Nuclear Reaction Rates at High Densities

Salpeter, E. E.; Horn, H. M. van

doi:10.1086/149858

Cited by 316 publications

(343 citation statements)

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“…If T is small, then the integrand in Eq. (3) is strongly peaked at the energy E pk = (π 2 E R T 2 ) 1/3 , and the integral can be evaluated as (Salpeter & Van Horn 1969) …”

Section: Classical Theory and Modern Approximationsmentioning

confidence: 99%

Thermonuclear fusion in dense stars

Potekhin

Chabrier

2012

A&A

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We study the plasma correlation effects on nonresonant thermonuclear reactions of carbon and oxygen in the interiors of white dwarfs and liquid envelopes of neutron stars. We examine the effects of electron screening on thermodynamic enhancement of thermonuclear reactions in dense plasmas beyond the linear mixing rule. Using these improved enhancement factors, we calculate carbon and oxygen ignition curves in white dwarfs and neutron stars. The energy balance and ignition conditions in neutron star envelopes are evaluated, taking their detailed thermal structure into account. The result is compared to the simplified "one-zone model", which is routinely used in the literature. We also consider the effect of strong magnetic fields on the ignition curves in the ocean of magnetars.

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“…If T is small, then the integrand in Eq. (3) is strongly peaked at the energy E pk = (π 2 E R T 2 ) 1/3 , and the integral can be evaluated as (Salpeter & Van Horn 1969) …”

Section: Classical Theory and Modern Approximationsmentioning

confidence: 99%

Thermonuclear fusion in dense stars

Potekhin

Chabrier

2012

A&A

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“…The plasma effects were described by Salpeter and Van Horn [5] (also see [6,7,25,31,33] and references therein). They modify the interaction potential U (r) but mainly at sufficiently large r, typically larger than nuclear scales, whereas we discuss the nuclear physics effects which influence U (r) at smaller r. It is commonly thought that the plasma physics and nuclear physics effects are distinctly different and can be considered separately.…”

Section: Studying Uncertainties Of S(e)mentioning

confidence: 99%

“…Pycnonuclear reactions occur due to zero-point vibrations of atomic nuclei in a crystalline lattice. Their physics is described, for instance, by Salpeter and Van Horn [5] and applied in later work (e.g. [6,7,25,31] and references therein).…”

Section: Studying Uncertainties Of S(e)mentioning

confidence: 99%

“…2 demonstrate possible effects of dense matter. Nuclear reaction rates are proportional to the value of S(E) at a typical reaction energy E. In pycnonuclear reactions the energy E is rather low [5], so that the reaction rate is actually determined by S(0). It is reasonable to expect that the presence of free neutrons between the reacting nuclei broadens and/or lowers the maximum of U (r).…”

Section: Studying Uncertainties Of S(e)mentioning

confidence: 99%

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Large collection of astrophysicalSfactors and their compact representation

et al. 2012

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Numerous nuclear reactions in the crust of accreting neutron stars are strongly affected by dense plasma environment. Simulations of superbursts, deep crustal heating and other nuclear burning phenomena in neutron stars require astrophysical S-factors for these reactions (as a function of center-of-mass energy E of colliding nuclei). A large database of S-factors is created for about 5,000 non-resonant fusion reactions involving stable and unstable isotopes of Be, B, C, N, O, F, Ne, Na, Mg, and Si. It extends the previous database of about 1,000 reactions involving isotopes of C, O, Ne, and Mg. The calculations are performed using the São Paulo potential and the barrier penetration formalism. All calculated S-data are parameterized by an analytic model for S(E) proposed before [Phys. Rev. C 82, 044609 (2010)] and further elaborated here. For a given reaction, the present S(E)-model contains three parameters. These parameters are easily interpolated along reactions involving isotopes of the same elements with only seven input parameters, giving an ultracompact, accurate, simple, and uniform database. The S(E) approximation can also be used to estimate theoretical uncertainties of S(E) and nuclear reaction rates in dense matter, as illustrated for the case of the 34 Ne+ 34 Ne reaction in the inner crust of an accreting neutron star.

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“…He showed that the reaction rate is enhanced increasingly strongly by plasma screening at high densities. These calculations were subsequently improved by Salpeter and Van Horn (1969) and further refined by DeWitt, Graboske, and Cooper (1973). The statistical physics foundation for nuclear reactionrate calculations in dense plasmas was substantially clarified by Jancovici (1977) and Alastuey and Jancovici (1978).…”

Section: I4i C-ignitionmentioning

confidence: 99%

Equations of State in Stellar Structure and Evolution

Horn

1994

International Astronomical Union Colloquium

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In this paper I summarize some of the recent advances in studies of dense matter. Research on phase separation in the binary ionic mixtures (BIMs) that constitute the matter in white dwarfs has been motivated by the need to obtain accurate estimates for the ages of the faintest white dwarfs and thus of the disk of our Galaxy. Substantial age increases appear possible, but it is not yet clear whether such large increases occur in real white dwarfs. A second advance is the prediction, based on state-of-the-art physical calculations, that ionization of H at low temperatures and increasing densities may occur via a first-order "plasma phase transition" (PPT). Astrophysical consequences of this result are still being explored in an effort to test this prediction. Related to these equation-of-state calculations are calculations of the enhancement of nuclear reaction rates at high densities. New thermonuclear rates have been computed for C+C reactions in BIMs, although there is currently some controversy about results at the highest densities. New pycnonuclear reaction rates have also been calculated for BIMs, and it has been suggested that He-burning at T = 0 may occur through a first-order phase transition. Finally, calculations of the equation of state of matter in strong magnetic fields and of radiative opacities at high densities have undergone very recent and substantial improvements, which are just beginning to be utilized in astrophysical calculations.Dans cette revue, je resumme les travaux les plus recents dans l'etude

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Nuclear Reaction Rates at High Densities

Cited by 316 publications

References 0 publications

Thermonuclear fusion in dense stars

Thermonuclear fusion in dense stars

Large collection of astrophysicalSfactors and their compact representation

Equations of State in Stellar Structure and Evolution

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