[Mesa-users] Be9 burning

[Masanobu Kunitomo]

Dear MESA users,

I am working on solar models and trying to see the evolution of the Be9 abundance. Be9 should be burned at around 3.5 MK (e.g., Pinsonneault 1997) but the attached figure (1Msun star at the solar age) shows that it’s burned only in the core (> 1e7 K). 

I am using MESA ver. 12115 with the attached inlist files (based on Farag et al. 2020) w/ some modifications:
 add_isos(h3, be9, b10, b11, neut, li6)
 add_reaction(
    r_h1_be9_to_he4_li6
    r_he4_li6_to_h1_be9
    r_h1_be9_to_h2_he4_he4
    r_h2_he4_he4_to_h1_be9
    r_neut_be9_to_h3_li7
    r_h3_li7_to_neut_be9
    r_be9_to_neut_he4_he4
    r_neut_he4_he4_to_be9
    r_neut_b11_to_h3_be9
    r_h3_be9_to_neut_b11
    )

I tried both choices of “rates_preference” (i.e., both NACRE and jina) but found no difference. I am not sure what is wrong/missing. Does anyone know how to calculate the Be9 abundance?

Thank you in advance for any help.

Best regards,
Masanobu

--
Masanobu Kunitomo, Ph.D.
Department of Physics, Kurume University
67 Asahi-machi, Kurume, Fukuoka 830-0011, Japan
* Visiting researcher at Observatoire de la Côte d’Azur (Nov 2023–Oct 2024)
Email: kunitomo.masanobu at gmail.com


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