[mesa-users] MESA3 paper 7_binary_with_rot

Roni Waldman roni181066 at gmail.com
Wed Jun 17 09:58:14 EDT 2015 

Hi Pablo,

I ran the same masses with a period of 3 d.
Run ended with accretor overflowing RL.
Donor was 2.9 Msun, so quite close to the result of 3 Msun from Yoon.
Mass transfer efficiency was low again, at about 0.4.
I conclude that due mainly to the differences in the recipes for angular
momentum accretion, the behavior of the secondary is different, however the
effect on the final state of the donor is relatively small.
This is good enough for my purpose.

Roni

‫בתאריך יום ד׳, 17 ביוני 2015 ב-13:26 מאת ‪Pablo Marchant‬‏ <‪
pamarca at gmail.com‬‏>:‬

> Hi Roni, I know two possible sources that can cause differences.
>
> - Angular momentum accretion: If I remember correctly, the models you are
> comparing to calculate accreted angular momentum by integrating the
> expected trajectory of the accretion stream, instead of the simple
> approximation we use.
> - For angular momentum loss from mass loss, they consider the change from
> a simple isotropic wind produced by the companion, following the
> computations of Brookshaw & Tavani (1993).
>
> Before checking any of those though, id try a slightly different period.
> As tidal strength can be reduced dramatically with separation, I wonder
> what would be the outcome if you model a slighly more compact system
> (P_i=3.5 days for example). You might be sitting right at the boundary
> where accretion spinup dominates over tidal sync.
>
> On Wed, Jun 17, 2015 at 12:09 PM, Roni Waldman <roni181066 at gmail.com>
> wrote:
>
>> Hi,
>>
>> So here's an update of what I got.
>> I tried to reproduce the fiducial case in Yoon et al 2010, 18+17, initial
>> period 4d.
>> I used three different tidal sync recipes as will be described below.
>>
>> In all cases the primary ends as a 3.3 Msun WR, with a CO core of 1.9
>> Msun, compared to 3.79 and 2.14 respectively in the reference.
>> This might be due to differences either in the parameters of single star
>> evolution (convection, mass loss, etc. - these I kept unchanged from the
>> inlists in the MESA3 paper), or the treatment of binary evolution (or
>> combination of both).
>> The more striking difference is the fact that I got much less
>> conservative mass transfer, since the accretor quickly reaches breakup
>> rotation and stops accreting.
>> While Yoon et al got a 0.8 efficiency during case A, and 0.4 during case
>> AB, I got as follows:
>>
>> With the Hurley tidal sync recipe (MESA default):
>> During case A mass transfer the donor ends with 7.2 Msun, with mass
>> transfer efficiency of about 0.3.
>> During case AB mass transfer the donor ends with 4 Msun, and the mass
>> transfer efficiency is very low, about 0.03.
>>
>> With the Zahn tidal sync recipe (as supplied by Pablo):
>> During case A mass transfer the donor ends with 7.4 Msun, with mass
>> transfer efficiency of about 0.6.
>> During case AB mass transfer the donor ends with 4.1 Msun, and the mass
>> transfer efficiency is very low, about 0.08.
>>
>> With the Tassoul tidal sync recipe (as in Yoon et al 2010):
>> During case A mass transfer the donor ends with 7.2 Msun, with mass
>> transfer efficiency of about 0.25.
>> During case AB mass transfer the donor ends with 4.1 Msun, and the mass
>> transfer efficiency is about 0.2.
>>
>> Cheers,
>> Roni
>>
>>
>> ‫בתאריך יום ג׳, 16 ביוני 2015 ב-12:37 מאת ‪Matteo Cantiello‬‏ <‪
>> matteo at kitp.ucsb.edu‬‏>:‬
>>
>>> Cool,
>>> Very useful stuff, Roni.
>>> Let us know how it goes!
>>>
>>> -M
>>>
>>> Matteo Cantiello  |  http://matteocantiello.com/
>>> Associate Specialist in Astrophysics  | Kavli Institute for Theoretical
>>> Physics
>>> Chief Scientist and Board Member, Authorea  |  https://www.authorea.com/
>>>
>>> On Jun 16, 2015, at 9:38 AM, Roni Waldman <roni181066 at gmail.com> wrote:
>>>
>>> Sure, and I will.
>>>
>>> ‫בתאריך יום ג׳, 16 ביוני 2015 ב-10:28 מאת ‪Pablo Marchant‬‏ <‪
>>> pamarca at gmail.com‬‏>:‬
>>>
>>>> No, but the use_other_tsync option is there for you to play with it ;)
>>>>
>>>> On Tue, Jun 16, 2015 at 9:10 AM, Roni Waldman <roni181066 at gmail.com>
>>>> wrote:
>>>>
>>>>> Thanks Pablo.
>>>>> Do you happen to have a subroutine for the Tassoul formula?
>>>>> I'm trying to compare to Yoon et al 2010.
>>>>>
>>>>> Roni
>>>>>
>>>>> ‫בתאריך יום ג׳, 16 ביוני 2015 ב-10:04 מאת ‪Pablo Marchant‬‏ <‪
>>>>> pamarca at gmail.com‬‏>:‬
>>>>>
>>>>>> My bad, here it is. Will update the ones on mesastar
>>>>>>
>>>>>> On Tue, Jun 16, 2015 at 8:37 AM, Roni Waldman <roni181066 at gmail.com>
>>>>>> wrote:
>>>>>>
>>>>>>> Hi,
>>>>>>> More on this one.
>>>>>>> The inlist_project has:
>>>>>>>    ! use_other_tsync will use the Zahn timescale as defined in
>>>>>>> run_binary_extras.f
>>>>>>>    !use_other_tsync = .true.
>>>>>>>
>>>>>>> I dont't see any other_tsync in the default run_binary_extras.f,
>>>>>>> and there's no special run_binary_extras.f in the 7_binary_with_rot
>>>>>>> directory.
>>>>>>>
>>>>>>> Roni
>>>>>>>
>>>>>>>
>>>>>>> ‫בתאריך יום ב׳, 15 ביוני 2015 ב-21:11 מאת ‪Roni Waldman‬‏ <‪
>>>>>>> roni181066 at gmail.com‬‏>:‬
>>>>>>>
>>>>>>>> Same here.
>>>>>>>>
>>>>>>>> ‫בתאריך יום ב׳, 15 ביוני 2015 ב-19:37 מאת ‪Willie Strickland‬‏ <‪
>>>>>>>> cwskas at gmail.com‬‏>:‬
>>>>>>>>
>>>>>>>>> Thanks for the confirmation.  I thought they were probably for
>>>>>>>>> debugging, but didnt see obvious way to turn them off.
>>>>>>>>>
>>>>>>>>> Willie
>>>>>>>>>
>>>>>>>>>
>>>>>>>>> On Jun 15, 2015, at 11:13 AM, Pablo Marchant <pamarca at gmail.com>
>>>>>>>>> wrote:
>>>>>>>>>
>>>>>>>>> The w > w_crit messages come from the implicit method that
>>>>>>>>> increases the wind strength so the star does not evolve avobe critical
>>>>>>>>> rotation. Maybe they could be turned off, I mainly used that info for
>>>>>>>>> debugging. And your results are the same as mine.
>>>>>>>>>
>>>>>>>>> On Mon, Jun 15, 2015 at 5:59 PM, Willie Strickland <
>>>>>>>>> cwskas at gmail.com> wrote:
>>>>>>>>>
>>>>>>>>>> Did you get a lot of w > w_crit lines in the rotating one?  I got
>>>>>>>>>> the same results as you it sounds like, but had all these redo lines.
>>>>>>>>>>
>>>>>>>>>> 8,821 lines fix w > w_crit: bisect mdots and redo
>>>>>>>>>>      89 lines w > w_crit: revise mdot and redo
>>>>>>>>>>
>>>>>>>>>> My run finished at step 6429, age 1.254e7, 2.45 mass1, 18.7 mass2.
>>>>>>>>>>
>>>>>>>>>> accretor photosphere has reached its Roche Lobe
>>>>>>>>>>                                      accretor (r-rl)/rl
>>>>>>>>>>  6429    5.0151227593021562D-02
>>>>>>>>>>
>>>>>>>>>> Willie
>>>>>>>>>>
>>>>>>>>>>
>>>>>>>>>>
>>>>>>>>>>
>>>>>>>>>> On Jun 15, 2015, at 7:49 AM, Roni Waldman <roni181066 at gmail.com>
>>>>>>>>>> wrote:
>>>>>>>>>>
>>>>>>>>>> Hi Pablo,
>>>>>>>>>>
>>>>>>>>>> Oops... right, I put the file in the wrong place.
>>>>>>>>>> Rerunning, and let's see what happens.
>>>>>>>>>>
>>>>>>>>>> I also ran the rotating binary example.
>>>>>>>>>> Ended up with donor mass 2.45 Msun and accretor reaching
>>>>>>>>>> Roche-lobe.
>>>>>>>>>> Does that sound right?
>>>>>>>>>>
>>>>>>>>>> Thanks,
>>>>>>>>>> Roni
>>>>>>>>>>
>>>>>>>>>> ‫בתאריך יום ב׳, 15 ביוני 2015 ב-14:11 מאת ‪Pablo Marchant‬‏ <‪
>>>>>>>>>> pamarca at gmail.com‬‏>:‬
>>>>>>>>>>
>>>>>>>>>>> Roni, together with the inlists there is a run_star_extras.f
>>>>>>>>>>> provided (and in the inlists it is said that you need it). Are you using
>>>>>>>>>>> it? From you output it seems not. This implements the switch from a
>>>>>>>>>>> Kudritski wind to a Hamann one as described in Wellstein & Langer 1999.
>>>>>>>>>>>
>>>>>>>>>>> I guess changing this will make it consistent with that of the
>>>>>>>>>>> paper. Your model is doing some crazy things though.
>>>>>>>>>>>
>>>>>>>>>>> On Mon, Jun 15, 2015 at 9:06 AM, Roni Waldman <
>>>>>>>>>>> roni181066 at gmail.com> wrote:
>>>>>>>>>>>
>>>>>>>>>>>> Hi Pablo,
>>>>>>>>>>>> Too big for one email, will send several.
>>>>>>>>>>>> Thanks,
>>>>>>>>>>>> Roni
>>>>>>>>>>>>
>>>>>>>>>>>> ‫בתאריך יום א׳, 14 ביוני 2015 ב-22:55 מאת ‪Pablo Marchant‬‏ <‪
>>>>>>>>>>>> pamarca at gmail.com‬‏>:‬
>>>>>>>>>>>>
>>>>>>>>>>>>> Roni, can you send me your history.data for each star and
>>>>>>>>>>>>> binary_history.data to compare?
>>>>>>>>>>>>>
>>>>>>>>>>>>> On Sun, Jun 14, 2015 at 8:35 PM, Roni Waldman <
>>>>>>>>>>>>> roni181066 at gmail.com> wrote:
>>>>>>>>>>>>>
>>>>>>>>>>>>>> Hi,
>>>>>>>>>>>>>>
>>>>>>>>>>>>>> I downloaded the inlists of the MESA3 paper, and ran the
>>>>>>>>>>>>>> example 6_massive_binary, without changing anything in the inlists or the
>>>>>>>>>>>>>> code, version 7624.
>>>>>>>>>>>>>> The run ends with the donor having 2Msun, the accretor
>>>>>>>>>>>>>> filling its Roche-lobe, and the time steps being super small (1e-12).
>>>>>>>>>>>>>> This not what seems to happen in the paper.
>>>>>>>>>>>>>> Am I doing anything wrong?
>>>>>>>>>>>>>>
>>>>>>>>>>>>>> Roni
>>>>>>>>>>>>>>
>>>>>>>>>>>>>>
>>>>>>>>>>>>>>
>>>>>>>>>>>>>> ------------------------------------------------------------------------------
>>>>>>>>>>>>>>
>>>>>>>>>>>>>> _______________________________________________
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>>>>>>>>>>>>>> <https://lists.sourceforge.net/lists/listinfo/mesa-users>
>>>>>>>>>>>>>>
>>>>>>>>>>>>>>
>>>>>>>>>>>>>
>>>>>>>>>>>>>
>>>>>>>>>>>>> --
>>>>>>>>>>>>> Pablo Marchant Campos
>>>>>>>>>>>>> M.Sc on Astrophysics, Universidad Católica de Chile
>>>>>>>>>>>>> PhD student, Argelander-Institut für Astronomie
>>>>>>>>>>>>>
>>>>>>>>>>>>
>>>>>>>>>>>
>>>>>>>>>>>
>>>>>>>>>>> --
>>>>>>>>>>> Pablo Marchant Campos
>>>>>>>>>>> M.Sc on Astrophysics, Universidad Católica de Chile
>>>>>>>>>>> PhD student, Argelander-Institut für Astronomie
>>>>>>>>>>>
>>>>>>>>>> ------------------------------------------------------------
>>>>>>>>>> ------------------
>>>>>>>>>> _______________________________________________
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>>>>>>>>>> https://lists.sourceforge.net/lists/listinfo/mesa-users
>>>>>>>>>>
>>>>>>>>>>
>>>>>>>>>>
>>>>>>>>>
>>>>>>>>>
>>>>>>>>> --
>>>>>>>>> Pablo Marchant Campos
>>>>>>>>> M.Sc on Astrophysics, Universidad Católica de Chile
>>>>>>>>> PhD student, Argelander-Institut für Astronomie
>>>>>>>>>
>>>>>>>>>
>>>>>>>>>
>>>>>>>>> ------------------------------------------------------------------------------
>>>>>>>>> _______________________________________________
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>>>>>>>>> https://lists.sourceforge.net/lists/listinfo/mesa-users
>>>>>>>>>
>>>>>>>>
>>>>>>
>>>>>>
>>>>>> --
>>>>>> Pablo Marchant Campos
>>>>>> M.Sc on Astrophysics, Universidad Católica de Chile
>>>>>> PhD student, Argelander-Institut für Astronomie
>>>>>>
>>>>>
>>>>
>>>>
>>>> --
>>>> Pablo Marchant Campos
>>>> M.Sc on Astrophysics, Universidad Católica de Chile
>>>> PhD student, Argelander-Institut für Astronomie
>>>>
>>>
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>
>
> --
> Pablo Marchant Campos
> M.Sc on Astrophysics, Universidad Católica de Chile
> PhD student, Argelander-Institut für Astronomie
>
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