in [16,17,18]. The photo-disintegration of nuclei is included via modifying EOS as in [19].…”

Section: Simulation Setupmentioning

confidence: 99%

Central engines of Gamma Ray Bursts. Magnetic mechanism in the collapsar model.

Barkov¹,

Komissarov²

2008

AIP Conference Proceedings

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Abstract. In this study we explore the magnetic mechanism of hypernovae and relativistic jets of long duration gamma ray bursts within the collapsar scenario. This is an extension of our earlier work [1]. We track the collapse of massive rotating stars onto a rotating central black hole using axisymmetric general relativistic magnetohydrodynamic code that utilizes a realistic equation of state and takes into account the cooling associated with emission of neutrinos and the energy losses due to dissociation of nuclei. The neutrino heating is not included. We describe solutions with different black hole rotation, mass accretion rate, and strength of progenitor's magnetic field. Some of them exhibits strong explosions driven by Poyntingdominated jets with power up to 12 × 10 51 erg s −1 . These jets originate from the black hole and powered via the BlandfordZnajek mechanism. A provisional criterion for explosion is derived. A number of simulation movies can be downloaded from

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Neutrino emission by the pair, plasma, and photo processes in the Weinberg-Salam model

Cited by 87 publications

References 14 publications

Photodisintegration-triggered Nuclear Energy Release in Superbursts

Photodisintegration-triggered Nuclear Energy Release in Superbursts

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

Central engines of Gamma Ray Bursts. Magnetic mechanism in the collapsar model.

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