JINA. Address open questions by working on the nuclear physics and the astrophysics

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1 JINA goals Astrophysics Nuclear Physics JINA Address open questions by working on the nuclear physics and the astrophysics

2 JINA workshop goals Interesting problems Ready to be addressed Unknowns ready to be addressed & feasible! GCE (Astro) Nuclear physics Identify this overlap Key problems in GCE ready to be addressed That also require work in nuclear physics (as these would likely not be done without cross field collaboration)

3 Approach 1: How to identify nuclear - astro overlap Identify key problems in GCE Identify among these critical nuclear physics problems Think about nuclear physics analysis/sensitivity studies See where nuclear physics progress would be feasible --> trigger new nuclear physics efforts Approach 2: This talk Look at ongoing and planned nuclear physics efforts (which processes see advances, which nuclei are affected) (note that feasibility is a big factor - so what can be done likely is done) Identify the interesting GCE problems where one can take advantage of improvements in nuclear physics --> trigger new astrophysics efforts

4 Area 1: r-process: recent nuclear physics efforts N=126 ORNL (d,p) transfer N=82 STOP ISOLTRAP masses N=50 STOP GSI β-decay ANL CPT masses GSI/Mainz β/pn-decay STOP r-process A<110 ISOLDE (< Pd) 130 Cd β-endpoint disentangle contributions GSI/RISING 130 Cd isomers LEPP GSI IMS mass measurements νp-process JYFLTRAP weak masses and main s-process ORNL β-decay NSCL TOF masses NSCL β/pn-decay campaign (Mainz, Maryland, MSU, Notre Dame, PNNL)

5 Example: impact of improved nuclear physics Can calculate relative pattern of 78 Se, 79 Br, 80 Se produced in a cassical r-process based on experimental nuclear data Solar data Hosmer et al. to be published

6 Area 2: rp-process (νp-process) ORNL α-decay JYFLTRAP - SnSbTe Cycle Decay studies (GSI, NSCL) Coulomb shift calculations (Brown et al.) Drip line studies (NSCL) JYFLTRAP SHIPTRAP CPT ISOLTRAP LEBIT Mass known <10 kev Mass known

7 Area 3: Galactic radioactivity 44 Ti by CGRO (T 1/2 = 60 yr) 60 Fe by INTEGRAL SPI (T 1/2 = yr) CGRO obs JINA Efforts (Timmes, Wiescher, et al.) improved reaction rates for 44 Ti production: 40 Ca(α,γ) improved reaction rates for 60 Fe production: 59,60 Fe(n,γ) supernova model calculations for 44 Ti and 60 Fe production

8 Area 4: Production of iron group isotopes in Sn Ia Change of ejecta composition in SN Ia model when using different sets of electron capture rates (Brachwitz et al. 2000) Affected are n-rich isotopes: 48 Ca, 50 Ti, 54 Cr, 54,58 Fe, and 58 Ni

9 NSCL charge-exchange program (R. Zegers et al.) probe weak interaction strength to test shell model large scale JINA project: database for experimental data large scale shell model calculations with different interactions --> understand error bars --> key reactions for theory improvements --> new astrophysical data set? 9

10 Area 5: neutron sources in the s-process Experimental efforts (Wiescher, Best, Falahat et al.): (α,n) rates on 22 Ne, 17 O, 18 O, 25 Mg, 26 Mg (and on α,γ competition) NuGRID Hirschi et al. --> main impact on weak s-process in massive stars

11 JINA reaclib database Richard Cyburt et al. Reaction rates (no uncertainties) Goal: provide best rates available in literature at any given time Continuous rapid updates Only modest evaluation for quality control (ensure new version is improvement) Include published evaluations (including evaluations by reaclib group)

12 Summary: areas affected by exp nuclear work stellar evolution affected by 3-alpha (talk by Sam Austin) p-process? (New program by Artemis Spyrou) r-process <Pd (LEPP, νp-process, s-process) and around A= Ti and 60 Fe iron group in Sn Ia ( 48 Ca, 50 Ti, 54 Cr, 54,58 Fe, and 58 Ni)) s-process: 22 Ne(α,n) and weak s-process νp-process (n-deficient isotopes up to A~100?) (Talk by Carla Fröhlich)

13 The r-process at A=80 Baruah et al Precision masses from ion traps (JYFLTRAP, ISOLTRAP)? known n-emission branchings 80 Zn 0.54s 79 Cu 0.19s 78 Ni 0.11s? 81 Zn 82 Zn 0.29s > Unique region where main nuclear physics for the r-process is now experimentally constrained