Neutrino Capture Reactions on {}^{40}Ar

Neutrino Capture Reactions on Ar

Toshio Suzuki and Michio Honma Department of Physics and Graduate School of Integrated Basic Sciences, College of Humanities and Sciences, Nihon University Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550, Japan
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Center for Mathematical Sciences, University of Aizu, Aizu-Wakamatsu, Fukushima 965-8580, Japan

Gamow-Teller (GT) strength in Ar is studied by shell-model calculations with monopole-based universal intearction, which has tensor components of +-meson exchanges. Calculated GT strength is found to be consistent with the experimental data obtained by recent () reactions. Neutrino capture cross sections on Ar for solar neutrinos from B are found to be enhanced compared with previous calculations. The reaction cross sections for multipoles other than and are obtained by random-phase approximation (RPA). Their contributions become important for neutrino energies larger than 50 MeV.

25.30.Pt, 21.60.Cs, 27.40.+z

I Introduction

A liquid Argon detector has excellent potentialities to detect core-collapse supernova neutrinos. A liquid Argon TPC (time projection chamber), proposed by the ICARUS Collaborations ICA (), can provide three-dimensional imaging of ionizing events. Recently, ArgoNeut Collaboration reported the first measurements of inclusive muon neutrino charged-current differential cross sections on argon Arg (). Here, we are interested in charged-current reactions on Ar induced by solar and supernova neutrinos. Direct measurements of the charged-current reaction cross sections on Ar are accessible by using a liquid Argon TPC detector and a spallation neutron source for neutrinos Cav ().

Recently, Gamow-Teller (GT) strength distribution for Ar K was measured by using the () reaction up to an excitation energy of 8 MeV Bhat (). The measured GT distribution is found to be close to that obtained by -decays of the mirror nucleus Ti up to an excitation energy of 6 MeV Bhat98 (). The GT strength obtained by a shell-model calculation Orm () is smaller than the observed strength As the neutrino capture reaction cross section on Ar is sensitive to the magnitude and the distribution of the GT strength, it is a remarkable progress if we can improve shell-model calculations to reproduce the experimental GT strength.

As shell-model calculations of Ar involve both - and shells, cross-shell correlations play important roles in the structure of the low-lying states in Ar. The choice of the cross-shell interaction is important and it will affect the GT strength distribution considerably. Here, we adopt the monopole-based-universal interaction (VMU) VMU () for the - cross-shell part. The VMU has tensor components of +-meson exchanges. A proper inclusion of the tensor force is essential for a successful description of spin-dependent modes in nuclei. The use of VMU in the - cross shell part of the interaction proved to be successful in the description of Gamow-Teller transitions and magnetic moments in - shell nuclei Yuan ().

In the next section, we discuss GT strength in Ar obtained by shell-model calculations and compare with experimental data. In Sect. III, cross sections of Ar (, ) K reaction are obtained by a hybrid model; shell-model method is used for the GT and isobaric analog (IA) transitions while random phase approximation (RPA) is employed for other multipoles. Summary is given in Sect. IV.

Ii Gamow-Teller Strength in Ar with Monopole-based- Universal Interaction

Figure 1: (Color on line) Cumulative sum of the GT strength for Ar K up to excitation energies of K, , obtained by the shell model calculation with the use of SDPF-VMU-LS. The experimental dataBhat () are shown by shaded area. Calculated values in Ref. Orm () are also shown by dashed line.

We study charged-current neutrino-induced reaction on Ar, Ar (, ) K, for neutrino energy below 100 MeV. We adopt a hybrid model in which the Gamow-Teller (GT) transitions and isobaric-analog (IA) transitions are evaluated by shell-model calculations while contributions from other multipoles are treated by RPA.

We first discuss GT transitions in Ar. The sdpf-m Utsuno () and GXPF1J Honma () interactions are used for -shell and -shell, respectively, in the shell-model calculations. The monopole-based-universal interaction (VMU) VMU (), which has the tensor force of +-meson exchanges, is adopted for the - cross-shell part. The two-body spin-orbit interaction due to meson exchanges is also added to the cross-shell part of the interaction. This intercation will be referred as SDPF-VMU-LS. Configurations within 2 excitations, , are taken with a quenching factor of = =0.775 Orm () for the axial-vector coupling with =-1.263. Single-particle energies of -shell for O core are tuned to reproduce those of GXPF1J in Ca. No further tunings are made. The shell-model calculations are performed by using OXBASH OXB () and MSHELL64 Mizu () program codes. Calculated ground state of K is 4 consistent with the experiment. The energy of the first 1 state is also close to the experimental excitation energy. In case of WBT interaction WB (), for example, it is shifted to a higher energy region; excitation energy of the first 1 state is calculated to be 4.14 MeV.

Calculated cumulative sum of ,


where =, up to the excitation energy of K () are shown in Fig. 1 as well as experimental values obtained by recent (, ) reaction Bhat (). The experimental GT strength from the () reaction is consistent with that obtained by -decays from the mirror nucleus Ti Bhat98 () except that the relative strengths for the lowest two strong transitions are reversed.

The experimental cumulative sum of the GT strength is rather well described by SDPF-VMU-LS while the strength in Ref. Orm () is smaller than the observed strength as shown in Fig. 1. The GT strength of the first strong peak is larger than that of the second strong peak in the present calculation, in agreement with the case of the GT strength obtained by the () reaction. The GT strength almost saturates around =18 MeV and the sum of the GT strength amounts to be 7.21, which is equal to 12. The sum of the strength exhausts the Ikeda sum-rule value in the present configuration space.

Iii Neutrino Capture Reaction Cross Sections on Ar

Figure 2: (Color on line) Calculated reaction cross sections for Ar (, ) K. (a) Contributions from the GT and IA transitions obtained by the shell-model calculations with the use of SDPF-VMU-LS are shown. (b) Contributions from multipoles except for and are obtained by RPA calculations with the use of SGII SG (). Total cross sections including all the multipoles are also shown by solid line.
Hamiltonian GT IA GT+IA
SDPF-VMU-LS 11.95 2.10 14.05
SDPF-VMU 10.99 2.10 13.10
Ref. Orm () 7.70 3.80 11.50
Table 1: Calculated cross sections for Ar (, ) K induced by solar B neutrinos for SDPF-VMU-LS and SDPF-VMU. Cross sections folded over the B neutrino spectrum Wint () are given in unit of cm. Cross sections in Ref. Orm () are also given.

Neutrino-nucleus reaction cross sections are evaluated by using the multipole expansion of the weak hadronic currents,


for charge-exchange reactions (, ) and (), where and are vector and axial-vector currents, respectively.

The reaction cross sections induced by or are given as follows Walecka (),


where and are neutrino and lepton momenta, respectively, is the lepton energy, , , and .

cos with the Fermi coupling constant, is the Cabbibo angle, and the lepton is electron or positron for charge-exchange reactions. The Coulomb correction is taken into account by multiplying the Fermi function for charge-exchange reactions at low neutrino energires () while the correction by the effective momentum transfer approximation is used at higher energies. Lower value of the cross section obtained by the two methods is adopted at each Engel (). In Eq. (3), and are Coulomb, longitudinal, transverse electric and magnetic multipole operators for vector and axial-vector currents

Calculated cross sections for Ar (, ) K induced by GT and IA transitions are shown in Fig. 2(a). Cross sections for Ar (, ) K folded over B neutrino spectrum Wint () are given in Table I. In Table I and Fig. 2, the cross sections are obtained with ICARUS condition, that is, electron energies are higher than 5 MeV. The cross section for the GT transition is enhanced for SDPF-VMU-LS compared to that of Ref. Orm () about by 55. When the two-body spin-orbit interaction is switched off in the - cross-shell matrix elements, which is referred as SDPF-VMU, the enhancement of the cross section is about 43. The spin-orbit interaction is found to increase the cross section by about 9. Here, all the components of the GT transition, that is, the axial electric dipole, the magnetic dipole, the axial Coulomb and the axial longitudinal contributions are taken into acount while in Ref. Orm () only the axial electric dipole term is considered. As for the IA transition, both the Coulomb () and the longitudinal () terms are taken into account. The inclusion of the longitudinal term reduces the total contributions in the IA transition as


This explains why the IA contribution in Ref. Orm (), where only the term is included, is smaller than the SDPF-VMU case. The cross section for GT+IA is also found to be enhanced for SDPF-VMU-LS (SDPF-VMU) about by 22 (14) compared to ref. Orm ().

Cross sections for multipoles including up to =4 except for and are obtained by RPA with the use of SGII interaction SG (). The same quenching factor for as in the GT transitions is used. Calculated cross sections for GT, GT+IA, multipoles other than GT and IA, and the total cross section are shown in Fig. 2. The contributions from spin-dipole transitions and multipoles other than and are found to become important at 50 MeV.

Calculated total cross section obtained here is found to be rather close to that in Ref. Kolb () obtained by RPA calculations for all the multipoles. The cross section by the present hybrid model is enhanced about by 20-40 compared to Ref. Kolb () at lower energies, =20-40 MeV, where the GT contributions dominate. The calculated cross section in Ref. Chow () obtained by QRPA is smaller than our cross sections as well as in Ref. Kolb () about by three times. The GT distribution in Ref. Chow () is shifted toward higher energy region and quite a tiny strength is found below =8 MeV in contrast to the present case.

Iv Summary

In summary, we have carried out shell-model calculations for GT and IA transitions in Ar with the use of VMU interaction. The GT strength obtained is found to reproduce the experimental values rather well. The GT strength obtained here is larger than that in Ref. Orm ().

Cross sections for the charged-current -induced reaction, Ar (, ) K, are evaluated by a hybrid model, where contributions from the GT and IA transtions are obtained by shell-model calculations while other multipoles are treated by RPA. A better evaluation of the cross section for the GT contributions has been achieved in the present work. An enhancement of the cross section for solar neutrinos from B is found compared to previous calculations. The contributions from the GT and IA transitions dominate below 50 MeV while other multipoles become important at higher energies. It is strongy recommended that direct measurements of the cross section is carried out by using a liquid Ar TPC in near future. An accurate knowledge of the cross section is important for the advancement of the studies of supernova neutrinos and neutrino oscillations.

Here, we did not discuss neutral-current induced reactions on Ar as the present shell-model configuration space is not large enough to evaluate the magnetic dipole (M1) transition Li () and neutral-current induced transitions and the expansion of the configuration space beyond is difficult due to slow convergence of wave functions Orm (). Study of neutral-current reactions with larger shell-model configurations are left to future investigations.

This work has been supported in part by Grants-in-Aid for Scientific Research (C) 22540290 of the Ministry of Education, Culture, Sports, Science and Technology of Japan.


  • (1) ICARUS Collaboration, INFN Report No.INFN/AE-85/7, 1985 (unpublished); ICARUS-II. A Second-Generation Proton Decay Experiment and Neutrino Observatory at the Gran Sasso Laboratory, Proposal No.LNGS-94/99, VOL I (1993) and II (1994); Addendum to Proposal, LNGS 95-10 (1995);
  • (2) C. Anderson et al. (ArgoNeuT Collaboration), Phys. Rev. Lett 108, 161802 (2012).
  • (3) F. Cavanna, in The 8th International Workshop on Neutrino-Nucleus Interactions in the Few-GeV Region (NuInt12) (Rio de Janeiro, 2012).
  • (4) M. Bhattacharya, C. D. Goodman and A. Garcia, Phys. Rev. C 80, 055501 (2009).
  • (5) M. Bhattacharya et al., Phys. Rev. C 58, 3677 (1998).
  • (6) W. E. Ormand, P. M. Pizzochero, P. F. Bortignon and R. A. Broglia, Phys. Lett. B345, 343 (1995).
  • (7) T. Otsuka, T. Suzuki, M. Honma, Y. Utsuno, N. Tsunoda, K. Tsukiyama and M. Hjorth-Jensen, Phys. Rev. Lett. 104, 012501 (2010);
    T. Otsuka, T. Suzuki, R. Fujimoto, H. Grawe and Y Akaishi, Phys. Rev. Lett. 95, 232502 (2005).
  • (8) C. Yuan, T. Suzuki, T. Otsuka, F. Xu and N. Tsunoda, Phys. Rev. C 85, 064324 (2012).
  • (9) Y. Utsuno, T. Otsuka, T. Mizusaki and M. Honma, Phys. Rev. C 60 054315 (1999).
  • (10) M. Honma, T. Otsuka, T. Mizusaki, M. Hjorth-Jensen and B. A. Brown, Journal of Physics: Conference Series 20, 7 (2005);
    M. Honma, T. Otsuka, B. A. Brown and T. Mizusaki, Phys. Rev. C 65, 061301 (2002); ibid. C 69, 034335 (2004).
  • (11) OXBASH, the Oxford, Buenos-Aires, Michigan State, Shell Model Program, B. A. Brown, A. Etchegoyen, and W. D. M. Rae, MSU Cyclotron Laboratory Report No. 524, 1986.
  • (12) T. Mizusaki, N. Shimizu, Y. Utsuno and M. Honma, MSHELL64 code(unpublished).
  • (13) E. K. Warburton and B. A. Brown, Phys. Rev. C 46, 923 (1992).
  • (14) J. D. Walecka, in Muon Physics, edited by V. H. Highes and C. S, Wu (Academic, New York, 1975), Vol. II;
    J. S. O’Connell, T. W. Donnelly, and J. D. Walecka, Phys. Rev. C 6, 719 (1972);
    T. W. Donnelly and J. D. Walecka, Nucl. Phys. A274, 368 (1976);
    T. W. Donnelly and W. C. Haxton, Atomic Data Nucl. Data Tables 23, 103 (1979).
  • (15) J. Engel, Phys. Rev. C 57, 2004 (1998).
  • (16) W. T. Winter, S. J. Freedman, K. E. Rehm and J. P. Schiffer, Phys. Rev. C 73, 025503 (2006).
  • (17) Nguyen Van Giai and H. Sagawa, Phys. Lett. B 106, 379 (1981).
  • (18) E. Kolbe, K. Langanke, G. Martínez-Pinedo and P. Vogel, J. Phys. G 29, 2569 (2003);
    I. Gil-Botella and A. Rubbia, arXiv:hep-ph/0307244v2.
  • (19) M-K. Cheoun, E. Ha and T. Kajino, Phys. Rev. C 83, 028801 (2011).
  • (20) T. C. Li et al., Phys. Rev. C 73, 054306 (2006).
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description