[mesa-users] Building stars via accretion with MESA

[Masanobu Kunitomo]

Dear Sergei,

I am not sure you remember me, but I met you in Heidelberg (PPVI) two years ago. I had lunch with you, Inutsuka-san (very fortunately, I am now a postdoc under Inutsuka-san!) and many Japanese. It was my honor to be with you then. It has been a long time.


Thank you very much for your interest in our work! All right, I will send you the preprint as soon as possible. It would take no longer than one month.

Thank you very much for the comments. I will read Bodenheimer 1974 and discuss this issue with Inutsuka-san. The possible 1Myr age difference on the starting points (2nd core formation) is important for the interpretation of age spread problem. And the mass of 2nd core affects the evolution significantly (e.g., Hosokawa et al. 2011; Baraffe, Vorobyov and Chabrier 2012), so its possible variation should be important. 

Again thank you very much for the comments!

Cheers,
Masanobu





> On Sep 9, 2015, at 13:58, Sergei Nayakshin <sn6985 at gmail.com> wrote:
> 
> Hi Masanobu,
> 
> I’d be quite interested to see the preprint, when it’s available, as the age of the star is also very important for planet formation (that I’m working on). One comment to make is that, for the second core of lowest masses, you may need to add the age of the second core to your age estimate of the star. Second cores of ~ 1 Jupiter masses go through H2 dissociation collapse after radiatively cooling for ~ 1 Myr (Bodenheimer 1974, but the result strongly depends on the dust opacity), so it may not be negligible. At 5-10 Jupiter masses and above, however, the cooling time is very short, of order 10^4 years, so then the second core formation is essentially instantaneous.
> 
> Cheers,
> Sergei.
> 
> 
>> On 8 Sep 2015, at 08:54, Masanobu Kunitomo <kunitomo.masanobu at c.mbox.nagoya-u.ac.jp <mailto:kunitomo.masanobu at c.mbox.nagoya-u.ac.jp>> wrote:
>> 
>> Dear Richard,
>> 
>> I will submit a paper on this subject shortly! Our work is similar to Baraffe et al. (2009, 2012) and Hosokawa et al. (2011), i.e., considering the accretion from a second core (~1-10 Mjup) to the final mass raging 0.05 to 1Msun and the heat injection by accretion parameterized with the “energy_routine” in src/run_star_extras.f. If you have any questions, I’ll be pleased to help.
>> 
>> Cheers,
>> Masanobu
>> 
>> 
>> --
>> Masanobu Kunitomo, Ph.D.
>> Department of Physics, Nagoya University
>> Furo-cho, Chikusa-ku, Nagoya, Aichi,  464-8602, Japan
>> Email: kunitomo.masanobu at c.mbox.nagoya-u.ac.jp <mailto:kunitomo.masanobu at c.mbox.nagoya-u.ac.jp>
>> 
>> 
>> 
>> 
>> 
>> 
>> 
>> 
>> 
>>> On Sep 8, 2015, at 16:14, Richard Townsend <rhtownsend at icloud.com <mailto:rhtownsend at icloud.com>> wrote:
>>> 
>>> Hi folks —
>>> 
>>> I’d like to see if I can use MESA to build up a star by accretion — basically, start with an adiabatic core with mass ~ Mjupiter, and then accrete mass (following some prescription) until it reaches its final mass and then contracts onto the main sequence.
>>> 
>>> Does anyone have any words of wisdom about this — things to watch out for with MESA, previous experiences with MESA or other codes, pointers?
>>> 
>>> Many thanks,
>>> 
>>> Rich
>>> 
>>> 
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