Measurement of the 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts /><mml:none /><mml:mn>12</mml:mn></mml:mmultiscripts><mml:mo>(</mml:mo><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts /><mml:none /><mml:mn>12</mml:mn></mml:mmultiscripts><mml:mo>,</mml:mo><mml:mi>p</mml:mi><mml:mo>)</mml:mo><mml:mmultiscripts><mml:mi>Na</mml:mi><mml:mprescripts /><mml:none /><mml:mn>23</mml:mn></mml:mm

Zickefoose, J.; Leva, A. Di; Strieder, F.; Gialanella, L.; Imbriani, G.; Cesare, N. De; Rolfs, C.; Schweitzer, J.S.; Spillane, T.; Straniero, O.; Terrasi, F.

doi:10.1103/physrevc.97.065806

Cited by 49 publications

(81 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…They are in good agreement with the data reported by Jiang et al [23] using similar techniques, and with the renormalized THM data [17]. In the intermediate energy range at E rel ¼ 3.8 MeV, a more prominent resonance is observed compared to previous measurements [19,20]. The bottom spectrum is the singles data without gamma-ray coincidence dominated by protons from the contaminating dð 12 C; pÞ 13 C reaction (locus labeled in blue).…”

supporting

confidence: 90%

“…This immediately suggests two techniques for determining the cross section of the 12 C þ 12 C fusion reaction, namely, (i) detection of evaporated charged particles (protons or α) and (ii) detection of gamma rays from excited states of 23 Na and 20 Ne. Both techniques have been extensively employed showing consistent results at higher energies but exhibiting inconsistencies at lower energies [18][19][20], suggesting that systematic effects are a significant limitation [21,22]. An approach, which provides a unique signature and which can circumvent these experimental limitations, is to detect evaporated charged particles and gamma rays in coincidence.…”

mentioning

confidence: 99%

“…Fusion event selection is demonstrated in Fig. 3 for E rel ¼ 3.77 MeV, where the deuterium contamination from dð 12 C; pÞ 13 C reactions [20] is entirely removed by selecting the γ-ray transition depopulating the first excited state in 20 Ne.…”

mentioning

confidence: 99%

See 2 more Smart Citations

Advances in the Direct Study of Carbon Burning in Massive Stars

Fruet¹,

Courtin²,

Heine³

et al. 2020

Phys. Rev. Lett.

View full text Add to dashboard Cite

The 12 C þ 12 C fusion reaction plays a critical role in the evolution of massive stars and also strongly impacts various explosive astrophysical scenarios. The presence of resonances in this reaction at energies around and below the Coulomb barrier makes it impossible to carry out a simple extrapolation down to the Gamow window-the energy regime relevant to carbon burning in massive stars. The 12 C þ 12 C system forms a unique laboratory for challenging the contemporary picture of deep sub-barrier fusion (possible sub-barrier hindrance) and its interplay with nuclear structure (sub-barrier resonances). Here, we show that direct measurements of the 12 C þ 12 C fusion cross section may be made into the Gamow window using an advanced particle-gamma coincidence technique. The sensitivity of this technique effectively removes ambiguities in existing measurements made with gamma ray or charged-particle detection alone. The present cross-section data span over 8 orders of magnitude and support the fusion-hindrance model at deep sub-barrier energies.

show abstract

supporting

confidence: 90%

mentioning

confidence: 99%

See 1 more Smart Citation

Advances in the Direct Study of Carbon Burning in Massive Stars

Fruet¹,

Courtin²,

Heine³

et al. 2020

Phys. Rev. Lett.

View full text Add to dashboard Cite

show abstract

“…The authors studied the two main channels: 12 C( 12 C, p) 23 Na and 12 C( 12 C, α) 20 Ne at Argonne National Laboratory using a Gammasphere array of 100 Compton-suppressed Ge spectrometers in coincidence with silicon detectors. The measurement was pushed down to 2.84 MeV and 2.96 MeV for the p and α channels, respectively; the results are in good agreement with other measurements using c Spillane et al (2007) and charged particle detection Zickefoose et al (2018), but with smaller uncertainties. Tumino et al (2018a) and Tumino et al (2018b) measured the cross-section of the 12 C( 12 C, p) 23 Na and 12 C( 12 C, α) 20 Ne reactions through the indirect THM.…”

Section: State-of-the-artsupporting

confidence: 86%

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

Ferraro

Ciani

Boeltzig

et al. 2021

Front. Astron. Space Sci.

View full text Add to dashboard Cite

The chemical evolution of the Universe and several phases of stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross-sections at the energies at which they take place in stellar environments. Direct cross-section measurements are mainly hampered by the very low counting rate and by cosmic background; nevertheless, they have become possible by combining the best experimental techniques with the cosmic silence of an underground laboratory. In the nineties, the LUNA (Laboratory for Underground Nuclear Astrophysics) collaboration opened the era of underground nuclear astrophysics, installing first a homemade 50 kV and, later on, a second 400 kV accelerator under the Gran Sasso mountain in Italy: in 25 years of experimental activity, important reactions responsible for hydrogen burning could have been studied down to the relevant energies thanks to the high current proton and helium beams provided by the machines. The interest in the next and warmer stages of star evolution (i.e., post-main sequence and helium and carbon burning) drove a new project based on an ion accelerator in the MV range called LUNA-MV, able to deliver proton, helium, and carbon beams. The present contribution is aimed to discuss the state of the art for some selected key processes of post-main sequence stellar phases: 12C(α,γ)16O and 12C+12C are fundamental for helium and carbon burning phases, and 13C(α,n)16O and 22Ne(α,n)25Mg are relevant to the synthesis of heavy elements in AGB stars. The perspectives opened by an underground MV facility will be highlighted.

show abstract

“…Therefore, the stellar reaction rates of 12 C+ 12 C rely on a number of extrapolations based on different model assumptions from reaction and structure theory. There are a number of different experimental techniques and methods [5][6][7][8][9][10][11] measuring the fusion cross sections of 12 C+ 12 C in the sub-Coulomb energy region. A summary of experimental data and fittings are given in Fig.…”

Section: Introductionmentioning

confidence: 99%

An Efficient Thick Target Method for Scanning Resonances of the ¹²C+¹²C Fusion at Stellar Energies

Fang

Bucher

Alongi

et al. 2020

Proceedings of the 15th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG15)

View full text Add to dashboard Cite

The 12 C+ 12 C fusion reaction at stellar energies, which is known as carbon burning in stars, plays an important role in stellar evolution. The astrophysically important energy range spans roughly from 1 MeV to 3 MeV. The complication of molecular resonances in 12 C+ 12 C fusion brings significant uncertainties into the study of astrophysics. It is extremely difficult to measure the cross sections of 12 C+ 12 C fusions at energies of astrophysical relevance due to low yields, therefore, new technique is urgently needed. An efficient thick target method has been developed and applied for the first time to scan resonances of 12 C+ 12 C fusion at low energies 3.0 MeV

show abstract

Measurement of the C12(C12,p)Na23

Cited by 49 publications

References 44 publications

Advances in the Direct Study of Carbon Burning in Massive Stars

Advances in the Direct Study of Carbon Burning in Massive Stars

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

An Efficient Thick Target Method for Scanning Resonances of the ¹²C+¹²C Fusion at Stellar Energies

Contact Info

Product

Resources

About

Measurement of the C12(C12,p)Na23

Cited by 49 publications

References 44 publications

Advances in the Direct Study of Carbon Burning in Massive Stars

Advances in the Direct Study of Carbon Burning in Massive Stars

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

An Efficient Thick Target Method for Scanning Resonances of the 12C+12C Fusion at Stellar Energies

Contact Info

Product

Resources

About

An Efficient Thick Target Method for Scanning Resonances of the ¹²C+¹²C Fusion at Stellar Energies