1. Reaction rates in the Laboratory Example I: 14 N(p,  ) 15 O stable target  can be measured directly: slowest reaction in the CNO cycle  Controls duration of hydrogen burning  Determines main sequence turnoff – glob. cluster ages but cross sections are extremely low:  Measure as low an energy as possible – then extrapolate to Gamow window Accelerator N-target  -ray detectors Proton beam vacuum beam line

2. beam of particles hits target at rest thickness d area A j,v assume thin target (unattenuated beam intensity throughout target) Reaction rate (per target nucleus): Total reaction rate (reactions per second) with n T : number density of target nuclei I =jA : beam number current (number of particles per second hitting the target) note: dn T is number of target nuclei per cm 2. Often the target thickness is specified in these terms. Calculating experimental event rates and yields

3. Events detected in experiment per second R det  is the detection efficiency and can accounts for: detector efficiency (fraction of particles hitting a detector that produce a signal that is registered) solid angle limitations absorption losses in materials energy losses that cause particles energies to slide below a detection threshold …

4. 00  -signature of resonance 6791 keV Direct gs capture ~7297 keV + E p Gamow window 0.1 GK: 91-97 keV 14 N(p,  ) level scheme

5. Gran Sasso Mountain scheme LUNA Laboratory Underground for Nuclear Astrophysics (Transparencies: F. Strieder http://www.jinaweb.org/events/tucson/Talk_Strieder.pdf) 1:1 Mio cosmic ray suppression

6. Spectra: above and under ground

7. Beschleuniger bild

8. Setup picture

9. Spectrum overall

10. Spectrum blowup

11. Results: Formicola et al. PLB 591 (2004) 61 Gamow Window New S(0)=1.7 +- 0.2 keVb (NACRE: 3.2 +- 0.8)

12. Resonance claim and TUNL disproof New Resonance ?

13. Effect that speculative resonance would have had

14. Example II: 21 Na(p,  ) 22 Mg problem: 21 Na is unstable (half-life 22.5 s) solution: radioactive beam experiment in inverse kinematics: 21Na + p  22Mg +  Accelerator I Accelerator 2 p beam thick 21Na production target ion source 21 Na beam hydrogen target  -detectors 22Mg products particle identification difficulty: beam intensity typically 10 7-11 1/s (compare with 100  A protons = 6x10 14 /s)  so far only succeeded in 2 cases: 13N(p,  ) at Louvain la Neuve and 21Na(p,  ) in TRIUMF (for capture reaction)

17. DRAGON @ TRIUMF

18. Result for 206 keV resonance: S. Bishop et al. Phys. Rev. Lett. 90 (2003) 2501 Results

19. Example III: 32 Cl(p,  ) 33 Ar Shell model calculations Herndl et al. Phys. Rev. C 52(1995)1078  proton width strongly energy dependent  rate strongly resonance energy dependent

20. H. Schatz NSCL Coupled Cyclotron Facility

21. Installation of D4 steel, Jul/2000

22. Fast radioactive beams at the NSCL: low beam intensities Impure, mixed beams high energies (80-100 MeV per nucleon) (astrophysical rates at 1-2 MeV per nucleon)  great for indirect techniques Coulomb breakup Transfer reactions Decay studies …

23. Focal plane: identify 33Ar S800 Spectrometer at NSCL: Plastic target Radioactive 34 Ar beam 84 MeV/u T 1/2 =844 ms (from 150 MeV/u 36 Ar) 33 Ar 34 Ar SEGA Ge array (18 Detectors) Beam blocker D. Bazin R. Clement A. Cole A. Gade T. Glasmacher B. Lynch W. Mueller H. Schatz B. Sherrill M. VanGoethem M. Wallace H. Schatz Setup People: d Plastic 34Ar 33Ar excited 34 Ar

24. SEGA Ge-array S800 Spectrometer

25. x10000 uncertainty shell model only  -rays from predicted 3.97 MeV state Doppler corrected  -rays in coincidence with 33Ar in S800 focal plane: 33 Ar level energies measured: 3819(4) keV (150 keV below SM) 3456(6) keV (104 keV below SM) 33 Ar level energies measured: 3819(4) keV (150 keV below SM) 3456(6) keV (104 keV below SM) H. Schatz reaction rate (cm 3 /s/mole) temperature (GK) x 3 uncertainty with experimental data stellar reaction rate New 32 Cl(p,  ) 33 Ar rate – Clement et al. PRL 92 (2004) 2502 Typical X-ray burst temperatures

26. NSCL Plans: facility for reaccelerated low energy beams Strawman layout created before workshop – space requirement confirmed, did not discuss details Low energy area 0.15-3 MeV/u gas jet target recoil separator special  and particle detection systems High energy area would also be used by astrophysics community probably in line with needs of nuclear physics community

27. >10 8 10 7-8 10 6-7 10 5-6 10 4-5 10 2-4 Rates in pps Science with CCF reaccelerated beams direct (p,  ) direct (p,  ) or ( ,p) transfer (p,p), some transfer Capabilities: sufficient beam intensities for many important measurements all beams available once system commissioned probably very good beam purity none of the measurements identified can be performed at another facility as of now Up to here: For indirect measurements: many For direct measurements: some important rates and p-process …

28. Future ISF Upgrade Options

29. Upgrade Option 1: ISF NSCL-Site Upgrade Detail Space for Front End Linac Linac Tunnel Coupling Line from K1200 to Linac RF Fragment Separator Cyc-Stopper, LE Separator Trapping, Laser Spectroscopy Sweeper MoNA SEE-Line Reaccelerator (12 MeV/nucleon) Low Energy Arena Production Target S800 Reconfigured A1900

30. 10 8-9 10 7-8 10 6-7 10 5-6 10 4-5 10 2-4 Rates in pps 10 9-10 10 >10 Science with reaccelerated beams at future ISF facility All reaction rates up to ~Ti can be directly measured most reaction rates up to ~Sr can be directly measured All reaction rates can be indirectly measured including 72 Kr waiting point  Very strong nuclear astrophysics science case Direct measurements for many (  ) reactions in p-process