1. Jorge Pereira, INPC 2007 Jorge Pereira (pereira@nscl.msu.edu) National Superconducting Cyclotron Laboratory (NSCL/MSU) Joint Institute for Nuclear Astrophysics (JINA) Studies of r-process nuclei at NSCL Astrophysical importance of  -decay studies in the understanding of the r-process Jorge Pereira, INPC 2007

2. Synthesis of Heavy Elements An overview on astronomical abundance observations SNR 0103-72.6 Credit: NASA/CXC/PSU/S.Park et al. M57 Ring Nebula.

3. Jorge Pereira, INPC 2007 Observed Solar-System Heavy-Element abundances log  = log 10 (Y el /Y H )+12 Solar s-process p-process r-process Different processes contribute to the observed Heavy-Element abundances r ≈ “leftovers” ( Solar – s )

4. Jorge Pereira, INPC 2007 CS22892-052 HD 115444 BD+17 0 3248 CS 31082-001 HD221170 J.Cowan and C.Sneden, Nature 440, 1151 (2006) R -process elemental abundances: Solar-System vs. Metal-Poor Stars (MPS) Consistent abundances (MPS and Solar) pattern for Z > 47 Very ROBUST r-process (MAIN r-process) Missing abundance  Another process contributing to solar light r-residuals?

5. Jorge Pereira, INPC 2007 LEPP elemental= HD122563– Main LEPP elemental= solar– s-process– Main F. Montes et al., submitted to ApJ LEPP contributes to r-process elemental abundances Very consistent pattern  Second ROBUST process LEPP contributes to r-process elemental abundances Very consistent pattern  Second ROBUST process What about less enriched stars? LEPP process C. Travaglio et al., ApJ 601, 864 (2004)

6. Jorge Pereira, INPC 2007 D. Swesty, A. Calder, E.Wang, D.Bock, NCSA (1998) How do these processes operate? What is their site? Comparing results (e.g. classical approach) with observed abundance pattern E0102-72.2

7. Jorge Pereira, INPC 2007 Astrophysical conditions: parameterized studies (e.g n n, T, t irr )…freeze-out, neutrinos Nuclear Physics (mostly theoretical):  -decay properties (T ½, P n, masses) What are these models sensitive to? Astrophysics VS. Nuclear Physics Mass number ETFSI-Q ETFSI-1 Classic model. Different Nuclear Physics C.Freiburghaus et al., ApJ516, 381 (1999) Astrophysical r-process model calculations are very sensitive to Nuclear Physics of nuclei involved

8. Jorge Pereira, INPC 2007 Why  -decay studies in the search for the r-process and LEPP sites? NSCL experiments with Exotic Beams

9. Jorge Pereira, INPC 2007  -decay properties in the r-process P n -values around r-process nuclei: What is the path followed by matter flow after freeze-out (Abundance pattern post freeze-out) Half-lives of r-process nuclei: The clock of the r-process What are the bottle-necks of matter flow?  Abundance pattern prior freeze-out T 1/2 and P n (gross  -decay properties): First insights into shell structure at low energies and above S n (Deformation, nucleon-nucleon interaction, new magic numbers, etc…)  -decay studies of very exotic neutron-rich nuclei at NSCL

10. Jorge Pereira, INPC 2007 Ion Source K500 : Operated 1982-1989 Coupled in 2000 K1200 : Operated 1989-1999 Exotic beam delivery: The CCF

11. Jorge Pereira, INPC 2007 Ion Source K500 K1200 A1900 Exotic beam delivery: The A1900 in-flight separator

12. Jorge Pereira, INPC 2007 A1900 Im2 Ion Source K500 K1200 Exotic beam delivery: The A1900 in-flight separator ToF Im2-N3  E PIN N3 vault Separation and identification of exotic beam: ToF vs.  E  E PIN (a.u.) ToF Im2-N3 (a.u.) 107 Zr

13. Jorge Pereira, INPC 2007 A1900 Im2 Ion Source K500 K1200 Exotic beam delivery: The A1900 in-flight separator N3 vault Separation and identification of exotic beam: ToF vs.  E Exotic beam  Implantation station (in the N3 vault)

14. Jorge Pereira, INPC 2007 Silicon PIN Stack 4 x Si PIN DSSD (  Implantation DSSD: x-y position (pixel), time Decay DSSD: x-y position (pixel), time 6 x SSSD (16) Ge Implantation station: The Beta Counting System (BCS) Veto light particles from A1900 J.J. Prisciandaro et al., NIMA 466, 492 (2001) 105 Zr Fit (mother, daughter, granddaughter, background)  T 1/2

15. Jorge Pereira, INPC 2007 Silicon PIN Stack 4 x Si PIN DSSD (  Implantation DSSD: x-y position (pixel), time Decay DSSD: x-y position (pixel), time 6 x SSSD (16) Ge Beta calorimetry Implantation station: The Beta Counting System (BCS) Veto light particles from A1900

16. Jorge Pereira, INPC 2007 Implantation station: The Neutron Emission Ratio Observer (NERO) Boron Carbide Shielding Polyethylene Moderator BF 3 Proportional Counters 3 He Proportional Counters G. Lorusso, J.Pereira et al., PoS NIC-IX (2007)

17. Jorge Pereira, INPC 2007 Implantation station: The Neutron Emission Ratio Observer (NERO) Nuclei with  -decayNuclei with  -decay AND neutron(s) P n -values Measurement of neutron in “delayed” coincidence with  -decay

18. Jorge Pereira, INPC 2007 Implantation station: The Segmented Germanium Array (SeGA) 16 SeGA detectors around the BCS Efficiency ~7.5% at 1 MeV W.Mueller et al., NIMA 466, 492 (2001)

19. Jorge Pereira, INPC 2007 Implantation station: The Segmented Germanium Array (SeGA)  -delayed gamma spectroscopy of daughter

20. Jorge Pereira, INPC 2007 Results from  -decay r-process campaigns at NSCL

21. Jorge Pereira, INPC 2007 NSCL r-process campaigns – MSU/Mainz/Notre Dame/Maryland Known before NSCL Experiments done P. Hosmer, P. Santi, H. Schatz et al. F. Montes, H. Schatz et al. B. Tomlin, P.Mantica, B.Walters et al. J.Pereira, K.-L.Kratz, A. Woehr et al. Critical region 78 Ni 107 Zr NSCL reach 129 Rh

22. Jorge Pereira, INPC 2007 Exp. 78 Ni T 1/2 = 110 ms Predicted 78 Ni T 1/2 : 460 ms P. Hosmer et al. PRL 94, 112501 (2005) +100 -60 I )  -decay half-live of 78 Ni 50 waiting point Half-live of ONE single waiting-point nucleus:  Speeding up the r-process clock  Increase matter flow through 78 Ni bottle-neck  Excess of heavy nuclei (cosmochronometry)

23. Jorge Pereira, INPC 2007 II ) “Gross” nuclear structure around 120 Rh 65 from  -decay properties F. Montes et al., PRC73, 35801 (2006) Inferring (tentative) nuclear deformations with QRPA model calculations Half-lives and P n -values sensitive to nuclear structure at different energies: (Complementary information to infer nuclear deformation) Need microscopic calculations beyond QRPA Possible signatures of new shell-structure when approaching r-process path

24. Jorge Pereira, INPC 2007 II )  Probing sustainability of N=82 at 120 Pd from  -delayed  -spectroscopy B.Walters, B.Tomlin et al., PRC70 034414 (2004) No evidence of shell-quenching when approaching waiting point 128 Pd at N=74 Need more E(2+) data at 74<N<82

25. Jorge Pereira, INPC 2007 III )  -decay properties of Zr isotopes beyond mid-shell N=66 A ≈110: Calculations fail to reproduce r-process abundance pattern below A=130 peak N~66 is at mid-shell: Shape transitions between sudden onset of deformation at N=60 and closed shell at N=82 Possible double-magic Z=40, N=70: Effects from spherical shape of 110 Zr 70 observable at 66<N<70? J. Dowaczewski et al.,PRL72, 981 (1994) J.Pereira et al., in preparation Shorter half-life of (potential) waiting-point 107 Zr 67 may affect predicted r-process abundances at A~110 QRPA consistent with spherical shapes beyond mid- shell (possible signatures of double magic N=40 N=70?) Urgent need of microscopic calculations beyond QRPA

26. Jorge Pereira, INPC 2007 Almost all  -decay half-lives of r-process nuclei at N=82 and N=126 will be reachable with ISF pps Reach for future r-process experiments with new facilities (ISF, FAIR, RIBF…) Fine!…but what do we do meanwhile? a)Keep observing abundances and wait for these facilities… b)Continue r-process studies with theoretically calculated  -decay properties (to be confirmed with new measurements)

27. Jorge Pereira, INPC 2007 Conclusions Despite many years of intensive effort, the r-process site continues to be one of the BIG SCIENCE QUESTIONS for the new century – NAS REPORT. New LEPP process complicates the situation Besides being direct r-process inputs, beta-decay properties of exotic nuclei turned out to be an effective probe for nuclear structure studies of exotic nuclei R-process experimental campaigns at NSCL provide an extensive data body of beta-decay properties of r-process nuclei. Comparisons with calculations microscopic models will improve astrophysical r-process calculations New facilities will largely extend the r-process regions accessible. Meanwhile, new observations (SEGUE) and new measurements of exotic n-rich nuclei are highly necessary

28. Jorge Pereira, INPC 2007 Thanks to: NSCL/MSU: Hendrik Schatz, Paul Mantica Ana Becerril, Tom Elliot, Alfredo Estrade, Ron Fox, Daniel Galaviz, Tom Ginter, Mark Hausmann, Paul Hosmer, Linda Kern, Giuseppe Lorusso, Milan Matoš, Fernando Montes Univ. Notre Dame: Andreas Woehr Ani Aprahamian, Matt Quinn Mainz Universität: Karl-Ludwig Kratz Oliver Arnd, Ruben Kessler, Stefan Hennrich, Bernd Pfeiffer, Florian Schertz University of Maryland: William Walters JINA and VISTAR collaborations

29. Jorge Pereira, INPC 2007 Backup Slides

30. Jorge Pereira, INPC 2007 The Big Question What is the origin of heavy elements from iron to uranium ? One of the “Eleven Science Questions for the New Century” (NAS report “Connecting Quarks with the Cosmos”) Do we understand the observed heavy- element abundances ?

31. Jorge Pereira, INPC 2007 What about less enriched stars? (Leftover of Leftover) Similar observations for Sr, Zr by C.Travaglio et al. Light Element Primary Process (LEPP) – C. Travaglio et al., ApJ 601, 864 (2004) – Some stars (e.g. HD122563) show enrichment of lighter elements (Sr-Ag) compared to MAIN r-process – F.Montes et al., submitted to ApJ –

32. Jorge Pereira, INPC 2007 [Eu/Fe] Enrichment with main r-process Light r / Heavy r (Eu)Heavy r / Heavy r (Eu) What about less MAIN r-process enriched stars?  Consistent with second process producing also Sr-Ag LEPP, identified by Travaglio et al. 2004 Montes et al. to be published Solar r Slope indicates ratio of light/heavy) changes for less enriched stars Some stars have light r-elements at solar level Heay r-pattern robust and agrees with solar Light r-elements at high enrichment fairly robust and subsolar [Y/Eu] [La/Eu] [Ag/Eu] [Sm/Eu] [Eu/Fe]

33. Jorge Pereira, INPC 2007 Trying to fit LEPP pattern with n-capture flow  Low n n and high n n fit low Z  Low n n also fits small high Z abundances

34. Jorge Pereira, INPC 2007 Conclusions depend on s-process s-process from Simmerer et al. (Cowan et al.) s-process from Travaglio et al.  Need reliable s-process (models and nuclear data)  Clearly something is going on for Z < ~50 (“light” p-process elements)  Need reliable s-process (models and nuclear data)  Clearly something is going on for Z < ~50 (“light” p-process elements) Need to look at many stars …

35. Jorge Pereira, INPC 2007 Astrophysical conditions: parameterized studies (e.g n n, T, t irr ) Nuclear Physics (mostly theoretical):  -decay properties (T ½, P n), masses Freeze-out Neutrino presence n-capture rates Fission barriers What are these models sensitive to? Astrophysics VS. Nuclear Physics Mass number ETFSI-Q ETFSI-1 Classic model. Different Nuclear Physics C.Freiburghaus et al., ApJ516, 381 (1999) 10 Hot bubble Classic model Mass number Abundances (Si≡10 6 ) Same Nuclear Physics Astrophysical r-process model calculations are very sensitive to Nuclear Physics of nuclei involved

36. Jorge Pereira, INPC 2007 Waiting point approximation Definition: ASSUME (n,  )-( ,n) equilibrium within isotopic chain This is a valid assumption during most of the r-process BUT: freezeout is neglected Freiburghaus et al. ApJ 516 (2999) 381 showed agreement with dynamical models How good is the approximation ? Consequences During (n,  )-( ,n) equilibrium abundances within an isotopic chain are given by: Time independent Can treat whole chain as a single nucleus in network Only slow beta decays need to be calculated dynamically Neutron capture rate independent (During most of the r-process n-capture rates do not matter !)

37. Jorge Pereira, INPC 2007 Inferring r-process conditions from “site-independent” models Parameterized Astrophysical conditions (e.g. n n, T, t irr ) Conditions which fit the A≈80 and A ≈ 130 r-process abundance peaks K.-L. Kratz et al., ApJ 403, 216 (1993)

38. Jorge Pereira, INPC 2007 Conditions for the r-process from “site-independent” models Parameterized Astrophysical conditions (e.g. n n, T, t irr ) Nuclear Physics of nuclei involved (mostly theoretical) K.-L. Kratz et al., ApJ 403, 216 (1993) Conditions which fit the A≈80 and A ≈ 130 r-process abundance peaks different components with large n n, T BUT very sensitive to Nuclear Physics!!! Mass number ETFSI-Q ETFSI-1 Classic model with different Nuclear Physics C.Freiburghaus et al., ApJ 516, 381 (1999)

39. Jorge Pereira, INPC 2007 n/seed is higher for lower Y e (more neutrons) higher entropy (low density  low 3  -rate  slow seed assembly) faster expansion (less time to assemble seeds) 1) high S, moderate Y e 2) low S, low Y e 2 possible scenarios: (Meyer & Brown ApJS112(1997)199) Neutron to seed ratios

40. Jorge Pereira, INPC 2007 Experiments with implanted RNB Production of Primary Beam: Coupled Cyclotron Facility, CCF Production of RNB: A1900 in-flight separator (Fragmentation reactions…and Fission (in progress))  -decay r-process motivated experiments at NSCL Beta Counting System: Half-lives (T 1/2 ) NERO:  -delayed n-emission probabilities (P n ) SeGA:  -delayed and “direct”  -spectroscopy

41. Jorge Pereira, INPC 2007 Results from earlier experiment in Ni I )  -decay half-live of 78 Ni waiting-point: testing model calculations Half-lives and Pn-values sensitive to nuclear structure at different energies: complementary information to rule out models

42. Jorge Pereira, INPC 2007 Results:  -decay Half-lives (even with low statistics) Decay-curves fits (mother, daughter, granddaughter) 105 Zr 107 Zr 106 Zr MLH: Find maximum of Likelihood function (sum of join probability density for 1, 2 and 3-member decay chains) 104 Zr 107 Zr

43. Jorge Pereira, INPC 2007 Calculated  -decay properties of r-process nuclei with FRDM-QRPA Macro/Microscopic model  global applicability (better suited for r-process models) 1. Calculation of ground-state masses and deformation parameters FRDM + Strutinsky microscopic corrections (Shell + Pairing) 2. Use deformation parameters to determine single-particle levels  (folded-Yukawa + Lipkin-Nogami) 3. Calculate Gamow-Teller  -strength function using calculated  and adding residual interaction V GT =2  GT :  1-  1+ : with operator  1± =∑ i (  t ± ) i Sensitivity to Deformation, Level ordering, Masses P. Möller et al., NPA 1992; ADNDT 1995, 1997; PRC2000

44. Jorge Pereira, INPC 2007 Future Facility Reach (here ISF) NSCL r-process campaign – MSU/Mainz/Notre Dame/Maryland Known before NSCL Experiments done P. Hosmer, P. Santi, H. Schatz et al. F. Montes, H. Schatz et al. J.Pereira, K.-L.Kratz, A. Woehr et al. Critical region NSCL reach 78 Ni 107 Zr

45. Jorge Pereira, INPC 2007 Initial conditions:  =29mg/cm 3 ; T=1.5GK; n/seed = 92 The r-process abundances (observed in Solar System and Metal-Poor Stars) is the only clue that “he” left behind…for us

46. Jorge Pereira, INPC 2007 Nuclear Physics in the r-process Nuclear Ingredient Direct Astrophysical interest Indirect Astrophysical interest Production cross-sections from different reaction mechanisms Production of r-process nuclei to be investigated   -decay half-lives (T 1/2 )   -delayed neutron-emission probabilities (P n )  r-process time scale (T 1/2 )  Abundance pattern prior (T 1/2 ) and post freeze-out (P n ) Nuclear structure information (at “low” cost) Nuclear masses (neutron separation energies) r-process pathNuclear structure Gamma spectroscopy Detailed nuclear structure information (shell-quenching)  Fission barriers  Fragment mass distributions  Primordial abundance pattern (Fission Cycling)  Final abundance pattern (  -delayed, -induced fission);  Endpoint What Nuclear Physics ingredients are really important?

47. Jorge Pereira, INPC 2007 (Pearson, et al. 1996) r-process studies in two different regions of Terra Incognita Two r-process regions were explored: Ge-Br (56≤N≤60): lies in the region prior to the “weak” r-process. It could also constitute part of the seed r-process nuclei Y-Mo (A ≈110): lies right before the abundance trough prior to the A=130 peak C.Freiburghaus et al., ApJ516 (1999) 381 Mass number ETFSI-Q ETFSI-1 A=110 Z number

48. Jorge Pereira, INPC 2007 Nuclear Structure motivation What do we want to measure?  -decay half-lives and P n -values Why? They provide insight into nuclear structure in two “critical” r-process regions Direct inputs in r-process calculations Evolution of nuclear shape in two regions of Terra Incognita Ge-Br (56≤N≤60): does the sudden onset of deformation (at N=60) persist “south” of 96 Kr? Y-Mo (A ≈110): are there more shape transitions between sudden onset of deformation at N=60 and closed shell at N=82 (new sub-shells?) Nuclear shape evolution in these two regions will affect substantially the calculated masses and   -decay processes: strong impact in r-process calculated abundances R.F. Casten, Nucl. Phys. A443 (1985) 1 N. Schunck et al., Phys. Rev. C63 (2004) 061305(R)

49. Jorge Pereira, INPC 2007 Gross  -decay properties used as nuclear structure probes Gross  -decay properties are sensitive to nuclear structure at different energy regimes Low energies Energies above S n Dobaczewski et al., PRL72 (1994) 981 B. Pfeiffer et al., NPA693 (2001) 282

50. Jorge Pereira, INPC 2007

52. Sensitivity of QRPA to Mass and Deformation

53. Jorge Pereira, INPC 2007 Preparation of experiments Nuclei produced by Fragmentation of 136 Xe on Be Beta Counting System (  CS): T 1/2 Neutron Emission Ratio Observer (NERO): P n Special blocking system (Slits + Finger) at Im1 to stop primary-beam charge-state BCS and NERO upgrades: VME-based DAQ, migration to production DAQ software (~400 channels), new Ge crystal (tested to be used for particle ID,  -spectroscopy) Special setup for particle ID based on known  sec-isomers with SeGA globes

54. Jorge Pereira, INPC 2007 Secondary Beam Experimental Setup Particle ID Setup (SeGA) Production Setup (BCS+NERO) Isomers (  sec) implanted in Al degrader Emitted gammas detected with 3 SeGA detectors (  6%) 4 Si PIN:  E, trigger 1 DSSD (1600 pixels): 4 cm x 4 cm active area 1 mm thick 40-strip pitch in x and y dimensions (1600 pixels) 1 SSSD (16 strips): Veto BCS (Beta Counting System) NERO (Neutron Emission Ratio Observer) Boron Carbide Shielding Polyethylene Moderator BF 3 Proportional Counters 3 He Proportional Counters Fragments implanted in DSSD Emitted  (DSSD) Delayed neutrons (NERO)

55. Jorge Pereira, INPC 2007 (Pearson, et al. 1996) Conquers of Terra Incognita in r-process campaigns at NSCL r process N=126 N=82 Z=50 Z=82 N=50 Z=28 F.Montes, H.Schatz, T 1/2,, P n B.Tomlin, B.Walters, P.Mantica, T 1/2,  -spectroscopy J.Pereira, A.Woehr, H.Schatz T 1/2,, P n J.Pereira, K.-L. Kratz, T 1/2,, P n P.Hosmer, H.Schatz, T 1/2,, P n M.Matoš, A.Estrade, Masses (ToF technique) Mass known Half-life known Terra Incognita

56. Jorge Pereira, INPC 2007 How about future? What can be done at NSCL for the r-process?

57. Jorge Pereira, INPC 2007 (Pearson, et al. 1996) How to reach now new territories at NSCL for r-process studies Mass known Half-life known Terra Incognita r process N=126 N=82 Z=50 Z=82 N=50 Z=28 Fission of 238 U at NSCL Optimistic results from test (May 2006) Beam test development (August 2006) 1. Future experiment to explore region around 128 Pd 2. Gain factor 10-100 with respect to Fragmentation of 136 Xe 3. Possibility to study E(2 1 +), E(4 1 +) isotopic evolution of nuclei near 132 Sn (BCS + SeGA) 4. Possibility to measure masses of waiting-point nuclei e.g. 130 Cd with ToF-B  technique (A1900+S800) If successful it will allow to go one step farther into Terra Incognita  New r-process regions to be explored at NSCL

58. Jorge Pereira, INPC 2007 Some advances of what it is coming in the near Future for the r-process RF-kicker Fragment Separator:.Purify beam-cocktail. Reduce background due to implanted contaminants in the BCS Development of U beams: Extend  -decay studies and mass measurements to new r-process regions Digital Data Acquisition (DDAQ): Increase SeGA resolutions and efficiencies (tests in progress) and BCS efficiencies (to be implemented). Precise  -decay half- lives, Q  values and spectroscopy information of new r-process LEBIT: Development of gas stopper for future use with reaccelerated beams. Measurement of important reactions occurring in the  -process (seed nuclei for the r-process) BCS calorimeter: Measurement of Q  values for r-process nuclei (additional structure information)

59. Jorge Pereira, INPC 2007 …and in the Future: NSCL upgrade NSCL upgrade will open new possibilities in Nuclear Astrophysics MSU Upgrade Beam intensities (pps) pps Fast beams: A very significant fraction of r-process nuclei will be reached experimentally. Integral  -decay properties of every r-process waiting-point below A=130 peak (included) and around N=126. Spectroscopy studies of waiting-point nuclei at N=82 and N=126: solution of the shell-quenching puzzle. Masses of very exotic nuclei: better determination of r-process path (S n ≈2MeV). Reaccelerated beams: Direct measurements of important reactions involved in the  -process (generation of r-process seed nuclei):  (nn,  ) 9 Be (di-neutron channel),  (  n,  ) 9 Be,  (t,  ) 7 Li, 7 Li(n,  ) 8 Li, 8 Li( ,n) 11 B… Other Nuclear Astrophysics aspects. Majority of reaction rates in rp-process will be within reach with indirect methods. Direct measurements will be achievable up to A<60. Measurement of GT-strength for e-capture by all relevant unstable nuclei in SNeI,II will be possible via charge exchange reactions. Very important reaction rates: e.g. 12 C( ,  ) 16 O

60. Jorge Pereira, INPC 2007 Epilogue

61. Jorge Pereira, INPC 2007 Summary Despite many years of active investigation the site of the r-process is still unknown. Nuclear Physics is crucial to solve this mystery My main research on the r-process included studies of reaction mechanisms to produce neutron-rich and  -decay studies of r-process nuclei: GSI: experimental studies of neutron-rich nuclei approaching the r-process region around N=126 GSI:  -decay properties of waiting-point 137 Sb  abundance spikes around A=130 peak NSCL: analysis of nuclear structure of r-process nuclei based on  -decay studies  abundance pattern around the weak r-process region and the A=110 abundance trough region Future developments at NSCL (including upgrade) will open new opportunities to extend our knowledge of the r-process NSCL will become the “r-process facility” and one of the dominant laboratories in Nuclear Astrophysics

62. Jorge Pereira, INPC 2007 Convince someone to cover the expenses of our adventure Develop new tools to reach “Terra Incognita” Learn from the natives living in the new territories The recipe to explore “Terra Incognita” The conquer of Terra Incognita (or the New World) …so that finally, Terra Incognita will not be “Incognita” anymore

63. Jorge Pereira, INPC 2007 Acknowledgements NSCL/MSU: Hendrik Schatz, Paul Mantica Ana Becerril, Tom Elliot, Alfredo Estrade, Ron Fox, Daniel Galaviz, Tom Ginter, Mark Hausmann, Vladimir Henzl, Daniela Henzlova, Paul Hosmer, Linda Kern, Giuseppe Lorusso, Milan Matoš, Fernando Montes, Josh Stoker, Andreas Stoltz, Oleg Tarasov, Remco Zegers Univ. Notre Dame: Ani Aprahamian, Andreas Woehr, Matt Quinn Univ. Santiago de Compostela: Jose Benlliure, Teresa Kurtukian Mainz Univ.: Karl-Ludwig Kratz Oliver Arnd, Ruben Kessler, Stefan Hennrich, Bernd Pfeiffer, Florian Schertz GSI colaboration: Peter Armbruster, Monique Bernas, Aleksandra Kelic, Valentina Ricciardi, Karl-Heinz Schmidt JINA and VISTAR collaborations

64. Jorge Pereira, INPC 2007 Backup Slides

65. Jorge Pereira, INPC 2007 OUTLOOK Introduction: what is the r-process? What do we need to know to learn about “him”? My relationship with the r-process: When we first met (at GSI): approaching Terra Incognita towards N=126 shell Learning more about r-process at GSI: studies around waiting point 137 Sb R-process experiments at NSCL: incursion into Terra Incognita through two different fronts Discovering what NSCL can do for the r-process What can we do for “them”? Future perspectives

66. Jorge Pereira, INPC 2007 (Pearson, et al. 1996) Present NSCL astrophysical motivated projects GroupProject Astrophysics (H.Schatz)  -decay (r-process) Masses (r-process) p-resonances (rp-process) HIRA (B.Linch) Masses (rp-process) 2p-correlations Isospin-EOS (Neutron Stars) LEBIT (G.Bollen, D.Morrisey) Masses (rp-process) Gas cell stopper (Reaccelerated beams) S800 (R.Zeger) (CE-reactions SNeI, II)

67. Jorge Pereira, INPC 2007 (Pearson, et al. 1996) An overview of the present situation of Nuclear Astrophysics at NSCL Group / PeopleProjects Senior researchers (Faculty/Staff) Post-docsGraduatesUndergraduates Astrophysics (H.Schatz) 4  353 HIRA (B.Linch) 22240 S800 (R.Zenger, S.Austin) 32200 Beta (P.Mantica) 11110 4 Groups8 Post-docs 10 Exp. Projects10 Graduates 6 Faculty/Staff 3 Undergraduates Clearly NSCL is a natural facility to cover an extensive range of different topics in Nuclear Astrophysics