Solar fusion cross sections. II. The<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>p</mml:mi><mml:mi>p</mml:mi></mml:math>chain and CNO cycles

Adelberger, E. G.; Garcı́a, A.; Robertson, R. G. H.; Snover, K. A.; Balantekin, A. B.; Heeger, K. M.; Ramsey-Musolf, Michael J.; Bemmerer, D.; Junghans, A. R.; Bertulani, C. A.; Chen, Jiunn-Wei; Costantini, H.; Prati, P.; Couder, M.; Uberseder, E.; Wiescher, M.; Cyburt, Richard H.; Davids, B.; Freedman, S. J.; Gai, M.; Gazit, Doron; Gialanella, L.; Imbriani, G.; Greife, U.; Hass, M.; Haxton, W. C.; Itahashi, T.; Kubodera, K.; Langanke, K.; Leitner, D.; Leitner, M.; Vetter, Paul; Winslow, L. A.; Marcucci, L. E.; Motobayashi, T.; Mukhamedzhanov, A. M.; Tribble, R. E.; Nollett, Kenneth M.; Nunes, F. M.; Park, T.-S.; Parker, P. D.; Schiavilla, R.; Simpson, E. C.; Spitaleri, C.; Strieder, F.; Trautvetter, H. P.; Suemmerer, K.; Typel, S.

doi:10.1103/revmodphys.83.195

Cited by 667 publications

(760 citation statements)

References 381 publications

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“…The key reactions and source of each adopted rate can be found in Table 1. Note that we employ the 14 N(p, γ) 15 O reaction rate provided by Champagne (private communication) which is consistent with that given by Adelberger et al (2011) and the LUNA collaboration. Palmerini et al (2011) discuss the consequences of the new rate for low-mass stellar evolution, including extra mixing.…”

Section: Overview Of the Stellar Modelsmentioning

confidence: 99%

Diagnostics of stellar modelling from spectroscopy and photometry of globular clusters

Angelou

D’Orazi

Constantino

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We conduct a series of comparisons between spectroscopic and photometric observations of globular clusters and stellar models to examine their predictive power. Data from medium-to-high resolution spectroscopic surveys of lithium allow us to investigate first dredge-up and extra mixing in two clusters well separated in metallicity. Abundances at first dredge-up are satisfactorily reproduced but there is preliminary evidence to suggest that the models overestimate the luminosity at which the surface composition first changes in the lowest-metallicity system. Our models also begin extra mixing at luminosities that are too high, demonstrating a significant discrepancy with observations at low metallicity. We model the abundance changes during extra mixing as a thermohaline process and determine that the usual diffusive form of this mechanism cannot simultaneously reproduce both the carbon and lithium observations. Hubble Space Telescope photometry provides turnoff and bump magnitudes in a large number of globular clusters and offers the opportunity to better test stellar modelling as function of metallicity. We directly compare the predicted main-sequence turn-off and bump magnitudes as well as the distance-independent parameter ∆M V MSTO bump . We require 15 Gyr isochrones to match the main-sequence turn-off magnitude in some clusters and cannot match the bump in low-metallicity systems. Changes to the distance modulus, metallicity scale and bolometric corrections may impact on the direct comparisons but ∆M V MSTO bump , which is also underestimated from the models, can only be improved through changes to the input physics. Overshooting at the base of the convective envelope with an efficiency that is metallicity dependent is required to reproduce the empirically determined value of ∆M V MSTO bump .

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Section: Overview Of the Stellar Modelsmentioning

confidence: 99%

Diagnostics of stellar modelling from spectroscopy and photometry of globular clusters

Angelou

D’Orazi

Constantino

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Open circles display the cases of weak screening, ∆t min =0.3 kyr, ∆α MLT = −0.2, and NACRE rates plus the LUNA rate for the 14 N+p reaction, respectively. " Adelberger et al (2011) 14 N+p rate" + "increased α MLT " would provide TRGB magnitudes on average ∼ 0.25 − 0.30 mag fainter than the combination "∆t min =3 kyr" + "full screening" + "NACRE 14 N+p rate" + "decreased α MLT ", at the extreme ends of the magnitude-colour calibration.…”

Section: Theoretical Uncertainties On Trgb Distances: Stellar Modelsmentioning

confidence: 99%

“…Nuclear reaction rates are not strictly the same. GARSTEC models use the Solar Fusion II (SFII) rates (Adelberger et al 2011) for all H-burning reactions and NACRE for the 3-α reaction, the only relevant He-burning reaction in triggering He-core ignition. The basic set of H-burning reaction rates in BaSTI are from NACRE (Angulo et al 1999b) with the rate of 14 N(p, γ) 15 O updated to the recommended value from LUNA.…”

Section: Two Stellar Codes Same Physicsmentioning

confidence: 99%

The brightness of the red giant branch tip

Serenelli

Weiß

Cassisi

et al. 2017

A&A

106

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Context. The brightness of the tip of the Red Giant Branch is a useful reference quantity for several fields of astrophysics. An accurate theoretical prediction is needed for such purposes. Aims. We intend to provide a solid theoretical prediction for it, valid for a reference set of standard physical assumptions, and mostly independent of numerical details. Methods. We examine the dependence on physical assumptions and numerical details, for a wide range of metallicities and masses, and based on two different stellar evolution codes. We adjust differences between the codes to treat the physics as identical as possible. After we have succeeded in reproducing the tip brightness between the codes, we present a reference set of models based on the most up to date physical inputs, but neglecting microscopic diffusion, and convert theoretical luminosities to observed infrared colours suitable for observations of resolved populations of stars and include analytic fits to facilitate their use. Results. We find that consistent use of updated nuclear reactions, including an appropriate treatment of the electron screening effects, and careful time-stepping on the upper red giant branch are the most important aspects to bring initially discrepant theoretical values into agreement. Small, but visible differences remain unexplained for very low metallicities and mass values at and above 1.2 M ⊙ , corresponding to ages younger than 4 Gyr. The colour transformations introduce larger uncertainties than the differences between the two stellar evolution codes. Conclusions. We demonstrate that careful stellar modeling allows an accurate prediction for the luminosity of the Red Giant Branch tip. Differences to empirically determined brightnesses may result either from insufficient colour transformations or from deficits in the constitutional physics. We present the best-tested theoretical reference values to date.

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“…Many decades passed by until we fully understood that Bethe's model is responsible for energy generation in massive, hot stars, only. For example, in contrast to Bethe's model our Sun catalyzes α-particles by means of proton-induced fusion reactions, also known as the pp-chain [30].…”

Section: Nucleons Nuclear Structure and Politicsmentioning

confidence: 99%

Current Status of Nuclear Physics Research

Bertulani

Hussein

2015

Braz J Phys

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In this review we discuss the current status of research in nuclear physics which is being carried out in different centers in the World. For this purpose we supply a short account of the development in the area which evolved over the last 9 decades, since the discovery of the neutron. The evolution of the physics of the atomic nucleus went through many stages as more data become available. We briefly discuss models introduced to discern the physics behind the experimental discoveries, such as the shell model, the collective model, the statistical model, the interacting boson model, etc., some of these models may be seemingly in conflict with each other, but this was shown to be only apparent.The richness of the ideas and abundance of theoretical models attests to the important fact that the nucleus is a really singular system in the sense that it evolves from two-body bound states such as the deuteron, to few-body bound states, such as 4 He, 7 Li, 9 Be etc. and up the ladder to heavier bound nuclei containing up to more than 200 nucleons. Clearly statistical mechanics, usually employed in systems with very large number of particles, would seemingly not work for such finite systems as the nuclei, neither do other theories which are applicable to condensed matter. The richness of nuclear physics stems from these restrictions. New theories and models are presently being developed. Theories of the structure and reactions of neutron-rich and proton-rich nuclei, called exotic nuclei, halo nuclei, or Borromean nuclei, deal with the wealth of experimental data that became available in the last 35 years. Further, nuclear astrophysics and stellar and Big Bang nucleosynthesis have become a more mature subject. Due to limited space, this review only covers a few selected topics, mainly those with which the authors have worked on. Our aimed potential readers of this review are nuclear physicists and physicists in other areas, as well as graduate students interested in pursuing a career in nuclear physics.

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Solar fusion cross sections. II. Theppchain and CNO cycles

Cited by 667 publications

References 381 publications

Diagnostics of stellar modelling from spectroscopy and photometry of globular clusters

Diagnostics of stellar modelling from spectroscopy and photometry of globular clusters

The brightness of the red giant branch tip

Current Status of Nuclear Physics Research

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