[mesa-users] Question with the binary module

[Kuo-Chuan Pan]

Dear Robert,

Thank you very much for your suggestion.
I have tried including initial rotations, but it doesn’t change the circularisation before the first RLOF.
According to Belczynski’s paper, the orbit should circularised before the RLOF.

Best regards,
Kuo-Chuan


On Apr 15, 2016, at 2:04 PM, Robert Farmer <rjfarmer at asu.edu<mailto:rjfarmer at asu.edu>> wrote:

Hi
I've not tried tidal syncs, but whats happens if you turn on rotation for the two stars in inlist1 and inlist2, and set some initial rotation rate?

See http://mesa.sourceforge.net/star_job_defaults.html#rotation_controls for the available options. Or look at the binary_with_rot inlists from the mesa3 paper http://mesastar.org/results/mesa-iii-instrument-paper-inlists

Rob

On Fri, Apr 15, 2016 at 9:31 AM, Kuo-Chuan Pan <kuo-chuan.pan at unibas.ch<mailto:kuo-chuan.pan at unibas.ch>> wrote:
Dear MESA users,

I have few problems with the tidal circularisation and the wind mass lost in the binary module.
I was trying to reproduce the binary evolution model that similar to the progenitor of GW 150914
in Belczynski et al. (2016; http://arxiv.org/abs/1602.04531v1 ) with MESA (version 8118).

In their paper (fig 1 in  http://arxiv.org/abs/1602.04531v1 ), the progenitor was a (96.2 + 60,2 msun)
binary with z= 3% z_sun. The initial binary separation is 2463 Rsun and eccentricity e=0.15.

I have included tidal circularisation, synchronisation, and mass lost due to “Nieuwenhuijzen” scheme
for cool wind and “Kudritzki” for hot wind. By playing around the wind parameters, I could reproduce
the mass of both stars at the first RLOF (stage 2 in Fig 1 in Belczynski  et al. 2016).
However, I couldn’t reproduce the evolution time (t=3.5445 Myr), binary separation (a=2140 Rsun),
and eccentricity (e=0) as in the paper.

In my run (version 8118 ,see attached inlist), the first RLOF happens at t=2.66 Myr (=model number 164),
and the binary separation is a=2530 Rsun (e~0.15). As you can seen in my attached figure fig_eccentricity.png,
the tidal circularisation did almost nothing (I have tried circa_type_* = “Hut_rad” and “Hut_conv”) before the first RLOF
(at model number =164). The binary separation seems increased (due to the wind) but not shrink as in the paper.
If I turned off winds, there is almost no mass-lost before the first RLOF and no changes in the eccentricity.

I was wondering if anyone could give me some suggestions to reproduce the results at the first RLOF in the paper.

Many thanks,
Kuo-Chuan




<fig_eccentricity.png>
<fig_mass.png>
<fig_rl_relative_1.png>
<fig_separation.png>

------------------------------------------------------------------------------
Find and fix application performance issues faster with Applications Manager
Applications Manager provides deep performance insights into multiple tiers of
your business applications. It resolves application problems quickly and
reduces your MTTR. Get your free trial!
https://ad.doubleclick.net/ddm/clk/302982198;130105516;z
_______________________________________________
mesa-users mailing list
mesa-users at lists.sourceforge.net<mailto:mesa-users at lists.sourceforge.net>
https://lists.sourceforge.net/lists/listinfo/mesa-users



-------------- next part --------------
An HTML attachment was scrubbed...
URL: <https://lists.mesastar.org/pipermail/mesa-users/attachments/20160415/ac2ecc6f/attachment.html>