Hi All,

I hope you all made it home (roughly in time). As promised I list here a number of key ingredients of our codes that we would describe briefly. I also add some suggestions for a few figures that could give a lot of insight. Furthermore, I list at the end the things that can be changed very easily in our code, which should lead us to agree on a set of assumptions that we use for the comparison.

Please let me know which key ingredients I still miss and what you think about making the figures.

As a last point I wanted to come back to Jarrods position. Although he was not present at our discussion I think he is more involved than the other groups, so I would suggest to get him involved, but let me know if you think this would complicate matters.

I am looking forward to a (hopefully) fruitful comparison!

Cheers,
Gijs

------------
Key ingredients to give a (very) short description of:

1/ Method to determine mass transfer type (i.e. zeta's. mass ratio's etc.) Possible figures: regions of nuclear/thermal/dynamical mass transfer in primary mass - (log) separation space for q = 1, 0.5, 2

2/ Method to determine the amount of mass loss from the system during the different types of mass transfer (i.e. constant fraction, depending on thermal time scale accretor etc).

3/ Stellar wind mass loss for (super) giants and Wolf-Rayet stars Possible figure: initial mass - final (pre SN) mass plot for single stars and binaries (case B)

4/ Compact objects formation: initial mass - compact object mass relation, kicks, mass loss in black hole formation/fall back Possible figure: initial mass - compact object mass plot

5/ Magnetic braking and tidal evolution

------------
Easily adjustable ingredients in SeBa (Simon, please correct/complement):

Trivial (i.e. change of parameter)

• common envelope efficiency
• fraction of common envelope accreted by companion
• common envelope formalism (energy balance vs angular momentum balance)
• angular momentum of matter lost in non-conservative (dynamically stable) mass transfer
• neutron star kick velocity: Maxwellian, Paczynski type, delta function, no kick
• black hole kick: no kick or scaled with mass
• magnetic braking scaling
• Darwin-Riemann (tidal) instability constant: J_star > const * J_orbit
• circularization constant (i.e. circularization starts if a * (1 - e) < const * R_biggest_star)

Easy (i.e. change code a little)

• change of zeta's
• Wolf-Rayet and helium star stellar wind
• (super) giant stellar wind
• fraction of mass accreted in non conservative mass transfer