1. Nuclear Astrophysics ARUNA Workshop, Notre Dame, IN Carl R. Brune Ohio University, Athens Ohio June 12-13, 2014

2. Beam Swinger Neutron Time-of-Flight Facility at Ohio University Swinger Magnet (-4°   lab  158°) 30-meter TOF Tunnel Edwards Accelerator Laboratory Cs Sputter Source Duoplasmatron He Source 4.5-MV T-shaped tandem Target chamber

3. Neutron Time-of-Flight Technique 24 Mg + 3 He  26 Si(*) + n Beam ( 3 He) neutron detector Target ( 24 Mg) neutron flight path (≤30m) time of flight  neutron energy kinematics  E x in 26 Si  t ≈ 2 ns long flight path, low E n desirable NE-213 scintillator  neutron / gamma discrimination Excellent energy resolution achievable (10 keV) !

4. Neutron Energy Spectra (Y. Parpottas) 24 Mg( 3 He,n) 26 Si(*) full spectra Key Result Mirror nucleus leads us to expect 3 + and 0 + in this region.

5. 16 O( 3 He,n) 18 Ne (Y. Parpottas) Neutron Energy (MeV)  (4.527) = 17(4) keV

6. Additional Considerations Charged-Particle or Gamma Coincidence (Sergio Almarez-Calderon et al.) Future need: more intense 3 He/α sources Specific cases: - 19 Ne via 19 F(p,n) (for 18 F+p) - 42 Ti via 40 Ca( 3 He,n) for 41 Ti(p,γ) 42 Ti Other Nuclear Astrophysics Projects: Sub-coulomb transfer reactions Statistical model studies