1. S & R Process Matt Penrice Astronomy 501 University of Victoria

2. Outline Overview S-Process R-Process Conclusion

3. Overview Neucleosythiesis beyond iron is driven primarily by neutron capture reactions If the time between neutron capture reactions is long compared to the time for beta decay to occur it is known as the s-process If the time between neutron capture reactions is short compared to the time for beta decay to occur it is known as the r-process

4. S-Process Because the neutron capture rate for the s- process is long compared to the beta decay rate, the s-process follows the valley of beta-stability Neutron capture continues along the stable isotopes of a given element until it reaches an unstable isotope where is subsequently beta decays into a new element

5. Abundance Change We can assume a constant Temp during a given neutron irradiation Can derive the time integrated neutron flux Using this we arrive at the rate of change of the abundance of a given nuclei

6. D.D. Clayton, WA. Fowler, TE. Hull & B.A. Zimmerman, Ann. Phys., 12,

7. Possible sites for s-process One candidate is the helium burning shell of a red giant One possible source for the neutrons is the reaction Helium shell flashes can also cause mixing which leads to the creation of carbon 13 and subsequently the neutron source reaction

8. R-Process Works similar to the s-process, but the neutron density is much higher so the neutron capture rates are much higher than beta decay rates Rapid accumulation of neutrons occurs until the neutron binding energy approaches zero. This occurs when the photodisintegration rate equals the neutron capture process The nuclei must wait until a beta decay occurs before continuing with neutron capture

9. Time dependence of abundances The abundances are characterized by nuclear charge, below is an equation for a given waiting point Lamb = decay rate of isotope (charge) at time t The equation reaches a point of equilibrium at Therefore N z abundances correlate with the beta-decay lifetimes at the waiting points

10. Alan P. Dickin Radiogenic Isotope Geology

11. Highlights of figure Magic neutron numbers N=50,82,126 These neucli have higher then average beta decay time and build up to relatively high abundances The r-process is terminated by neutron induced fission The fission reaction cycles material back into the process

12. R-Process The r-process occurs in unstable nuclei which are extremely difficult to work with in the laboratory. This gives rise to large uncertainty in calculations Possible sites for the r-process are supernova and other extreme events where the condition for high neutron flux can be met

13. Conclusion For the s-process the beta decay rate is longer then the neutron capture rate, where as for the r-process the situation is reversed A possible site for the s-process is the helium shell of a red giant star A possible site for the r-process is a supernova Differences between s and r-proceces can be investigated by looking at isotopes which are produced in isolation from each other