2. What are we doing?

3. Large-scale ab initio No-core Shell Model calculations

4. What are we doing? Large-scale ab initio No-core Shell Model calculations + new realistic NN interaction JISP

5. Ab initio:

6. No model assumptions (shell model with inert core, cluster model, etc., are not ab initio)

7. Ab initio: No model assumptions (shell model with inert core, cluster model, etc., are not ab initio) Ab initio approaches: Faddeev (A  4) hyperspherical (A  6) Green function’s Monte Carlo (A  13) no-core shell model (A < 20) coupled-cluster approach (around closed shells)

8. Modern NN interaction models:

9. Realistic (phenomenological) meson-exchange NN potentials (Nijmegen, Bonn, Argonne) + NNN phenomenological potentials

10. Modern NN interaction models: Realistic (phenomenological) meson-exchange NN potentials (Nijmegen, Bonn, Argonne) + NNN phenomenological potentials EFT (ChPT) NN potentials + NNN EFT (ChPT) potentials

11. Modern NN interaction models: Realistic (phenomenological) meson-exchange NN potentials (Nijmegen, Bonn, Argonne) + NNN phenomenological potentials EFT (ChPT) NN potentials + NNN EFT (ChPT) potentials JISP16 NN interaction no NNN interaction fitted to light nuclei

12. Why would be nice to avoid NNN forces?

13. Role of NNN force? W. Polyzou and W. Glöckle theorem (Few-body Syst. 9, 97 (1990)):H=T+V ij  H’=T+V’ ij +V ijk, where V ij and V’ ij are phase-equivalent, H and H’ are isospectral. Hope: H’=T+V’ ij +V ijk  H=T+V ij with (approximately) isospectral H and H’. JISP type interaction seems to be NN interaction minimizing NNN force. Without NNN force calculations are simpler, calculations are faster, larger model spaces become available; hence predictions are more reliable.

14. JISP = J-matrix inverse scattering potential

15. J-matrix formalism: scattering in the oscillator basis

16. JISP NN interaction NN interaction is a small matrix of the in the oscillator basis: 9 ћΩ truncation, ћΩ = 40 MeV fast convergence of shell model calculations Good description of NN data

17. JISP16 properties 1992 np data base (2514 data): χ 2 /datum = 1.03 1999 np data base (3058 data): χ 2 /datum = 1.05

18. PETs

19. Ambiguity of JISP interaction Any unitary transformation of NN Hamiltonian H generates a Phase-equivalent transformation (PET). Simplest PETs with continuous parameters are used to fit properties of light nuclei in No-core Shell Model (NCSM) calculations.

20. JISP NN interaction A. M. Shirokov, A. I. Mazur, S. A. Zaytsev, J. P. Vary, T. A. Weber, Phys. Rev. C 70, 044005 (2004): A ≤ 4 A. M. Shirokov, J. P. Vary, A. I. Mazur, S. A. Zaytsev, T. A. Weber, Phys. Lett. B 621, 96 (2005): A ≤ 6 — JISP6 A. M. Shirokov, J. P. Vary, A. I. Mazur, T. A. Weber, Phys. Lett. B 644, 33 (2007): A ≤ 16 — JISP16

21. Modern NN interaction models: Meson-exchange NN potentials (Nijmegen, Bonn, Argonne) and EFT (ChPT) NN potentials + NNN phenomenological or EFT (ChPT) potentials JISP16 NN interaction good enough convergence with bare interaction bad convergence; effective interaction is needed

22. Our initial approach

27. From effective interactions to no-core full configuration calculations Extrapolation: E gs (N max ) = ae -bN max + E gs (∞) Works with bare interaction only (e.g., JISP16) Example: P. Maris, J. P. Vary, A. M. Shirokov, Phys. Rev. C 79, 014308 (2009)

28. Successful prediction: 14 F 1,990,061,078 basis states each ħΩ point requires 2 to 3 hours on 7,626 quad-core compute nodes (30,504 processors in total) at the Jaguar supercomputer at ORNL

29. Successful prediction: 14 F spectrum

30. Deficiency of JISP16 revealed by NCFC extrapolations

31. How it looked initially: How it looks now:

32. Improved interaction JISP16 2010 Obtained by a more accurate fit to nuclear data using NCFC

33. Nuclear matter with JISP16

34. Nuclear matter JISP16 2010 improves NM properties. Strong dependence on high partial waves makes it possible to fit NM to phenomenological data without violating description of light nuclei.

35. Conclusions Ab initio NCFC approach based on NCSM is able to describe light nuclei with A < 20. JISP16 provides a good description of NN data and binding energies, spectra, EM transitions in light nuclei, etc., without NNN forces. An improved version JISP16 2010 providing a more accurate description of nuclei is available. Later this version will be additionally fitted to nuclear matter too. Further development: description of other observables, e.g., rms radii in heavy enough nuclei, description of heavier nuclei, design of charge-dependent version of the interaction.

36. Thank you!