New Results for р14N Capture to the 3/2+ Level of the 15O Nucleus at 6.79 MeV

Dubovichenko, S. B.; Burkova, N. А.

doi:10.1007/s11182-018-1469-4

Cited by 4 publications

(5 citation statements)

References 24 publications

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“…If the total reaction cross sections or astrophysical S-factor of the radiative capture process are known, the rate of this reaction, which is used for astrophysical applications, can be determined as Ref. 31 4 1/ 2 3/ 2 9 9 0 3.7313 10 ( ) exp( 11.605 / )…”

Section: Calculation Methodsmentioning

confidence: 99%

“…Previously we considered it in Ref. 4. Also we give a method for calculating total cross sections for states mixed by the spin of channel S.…”

Section: Astrophysical S-factor For Capture To the 4 Th Esmentioning

confidence: 99%

“…7 from Table 2. The E1 transitions from all 4 Р scattering waves with zero depth potentials were considered -results are presented in Fig. 2a with a red dashed curve.…”

Section: Astrophysical S-factor For Capture To the 4 Th Esmentioning

confidence: 99%

“…In addition, one can consider M1 transitions between P waves of continuous spectrum and the 2+4 P 1/2 GS of nucleus. 4…”

Section: Transitions At the Capture To The Gsmentioning

confidence: 99%

“…Furthermore, we consider р 14 N  15 О capture reaction to all other excited states (ES) of 15 O. It is shown that experimental data for the astrophysical S-factor for capture to all excited states can be described only under assumption that all five considered resonances at energies from 260 keV to 3.2 MeV are in 4 , determine mixed with possible spin values of channel S 1 and S 2 state with a given total J and orbital L moments.…”

Section: Introductionmentioning

confidence: 99%

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Reaction rate of p14N →15Oγ capture to all bound states in potential cluster model

Dubovichenko

Burkova

Dzhazairov-Kakhramanov

et al. 2020

Int. J. Mod. Phys. E

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Review of calculation results for astrophysical S-factor of the 14 N(р,  15 О capture reaction in the p 14 N channel of 15 O was presented. It was carried out in the frame of the modified potential cluster model, taking into account resonances in the 15 O spectrum up to 3.2 MeV at energy of incident protons varying from 30 keV to 5 MeV. It is possible to describe experimental data for the astrophysical Sfactors of the radiative proton capture on 14 N to five excited states of 15 O at excitation energies from 5.18 MeV to 6.86 MeV, only under assumption, that all five resonances are D scattering waves. Quality new physical interpretation of the capture mechanism is discussed in this channel to the ground state of 15 O. Carried out by us assumption that the ground state of 15 O is determined by the p 14 N * channel with excited 14 N * cluster, immediately allowed us to correctly describe order of values of the experimental S-factor for capture to this state. Taking into account these results, the total S-factor of the proton capture on 14 N and the reaction rates to the ground and five excited states of 15 O were determined at temperatures from 0.01 to 10 T 9 . The parametrization of the total reaction rate with a simple form is performed, which allows to obtain  2 equal to 0.06 with 5% errors of the calculated rate.1. With an excitation energy of 5.183(1) MeV above BS or -2.1141 MeV in c.m. Ref. 26 relative to threshold of the р 14 N channel, there is a first excited, but bound in this channel, state with the moment J  = 1/2 + , which can be matched to the doublet 2 S 1/2 wave with FS. Although such state can, of course, be considered as a quartet 4 D 1/2 wave with FS.2. The second ES (2 nd ES) with an excitation energy of 5.2409(3) MeV Ref. 26 relative to the GS or -2.0562 MeV relative to the threshold of the р 14 N channel has J  = 5/2 + and it can be matched to the mixture of doublet and quartet 2+4 D 5/2 waves with FS.3. The third excited state (3 rd ES) at an excitation energy of 6.1763(17) MeV Ref. 26 relative to the GS or -1.1208 MeV relative to channel threshold has J  = 3/2and it can be compared to a mixture of doublet and quartet 2+4 Р 3/2 -waves without an associated FS.4. The fourth excited state (4 th ES) has an excitation energy of 6.7931(17) MeV relative to the GS or -0.504 MeV Ref. 26 or relative to the channel threshold has J  = 3/2 + and it can be compared with the quartet 4 S 3/2 wave with the FS. Of course, this state may also be a mixture of doublet and quartet 2+4 D 3/2 waves with the FS.5. The fifth excited state (5 th ES) with an excitation energy of 6.8594(9) MeV Ref. 26 relative to the GS or -0.4377 MeV relative to the channel threshold has J  = 5/2 + and it can also be compared to a mixture of doublet and quartet 2+4 D 5/2 wave with the FS 6. There is another bound state in the р 14 N channel with J  = 7/2 + at an excitation energy of 7.2759(6) MeV Ref. 26 relative to the GS or -0.0212 MeV relative to the threshold of the considered channel, which can be compared to the 4 D 7/2 s...

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Section: Calculation Methodsmentioning

confidence: 99%

“…Previously we considered it in Ref. 4. Also we give a method for calculating total cross sections for states mixed by the spin of channel S.…”

Section: Astrophysical S-factor For Capture To the 4 Th Esmentioning

confidence: 99%

“…7 from Table 2. The E1 transitions from all 4 Р scattering waves with zero depth potentials were considered -results are presented in Fig. 2a with a red dashed curve.…”

Section: Astrophysical S-factor For Capture To the 4 Th Esmentioning

confidence: 99%

“…In addition, one can consider M1 transitions between P waves of continuous spectrum and the 2+4 P 1/2 GS of nucleus. 4…”

Section: Transitions At the Capture To The Gsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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