Elementary excitations in Neutron Star matter

1. Elementary excitations in Neutron Star matter M. Baldo INFN, Sezione di Catania ECT* , March 2017

2. Schematic view of a neutron star

3. Asection(schematic) of a neutron star

4. MOTIVATIONS . Neutrino emission from the superfluid matter . Neutrino mean free path . Heat capacity . Thermal and electrical conductivity

5. The physical picture of the matter The homogeneous Neutron Star matter below the crust is mainly composed of neutrons, protons and electrons, in beta and chemical equilibrium and at low temperature. Charge neutrality imposes equal number of protons and electrons. The matter is extremely asymmetric, with the proton fraction ranging from 1% to 10 % Both neutrons and protons can be superfluid

6. Possible physical effects Neutrino emission # A collective mode with energy linear in momentum cannot decay into a neutrino-antineutrino pair. It is essential to know the strength function # Vertex renormalization of the response function Neutrino mean free path # Scattering from the Goldstone mode or collective modes in general Heat capacity # Counting correctly the effective degrees of freedom Transport coefficients # Screening of the effective interaction by the collective modes

7. Some references J. Kundu and S. Reddy, PRC 70, 055803 (2004) L.B. Leinson and A. Perez, PLB 638, 114 (2006) A. Sedrakian, H. Muether and P. Schuck, PRC 76, 055805 (2007) A.W. Steiner and S. Reddy, PRC 79, 015802 (2009) L.B. Leinson, PRC 79, 045502 (2009) E. Kolomeitsev and D. Voskresenky, PRC 81, 065801 (2010) M.B. and C. Ducoin, PRC 84, 035806 (2011) N. Martin and M. Urban, PRC 90, 065805 (2014)

8. We will include neutron, proton and electron components Questions to be answered . How much protons and neutrons decouple ? . How efficient is the electron screening ? . How much neutron modes are affected by protons ?

9. Linear response including electrons and protons only

10. NORMAL SYSTEM. Electron screening effect. From the proton plasmon to the sound mode Static electron background Plasmon mode With screening Sound mode

11. Proton and electron spectral functions. Normal system M.B. and C. Ducoin , PRC79, 035901 (2009)

12. Overview of superfluid gaps in homogeneous matter (below the crust) We consider the region where neutron superfludity can be neglected

13. Difficulty in the gap calculation The pairing gap will be considered as a parameter Final proton gap M.B. , H.-J. Schulze, PRC 75, 025802 (2007)

14. Pairing interaction only Spectrum Strength function Goldstone mode Pair-breaking mode

15. Including the Coulomb interaction Death and resurrection of the Goldstone mode Static electrons Proton plasmons Including electrons “Pseudo-Goldstone” mode

16. Evolution of the spectrum. Pairing + Coulomb

18. From the pseudo-Goldstone to the sound mode Pseudo- Goldstone Sound mode

19. The electron plasmon damping

20. Including the nuclear interaction and neutrons in the normal phase Nuclear interaction from BHF as Skyrme-like functional monopolar approximation

21. Three components spectral function The proton pseudo-Golstone mode persists

23. The proton sound mode persists

25. A closer comparison No np coupling With np coupling Notice : no sound mode for the neutron gas ( attractive nn particle-hole effective interaction )

26. No np coupling With np coupling

27. No np coupling With np coupling proton pair breakinh mode

28. Two times saturation density Pseudo-Goldstone Neutron zero-sound mode No np coupling With np coupling Pair-breaking mode

29. Two times saturation density

33. THANKS !!

34. Position of the centroid of the peak in the proton spectral function