1. Impact of electro-weak processes in Type II Supernovae collapse
IPN Orsay
CEA, DAM, DIF
Observatoire de Paris,
Meudon
Università degli Studi di Milano
Dipartimento di Fisica
Université Libre de Bruxelles
IAA
energie atomique . energies alternatives
Impact of electro-weak processes
in Type II Supernovae collapse
Patrick BLOTTIAU & Anthea F. FANTINA
(CEA/DAM/DIF) (IAA – ULB Brussels)
Dr. E. Khan, Dr. J. Margueron (IPN Orsay)
Dr. Ph. Mellor (CEA, DAM, DIF)
Dr. J. Novak, Dr. Micaela Oertel (Luth, Meudon)
Prof. P. Pizzochero & Dr. P. Donati
(Univ. Milano & INFN)
MODE, Bordeaux, November 15-17, 2010

2. Nucleon effective mass
Outline
MICROPHYSICS
MACROPHYSICS
Weak-processes
Neutrino transport
Symmetry energy(T)
SN Simulations
Nucleon effective mass
Hydrodynamics
Equation of State
One-zone
General
Relativity
Newtonian
P. Blottiau & A.F. Fantina
MODE 2010

3. Part I: intro & 1D Newtonian code (with n transport)
P. Blottiau & A.F. Fantina
MODE 2010

4. Motivations: nuclear physics in SN
Condition in the core
during collapse :
1) Very wide range of rho, T, Ye
2) We expect effects of T important
3) Asymmetry -> importance of the symmetry energy
Esym (T)
15 solar mass progenitor
P. Blottiau & A.F. Fantina
MODE 2010

5. T-dependence of Esym Theoretical studies on influence
of T-dependence of nuclear symmetry energy
on collapse trajectory:
Donati P. et al, Phys. Rev. Lett. 72, 2835 (1994)
Esym(T) obtained in analogy with Fermi gas model via m*(T):
PVC
dynamical effects
beyond mean field
(E-dependence of MF)
Dean D.J. et al, Phys. Rev. C66, (2002)
P. Blottiau & A.F. Fantina
MODE 2010

6. EoS in SN simulations (see M. Oertel’s talk)
Lattimer and Swesty, Nucl. Phys. A 535, 331 (1991)
- based on a liquid drop model -
Shen et al., Nucl. Phys. A 637, 435 (1998)
- based on RMF -
and : ? (or Esym(T) as in Donati et al.?)
but : not easy to implement Esym(T) in these EoS
Bethe H.A. et al., Nucl. Phys. A 324, 487 (1979) (BBAL)
based on a liquid drop model
analytical EoS
m*(T) has been implemented according to calculations by Donati et al.
Outlooks: include this “thermal” effect in modern EoS
P. Blottiau & A.F. Fantina
MODE 2010

7. Effect of Esym(T) on CCSN
on free protons
on nuclei
larger values of Ylept at trapping
 less deleptonization
 less energy dissipated
m*(T) Esym Yl,tr Shock wave energy
In one-zone model  m*(T) leads to systematic reduction of deleptonization
in the core: dT Ylept ≈ ⇒ dT Ediss ≈ 0.4 foe
( A.F.Fantina, P. Donati and P. M. Pizzochero, Phys. Lett. B676, 140 (2009) )
P. Blottiau & A.F. Fantina
MODE 2010

8. Results of collapse simulation at bounce: impact of Esym(T), BBAL EoS (1D Newtonian)
Systematic effect!
( A.F.Fantina, P. Blottiau, J. Margueron, Ph. Mellor, and P. Pizzochero, in preparation)
P. Blottiau & A.F. Fantina
MODE 2010

9. Conclusions & Outlook (I)
Influence of T-dependence of Esym on the evolution of collapse
→ systematic reduction of neutronization of the core
(increasing of final lepton fraction) & less energy dissipated by shock wave
- one zone model -
→ position of shock wave formation: bigger homologous core
- 1D Newtonian code -
 even if no dramatic effect on dynamics of the collapse is expected
(see fluid instabilities, SASI, magnetic field, …)
effects are not negligible!
P. Blottiau & A.F. Fantina
MODE 2010

10. Part II: 1D GR (+ Newtonian vers.) code (no n transport)
P. Blottiau & A.F. Fantina
MODE 2010

11. Results of collapse simulation at bounce: “std” trapping (1D GR), LS EoS K=180MeV
Bruenn 1985 rates
P. Blottiau & A.F. Fantina
MODE 2010

12. GR vs Newtonian simulation at bounce
P. Blottiau & A.F. Fantina
MODE 2010

13. Conclusions (II) GR code : improvements
→ introduction of a trapping scheme
→ implementation of the Newtonian version
→ results in global agreement with the literature
Influence of neutrinos in GR framework :
→ multi-group + trapping scheme allows for a first spectral information
but : - trapping on density (same treatment for different neutrino energy)
- processes other than capture (e.g. scattering) missing!
P. Blottiau & A.F. Fantina
MODE 2010

14. General Conclusions & Outlooks
Microphysics Macrophysics
nuclear physics dynamics of collapse
Nuclear inputs (microscopic calculation):
EoS: extension of LS; different tables
(J. Margueron, M. Oertel,
S. Goriely, N. Chamel)
deleptonization processes
electron capture rates (E. Khan)
symmetry energy
nucleon effective mass
and their T-dependence (RPA)
(P. Donati, J. Margueron, P. Pizzochero)
neutrino physics
(P. Blottiau, J. Margueron, Ph. Mellor)
Hydrodynamics:
One-zone
(P. Donati, P. Pizzochero)
1D Newtonian
(P. Blottiau, Ph. Mellor)
1D General Relativistic:
n transport
(J. Novak, J. Pons,
P. Blottiau, Ph. Mellor)
P. Blottiau & A.F. Fantina
MODE 2010

15. Thank you