1. On Non-Primordial Deuterium Production by Accelerated Particles by Tijana Prodanović Brian D. Fields University of Illinois at Urbana-Champaign

2. Why Should We Care about D? Epstein et al. ( 1976) – Deuterium only produced in Big Bang Monotonic decline!  can measure primordial abundance But variations in local ISM !? Mullan & Linsky (1998) say: Epstein et al. (1976) neglected radiative capture of n n + p  d +  capture  high p density  Flares can be significant sources of D Can they really?

3. The Plan Two ways to test ML: 1)Stick with the basic particle physics and see how many neutrons can flares make 2) predict a flux and look for 2.22 MeV  rays

4. Element Production in Flares Thick target model: spectrum of projectiles is modified – ionization energy losses Particle production via spallation i + j  l + … (eg. p+  n +…) Projectile spectrum reasonable (solar) s  4  1 Results: n/p  1 but 6 Li/ (n+d)  500 ( 6 Li/ d ) solar making d overproduces 6 Li

5. Gamma-Ray Constraint Radiative capture: 2.223 MeV  ray intensity : Expected lower limit (Galactic d destruction = production): I  > 5  10 -2 cm -2 sec -1 sr -1 But we see : I  < 5  10 -4 cm -2 sec -1 sr -1 Expect: But we see: McConnell et al. (1998 ) IR image by COBE (K giants)

6. Conclusion Flares do not produce much more n’s than d, and they also produce enough 6 Li  Epstein et al. (1976) argument holds! From COMPTEL we see what flare stars do: Not even clumps of flare stars can be the answer to local deuterium variations