S-matrix calculation of the triple-alpha reaction

Fushiki, Ikko; Lamb, D. Q.

doi:10.1086/165284

Cited by 50 publications

(38 citation statements)

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“…Helium burning at such conditions is possible in accretion on white dwarfs and neutron stars. The non-resonance reaction was considered in a number of papers [11,12,13,14] based on the model assumptions; however, a consistent treatment of the three-body dynamics is lacking. In this respect, note that at ultra-low energies any approximation can lead to an error of a few orders of magnitude in the calculated reaction rate.…”

Section: Introductionmentioning

confidence: 99%

3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
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Section: Introductionmentioning

confidence: 99%

3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
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show abstract

“…(1.4)] and a screening factor (see e.g. Salpeter & van Horn 1969, Itoh, Totsuji, & Ichimaru 1977, Hansen, Torrie, & Veillefosse 1977, Alastuey & Jancovici 1978, Itoh et al 1979, Ichimaru, Tanaka, Iyetomi 1984, Ichimaru & Utsumi 1983, Fushiki & Lamb 1987, Itoh et al 1990, Schramm & Koonin 1990, Ichimaru 1993, Chabrier & Schatzman 1994, Kitamura & Ichimaru 1995, Brown & Sawyer 1997 < j, k > * = f scr (Z j , Z k , ρ, T, Y i ) < j, k > .…”

Section: Thermonuclear Reaction Ratesmentioning

confidence: 99%

“…In the extreme case of very low temperatures, where reactions are only possible via ground state oscillations of the nuclei in a Coulomb lattice, Eq. (1.5) breaks down, because it was derived under the assumption of a Boltzmann distribution (for recent references see Fushiki & Lamb 1987, Itoh et al 1990, Schramm & Koonin 1990, Ichimaru 1993, Chabrier & Schatzman 1994, Ichimaru 1996.…”

Section: Thermonuclear Reaction Ratesmentioning

confidence: 99%

Nucleosynthesis basics and applications to supernovae

Thielemann¹,

Rauscher²,

Freiburghaus³

et al. 1998

Nuclear and Particle Astrophysics

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This review concentrates on nucleosynthesis processes in general and their applications to massive stars and supernovae. A brief initial introduction is given to the physics in astrophysical plasmas which governs composition changes. We present the basic equations for thermonuclear reaction rates and nuclear reaction networks. The required nuclear physics input for reaction rates is discussed, i.e. cross sections for nuclear reactions, photodisintegrations, electron and positron captures, neutrino captures, inelastic neutrino scattering, and beta-decay half-lives. We examine especially the present state of uncertainties in predicting thermonuclear reaction rates, while the status of experiments is discussed by others in this volume (see M. Wiescher). It follows a brief review of hydrostatic burning stages in stellar evolution before discussing the fate of massive stars, i.e. the nucleosynthesis in type II supernova explosions (SNe II). Except for SNe Ia, which are explained by exploding white dwarfs in binary stellar systems (which will not be discussed here), all other supernova types seem to be linked to the gravitational collapse of massive stars (M>8M ) at the end of their hydrostatic evolution. SN1987A, the first type II supernova for which the progenitor star was known, is used as an example for nucleosynthesis calculations. Finally, we discuss the production of heavy elements in the r-process up to Th and U and its possible connection to supernovae.

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“…The first discussion of this process was given by Cameron (1959) and was later elaborated by Wolf (1965), Salpeter and Van Horn (1969), Schramm and Koonin (1990) and Ogata et al (1991), in the case of one component plasma. The case of binary ionic mixtures has been recently treated by Ichimaru et al (1992), while the case of the 3a process has been treated by Salpeter and Van Horn (1969), Fushiki and Lamb (1987), Schramm et al (1992) and Langanke and Miiller 1993).…”

Section: Pycnonuclear Reactionsmentioning

confidence: 99%

“…The 3a reaction in the pycnonuclear regime was considered for the first time by Cameron (1959) and later on by Salpeter and Van Horn (1969), Fushiki and Lamb (1987) and Schramm et al (1992). Besides the problem of its three-body nature, the pycnonuclear 3a reaction is characterized by the fact that temperatures are too low to allow the resonance of 8 Be and by the fact that in the region of interest helium is a quantum fluid rather than a Coulomb lattice.…”

Section: The 3a Fusion Ratementioning

confidence: 99%

Astrophysical consequences of the screening of nuclear reactions

Isern

Hernanz

1994

International Astronomical Union Colloquium

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A b s t r a c tThe rate of nuclear reactions depends on the influence of the surrounding particles that compose the plasma. At high densities the situation is far from being satisfactory and the influence of electron polarization has not been completely elucidated. In particular, it is shown that the possibility of an accretion induced collapse of a carbon-oxygen white dwarf instead of a supernova explosion completely depends on the screening factors and pycnonuclear rates that are adopted. Similarly, the possibility of detecting isolated neutron stars that accrete matter from the interstellar medium depends on the adopted pycnonuclear rates. Low rates allow the formation of a metastable layer that can release energy explosively and produce a7-ray burst. Nevertheless, current rates seem to prevent such a situation.Le taux des reactions nucleaires depend de l'influence exercee par les particules voisines qui composent le plasma. A haute densite, la situation est loin d'etre satisfaisante et l'influence de la polarization electronique n'est pas sufisamment claire. En particulier, on montre que la possibilite d'obtenir un collapse non explosif d'une naine blanche de carbone oxygene depend des facteurs d'ecrantage et des taux pycnonucleaires adoptes. Egalement, la possibilite de detecter des etoiles a neutrons isoiees depend des taux pycnonucleaires adoptes. Des petites valeurs favorisent la formation d'une couche metastable qui peut liberer de l'energie explosivement et produire 106 at https://www.cambridge.org/core/terms. https://doi

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S-matrix calculation of the triple-alpha reaction

Cited by 50 publications

References 0 publications

3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
View full text Add to dashboard Cite

3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
View full text Add to dashboard Cite

Nucleosynthesis basics and applications to supernovae

Astrophysical consequences of the screening of nuclear reactions

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S-matrix calculation of the triple-alpha reaction

Cited by 50 publications

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3α-cluster structure of the0+states inC12Fedotov1, Kartavtsev2, Kochkin3 et al. 2004Phys. Rev. C313500View full textAdd to dashboardCite

3α-cluster structure of the0+states inC12Fedotov1, Kartavtsev2, Kochkin3 et al. 2004Phys. Rev. C313500View full textAdd to dashboardCite

Nucleosynthesis basics and applications to supernovae

Astrophysical consequences of the screening of nuclear reactions

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3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
View full text Add to dashboard Cite

3α-cluster structure of the0+states inC12
Fedotov
¹
,
Kartavtsev
²
,
Kochkin
³

et al. 2004
Phys. Rev. C
31
3
50
0
View full text Add to dashboard Cite