1) What should/can be modelled in which dimension 1/2/3D?
- H-ingestion into He-burning shells in both massive, AGB stars and accreting WDs to be modelled in 3D.
- Model advanced burning shells/Si-burning in 3D (thermal/radiative effects small/negligible)
- Link to observational constraints crucial but difficult: to be done via 1D models
2) Input Physics/unsolved problems:
What is the impact of binarity/magnetic fields on SE?
- Improvement in interplay between rotation and magnetic fields needed:
- - Asteroseismology --> New braking process needed for red giant
- - WDs/NSs rotation rates slower than models predict
- - combine constraints from boosted weak and main s process
- Mass loss uncertainties: close to Eddington limit, LBV/RSG large. Hard to make progress on this point
- How to explain odd-Z elements observational constraints?
Neutron excess (induced by rotation) can help, even for elements between silicon and iron
test with one zone calculation/full star models
3) Low and intermediate mass stars:
- Investigate convective boundary mixing below and above He-burning thermal pulse driven convective zone --> carbon content in intershell
- Investigate the impact of rotation+magnetic fields on the carbon-13 pocket --> size of carbon-13 pocket
- Gather observational constraints (WD rotation rate, elemental abundance ratios)
- Investigate the importance of the i-process: How frequent is it? Could it also occur in massive stars?
- Model accretion phase towards type Ia SNe. How difficult is it to reach Chandrasekhar mass in the single degenerate scenario?
- - n-capture nucleosynthesis to determine if SNIa can contribute to p nuclei.
4) Priority list for reaction rates (re-)measurement:
- Charged-particle reactions: 12C(a,g),22Ne(a,n)/(a,g),17O(a,g)/(a,n), n-captures on e.g. Si28-30 for grains, ?
- Investigate molecule condensation and dust production in SNe.
Link to SN theme:
- Determine what level of asymmetry would affect SN explosions
- Provide progenitor models with and without rotation, magnetic fields and binary effects
- Determine what are reasonable rotation/B-field initial conditions for MHD simulations