Neutrino Processes and Pair Formation in Massive Stars and Supernovae.

Fowler, William A.; Hoyle, F.

doi:10.1086/190103

Cited by 527 publications

(370 citation statements)

References 1 publication

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“…The resonant reaction rate for capture on a nucleus in an initial state i, N A < σv > res i for isolated narrow resonances is calculated as a sum over all relevant compound nucleus states f above the proton threshold [11] N A < σv > res i = 1.540 × 10 11 (µT 9 ) −3/2…”

Section: Results For the Reaction Ratementioning

confidence: 99%

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
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We present results for levels in 36 K (the mirror of nucleus 36 Ar) that are used in rp reaction rate calculations. The levels are also determined from the Isobaric Mass Multiplet Equation and the binding energies of the T=1 analog states as a check on the assignment of spins and parity. Where the analog states are not known the levels are calculated with two-body interactions that use the sd-shell interactions USDA and USDB as the charge-independent parts, with a Coulomb, chargedependent and charge-asymmetric Hamitonian added. The gamma-decay lifetimes and 35 Al to 36 K spectroscopic factors are calculated with the same interactions, and together with experimental information on the levels of excited states, are used to determine the 35 Ar(p,γ) 36 K reaction rates.

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Section: Results For the Reaction Ratementioning

confidence: 99%

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
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“…These processes have been studied since the beginning of the 1960s in a number of seminal papers (see, e.g., Pinaev 1963, Fowler and Hoyle 1964, Beaudet et al 1967, and references therein, as well as references in subsequent sections of this chapter). The early studies were conducted in the framework of an old, simplified Fermi theory of weak interactions and required revision in the 1970s after the Weinberg-Salam-Glashow theory was widely accepted.…”

Section: Neutrino Emission From Neutron Star Crusts 21 Main Neutrinomentioning

confidence: 99%

“…(c) Other photon processes In addition, there are other processes of neutrino generation considered in the literature, particularly, the processes proposed by Chiu and Morrison (1960) and discussed, for instance, by Fowler and Hoyle (1964), and Beaudet et al (1967):…”

Section: Other Electron-photon Neutrino Processesmentioning

confidence: 99%

Neutrino emission from neutron stars

Kaminker²,

et al. 2001

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We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.

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“…Fowler and Hoyle (1964) have discussed in detail the nuclear reactions occurring in subsequent evolution. * For pure hydrogen the limit is higher, (see Chandrasekhar (1939) …”

mentioning

confidence: 99%

Gravitational Collapse and Weak Interactions

Arnett¹

1966

Can. J. Phys.

163

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The behavior of a massive star during its final catastrophic stages of evolution has been investigated theoretically, with particular emphasis upon the effect of electron-type neutrino interactions. The methods of numerical hydrodynamics, with coupled energy transfer in the diffusion approximation, were used. In this respect, this investigation differs from the work of Colgate and White (1964) in which a "neutrino deposition" approximation procedure was used. Gravitational collapse initiated by electron capture and by thermal disintegration of nuclei in the stellar center is examined, and the subsequent behavior does not depend sensitively upon which process causes the collapse.As the density and temperature of the collapsing stellar core increase, the material becomes opaque to electron-type neutrinos and energy is transferred by these neutrinos to regions of the star less tightly bound by gravity. Ejection of the outer layers of the star can result. This phenomenon has been identified with supernovae.Uncertainty concerning the equation of state of a hot, dense nucleon gas causes uncertainty in the temperature of the collapsing matter. This affects the rate of energy transfer by electron-type neutrinos and the rate of energy lost to the star by muon-type neutrinos.The effects of general relativity do not appear to become important in the core until after the ejection of the outer layers.

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Neutrino Processes and Pair Formation in Massive Stars and Supernovae.

Cited by 527 publications

References 1 publication

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
View full text Add to dashboard Cite

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
View full text Add to dashboard Cite

Neutrino emission from neutron stars

Gravitational Collapse and Weak Interactions

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Neutrino Processes and Pair Formation in Massive Stars and Supernovae.

Cited by 527 publications

References 1 publication

Shell-model studies of therpreaction35Ar(p,γRichter1, Brown2 2012Phys. Rev. C171160View full textAdd to dashboardCite

Shell-model studies of therpreaction35Ar(p,γRichter1, Brown2 2012Phys. Rev. C171160View full textAdd to dashboardCite

Neutrino emission from neutron stars

Gravitational Collapse and Weak Interactions

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Resources

About

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
View full text Add to dashboard Cite

Shell-model studies of therpreaction35Ar(p,γ
Richter
¹
,
Brown
²

2012
Phys. Rev. C
17
1
16
0
View full text Add to dashboard Cite