Experimental inputs for supernova dynamics

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1 Experimental inputs fr supernva dynamics Francesca Gulminelli - LPC Caen Eric Bnnet Subatech Nantes Beyhan Bastin & Françis de Oliveira Ganil Adriana Raduta IFIN LIA COSMA

2 Type II Supernvae Supernva explsin ccurs via cre-cllapse in very massive stars (M>8M sun ) Shck frnt is stalled unless revived by extra neutrin emissin Critically depends n electrn capture during cllapse e+p->n+n Ejecta might be seeds fr r- prcess if matter is sufficiently n-rich Critically depends n the glbal prtn fractin and n the cmpsitin f matter at the neutrinsphere F.S.Kitaura et al, A&A 450 (06) 345

3 Type II Supernvae Our LIA prject: study e-capture rates (I) and matter cmpsitin (II) within a mdel including realistic nuclear inputs Identify key nuclear bservables Stimulate experiments and prvide theretical simulatins and interpretatins F.S.Kitaura et al, A&A 450 (06) 345

4 (1) Electrn capture during cre cllapse The supernva evlutin and n luminsity crucially depends n the e-capture rate. The main nuclei invlved are very neutrn rich istpes arund the N=50 and N=82 magic numbers Their mass and e-capture prbability gvern the glbal deleptnizatin rate C.Judagalvis 2010 C.Sullivan 2016

5 (1) Electrn capture during cre cllapse Effect f the mass Effect f the capture rate A.Raduta 2016 A.Raduta 2017 These are nly sensitivity studies. The final answer can nly cme frm measurements arund N=50 and N=82

6 (1) Electrn capture during cre cllapse I-220 JYFL prpsal (B.Bastin, A.Kankainen) Mass measurements in the vicinity f 78Ni t cnstraint cre cllapse supernvae mdels and t study the N=50 and Z=28 shell t be run in 2017 High precisin mass measurement fr 5 new istpes arund Z=28 N=50 E-capture rates n these same extic nuclei can be deduced frm the inverse b decay prcess GT strength measurement Study in prgress Phase space factr Transitin rate

7 The pssibility f generating a strng r-prcess in SN explsins depends n the initial prtn fractin and matter cmpsitin In turn, this depends n the in-medium mdificatin f nuclear masses Exp.study requires many light nuclei at lw r and finite T => vaprizatin data withut Present data (Texas A&M) (2) Matter cmpsitin at the n-sphere One single data set Symmetric N~Z system nly N verificatin f equilibrium T and r frm theretical mdel with

8 (2) Matter cmpsitin at the n-sphere Analysis f INDRA data Ni+Ni 90 A.MeV Temperature frm particle spectra

9 (2) Matter cmpsitin at the n-sphere Analysis f INDRA data Ni+Ni 90 A.MeV Temperature frm particle spectra Density frm bund particle fractin

10 (2) Matter cmpsitin at the n-sphere Analysis f INDRA data Ni+Ni 90 A.MeV Temperature frm particle spectra Density frm bund particle fractin N deviatin f equilibrium up t secnd mments

11 (2) Matter cmpsitin at the n-sphere Analysis f INDRA data Ni+Ni 90 A.MeV Temperature frm particle spectra Density frm bund particle fractin N deviatin f equilibrium up t secnd mments Analysis in prgress Prpsitin f a FAZIA@GANIL LI (E.Bnnet) t extend t asymmetric nuclei

12 Cnclusins The understanding f cre cllapse supernva dynamics and explsive nuclesynthesis requires a realistic nuclear mdelling including key inputs frm experimental data n n-rich nuclei Our cntributin: A micrscpic ES mdel including the full distributin f nuclear species LI FAZIA@GANIL =>2016 Mass measurement at IGISOL (n-rich Fe and C istpes) =>2017 Analysis f INDRA vaprizatin data =>nw GT strenght prpsal t extract e-capture rates =>in prgress