Astrophysical factors: Zero energy vs most effective energy

Liolios, Theodore E.

doi:10.1103/physrevc.64.018801

Cited by 7 publications

(15 citation statements)

References 17 publications

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“…Compared with T 9 -axis from the relation (2) the change of the T 9 scale is clearly observed at about the low energy resonance. The last example is the reaction 2 H(d, n) 3 He, which is non-resonant, but the S-factor of this reaction has slow energy dependence in the energy region above 50 keV, as is shown in Fig. 5.…”

Section: Fig 2: (Color Online)mentioning

confidence: 95%

“…This definition of the width is different from the one chosen in [4,5], but it shows clearly that the width is consistent with the Gamow window if the S-factor does not depend on the incident energy. We evaluate this condition numerically by using the S-factors determined experimentally for three selected resonant reactions: 11 B(p, α) 8 Be, 10 B(p, α) 7 Be and 3 H(d, n) 4 He, besides a non-resonant reaction 2 H(d, n) 3 He. All four reactions are of importance in the application of the laserinduced nuclear reactions.…”

Section: Arxiv:13052105v1 [Nucl-th] 9 May 2013mentioning

confidence: 99%

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Gamow peak approximation near strong resonances

Kimura

Bonasera

2013

Phys. Rev. C

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We discuss the most effective energy range for charged particle induced reactions in a plasma environment at a given plasma temperature. The correspondence between the plasma temperature and the most effective energy should be modified from the one given by the Gamow peak energy, in the presence of a significant incident-energy dependence in the astrophysical S-factor as in the case of resonant reactions. The suggested modification of the effective energy range is important not only in thermonuclear reactions at high temperature in the stellar environment, e.g., in advanced burning stages of massive stars and in explosive stellar environment, as it has been already claimed, but also in the application of the nuclear reactions driven by ultra-intense laser pulse irradiations

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Section: Fig 2: (Color Online)mentioning

confidence: 95%

Section: Arxiv:13052105v1 [Nucl-th] 9 May 2013mentioning

confidence: 99%

Gamow peak approximation near strong resonances

Kimura

Bonasera

2013

Phys. Rev. C

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“…Recently these issues were discussed by Liolios et al (2000Liolios et al ( , 2001, Kravchuk et al (2014), andLiu (2013). However, they neglected the effects of SES on thermonuclear reaction rate in superstrong magnetic field (SMF).…”

Section: Introductionmentioning

confidence: 99%

Resonant nuclear reaction ²³ Mg (p, γ ) ²⁴ Al in strongly screening magnetized neutron star crust

Liu¹,

Li²

2017

Chinese Phys. C

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Based on the relativistic theory of superstrong magnetic field (SMF), by using three models of Lai (LD), Fushiki (FGP), and ours (LJ), we investigate the influence of SMFs due to strong electron screening (SES) on the nuclear reaction 23 Mg (p, γ) 24 Al in magnetars. At relatively low density environment (e.g., ρ 7 < 0.01) and 1 < B 12 < 10 2 , our screening rates are in good agreement with those of LD and FGP. However, in relatively high magnetic fields (e.g., B 12 > 10 2 ), our reaction rates can be 1.58 times and about three orders of magnitude larger than those of FGP and LD, respectively (B 12 , ρ 7 are in units of 10 12 G, 10The significant increase of strongly screening rates can imply that more 23 Mg will escape from the Ne-Na cycle due to SES in a SMF. As a consequence, the next reaction 24 Al (β + , ν) 24 Mg will produce more 24 Mg to participate in the Mg-Al cycle. Thus, it may lead to synthesize a large amount of production of A > 20 nuclides in magnetars, respectively.

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“…The enhancing influence of stellar plasmas on astrophysical thermonuclear reactions (and on the respective thermonuclear reaction rates) has been studied by many authors (see for example Refs. [11][12][13][14][15][16][17][18][19], and references therein) who derive corrective factors (known as Screening Enhancement Factors:SEFs) by which the reaction rates are multiplied in order to take into account screening effects.…”

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confidence: 99%

“…Actually these models are frequently used in solar evolution codes giving quantitative estimates of the neutrino flux uncertainties associated with the screening effect(see for example Refs. [11][12][13][14][15][16][17][18][19] and references therein). Others studies [23] have dealt with strongly degenerate regimes where screening effects are extremely important.…”

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confidence: 99%

Screened thermonuclear reactions and predictive stellar evolution of detached double-lined eclipsing binaries

Liolios

Kosmas

2005

Phys. Rev. C

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The low energy fusion cross sections of charged-particle nuclear reactions (and the respective reaction rates) in stellar plasmas are enhanced due to plasma screening effects. We study the impact of those effects on predictive stellar evolution simulations for detached double-lined eclipsing binaries. We follow the evolution of binary systems (pre-main sequence or main sequence stars) with precisely determined radii and masses from 1.1M ⊙ to 23M ⊙ (from their birth until their present state). The results indicate that all the discrepancies between the screened and unscreened models (in terms of luminosity, stellar radius, and effective temperature) are within the observational uncertainties. Moreover, no nucleosynthetic or compositional variation was found due to screening corrections. Therefore all thermonuclear screening effects on the charged-particle nuclear reactions that occur in the binary stars considered in this work (from their birth until their present state) can be totally disregarded. In other words, all relevant charged-particle nuclear reactions can be safely assumed to take place in a vacuum, thus simplifying and accelerating the simulation processes. PACS number(s):

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Astrophysical factors: Zero energy vs most effective energy

Cited by 7 publications

References 17 publications

Gamow peak approximation near strong resonances

Gamow peak approximation near strong resonances

Resonant nuclear reaction ²³ Mg (p, γ ) ²⁴ Al in strongly screening magnetized neutron star crust

Screened thermonuclear reactions and predictive stellar evolution of detached double-lined eclipsing binaries

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Astrophysical factors: Zero energy vs most effective energy

Cited by 7 publications

References 17 publications

Gamow peak approximation near strong resonances

Gamow peak approximation near strong resonances

Resonant nuclear reaction 23 Mg (p, γ ) 24 Al in strongly screening magnetized neutron star crust

Screened thermonuclear reactions and predictive stellar evolution of detached double-lined eclipsing binaries

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Resonant nuclear reaction ²³ Mg (p, γ ) ²⁴ Al in strongly screening magnetized neutron star crust