Impact of the New Measurement of the <sup>12</sup>C + <sup>12</sup>C Fusion Cross Section on the Final Compactness of Massive Stars

Chieffi, A.; Roberti, Lorenzo; Limongi, Marco; Cognata, M. La; Lamia, L.; Palmerini, S.; Pizzone, R. G.; Spartà, R.; Туміно, А.

doi:10.3847/1538-4357/ac06ca

Cited by 23 publications

(20 citation statements)

References 27 publications

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“…Limongi and Chieffi [169] showed that there is a tight monotonic correlation between ξ 2.5 and m CO , which can be expressed as ξ 2.5 = 0.55 − 1.1m −1 CO , with m CO given in units of M [170]. This is in qualitative agreement with the simplified approach of Fryer et al [26], but different assumptions on carbon nuclear reaction rates might significantly affect the correlation (e.g., [171]).…”

Section: Compact Remnants and The Lower Mass Gapsupporting

confidence: 63%

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

2022

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On 11 February 2016, the LIGO and Virgo scientific collaborations announced the first direct detection of gravitational waves, a signal caught by the LIGO interferometers on 14 September 2015, and produced by the coalescence of two stellar-mass black holes. The discovery represented the beginning of an entirely new way to investigate the Universe. The latest gravitational-wave catalog by LIGO, Virgo and KAGRA brings the total number of gravitational-wave events to 90, and the count is expected to significantly increase in the next years, when additional ground-based and space-born interferometers will be operational. From the theoretical point of view, we have only fuzzy ideas about where the detected events came from, and the answers to most of the five Ws and How for the astrophysics of compact binary coalescences are still unknown. In this work, we review our current knowledge and uncertainties on the astrophysical processes behind merging compact-object binaries. Furthermore, we discuss the astrophysical lessons learned through the latest gravitational-wave detections, paying specific attention to the theoretical challenges coming from exceptional events (e.g., GW190521 and GW190814).

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Section: Compact Remnants and The Lower Mass Gapsupporting

confidence: 63%

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

2022

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“…Using solely the Hin reaction rates halves the lifetimes in comparison to the other models, due to the higher central temperature regime. Interestingly Chieffi et al (2021), using rates that are much higher than those of Caughlan & Fowler (1988) in the 0.1−1 GK range, find that C-burning occurs at lower densities (see Fig. 3 in Chieffi et al 2021).…”

Section: Stellar Modelsmentioning

confidence: 82%

“…Interestingly Chieffi et al (2021), using rates that are much higher than those of Caughlan & Fowler (1988) in the 0.1−1 GK range, find that C-burning occurs at lower densities (see Fig. 3 in Chieffi et al 2021). Indeed, since the nuclear rates are higher, a lower density is needed to reach the required amount of nuclear energy to counteract the contraction post He-b.…”

Section: Stellar Modelsmentioning

confidence: 88%

“…Arnett & Truran 1969;Lamb et al 1976;Weaver et al 1978;Sparks & Endal 1980;Arnett & Thielemann 1985) but, interestingly, it still remains a topic of lively research today. For instance, Gasques et al (2007), Pignatari et al (2013) discussed the impact of the 12 C + 12 C rates on the s-process occurring in C-burning regions; Sukhbold & Adams (2020) studied the impact of the core C-burning phase on the final fate of red supergiants; Fields et al (2018), in a very exhaustive study of the impact of nuclear uncertainties in models for pre-supernovae, identified, among the reactions having the largest impact on the pre-supernova structure, the reaction 12 C( 12 C,p) 23 Na; Chieffi et al (2021) have investigated the impact of new rates for the carbon fusion reaction in stellar models.…”

Section: Introductionmentioning

confidence: 99%

“…We also use simpler models, where we focus on the detailed abundances variations resulting from a very large nuclear reaction network (following more than 1400 isotopes). Compared to the recent work by Chieffi et al (2021), here we use different experimental data for the nuclear reaction rates that, as we shall see, lead to very different consequences.…”

Section: Introductionmentioning

confidence: 99%

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A new ¹²C + ¹²C nuclear reaction rate: Impact on stellar evolution

Monpribat

Martinet

Courtin

et al. 2022

A&A

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Context. By changing the internal composition of stars, nuclear reactions play a key role in their evolution and spur their contribution to the chemical evolution of galaxies. The STELLA collaboration recently carried out new direct measurements of the 12C + 12C fusion cross section – one of the key reactions occurring in C-burning regions in massive stars. Using a coincidence technique, accurate measurements were obtained for many different energies, with the lowest energy explored according to the Gamow window for massive stars. Aims. This work presents new 12C + 12C reaction rates in the form of numerical tables with associated uncertainty estimations, as well as analytical formulae that can be directly implemented into stellar evolution codes. We also describe the impact of these new rates on C-burning in stars. Methods. We determined reaction rates for two cross section extrapolation models: one based on the fusion-hindrance phenomenon and the other on fusion-hindrance plus a resonance. We then compared our results to prior data. Using the GENEC stellar evolution code, we study how these new rates impact the C-burning phases in two sets of stellar models for stars with 12 M⊙ and 25 M⊙ initial masses, which were chosen to be highly representative of the diversity of massive stars. Results. The effective temperatures of C-burning in both sets of stellar models are entirely covered by the sensitivity of the present experimental data and no extrapolation of the rates is required. Although the rates may differ by more than an order of magnitude for temperatures typical of C-burning, the impacts on the stellar structures during that phase remain modest. This is a consequence of the readjustment of the stellar structure to a change of nuclear reaction rate for reactions that are shown to be important for energy production. For the hindrance case, the C-burning phase is found to occur at central temperatures that are 10% higher than with the hindrance plus resonance rate. Its C-burning lifetime is reduced by a factor of two. This model, nevertheless, loses more entropy than the other one; thus, it enters into the degeneracy regime earlier, which will impact the last stages of the evolution at the pre-core collapse time. The hindrance model produces up to 60% more neon. The impact of the different rates on the s-process occurring during the C-burning phase is modest, affecting the final abundances of s-processed elements by at most 20% (cobalt).

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