MESA and dStar Results From the Meisel Group

Contact: Zach Meisel (email: meisel@ohio.edu, Ohio University)

Overview

This is a repository of inputs and results from MESA and dStar calculations performed by Zach Meisel and/or his research group at Ohio University. For more information about MESA, visit the MESA Marketplace and the MESA sourceforge page. For more information about dStar, vist the Astrophysics Source Code Library record ascl:1505.034 and Ed Brown's github page.

Please cite the relevant paper if you use these results for a publication. If it's not clear what the relevant paper is, please contact me.


X-ray Burst Materials

Papers to Cite:
  • Z. Meisel, "Consistent Modeling of GS 1826-24 X-Ray Bursts for Multiple Accretion Rates Demonstrates the Possibility to Constrain rp-process Reaction Rates", Astrophysical Journal 860, 147 (2018).
  • Z. Meisel, G. Merz, S. Medvid, "Influence of Nuclear Reaction Rate Uncertainties on Neutron Star Properties Extracted from X-ray Burst Model-Observation Comparisons", Astrophysical Journal, 872, 84 (2019).

Contributors: Zach Meisel, Grant Merz, Sophia Medvid

General Comments:
If you want to try your own hand at MESA bursts, but don't have much experience, see the MESA page to get started, Ed Brown's MESA 2013 summer school lecture on creating a neutron star envelope, and Andrew Cumming's MESA 2015 summer school lecture on X-ray burst calculations.

You may want to compare the results shown here to the KEPLER burst library and/or the Reference burst library from Monash.

Grid a:
This table contains results from a grid of bursts intended to approximate GS1826-24, or for similar conditions. The model names are ma#, where `m' is for MESA, `a' is for this grid of bursts, and the number is the burst variation number.
You can see the averaged burst light curves (with comparable Kepler bursts for reference) here.

The MESA inputs which can be used to reproduce these calculations can be downloaded in a zip file (35Mb) by clicking on this link.

The profiles (data vs depth) for every timestep of the 20th burst from model ma6 can be downloaded as a tgz file (6Gb, extract via tar -xzf) by clicking on this link. Burst ignition occurs at profile 50. Profile 180 is 128 seconds after ignition, which is around the time all nuclear burning (aside from decays) has ceased.

Model H Mass Frac [X] Metal Mass Frac [Z] Qbase [MeV/u] set [Edd] act. [Edd] Nbursts Special Rxn. Rates? LC Train Data Avg. LC Data
ma1 0.7 0.02 0.1 0.051 0.061 15 --- file file
ma2 0.7 0.02 0.1 0.069 0.079 14 --- file file
ma4 0.7 0.02 0.1 0.111 0.123 19 --- file file
ma5 0.7 0.02 0.1 0.150 0.164 20 --- file file
ma6 0.7 0.02 0.1 0.170 0.185 20 --- file file
ma7 0.7 0.01 0.1 0.051 0.065 9 --- file file
ma8 0.7 0.01 0.1 0.069 0.088 8 --- file file
ma9 0.7 0.01 0.1 0.079 0.090 16 --- file file
ma10 0.7 0.01 0.1 0.111 0.123 18 --- file file
ma11 0.7 0.01 0.1 0.150 0.164 19 --- file file
ma12 0.7 0.01 0.1 0.170 0.193 2 --- file file
ma13 0.7 0.01 1.0 0.051 0.105 2 --- file file
ma14 0.7 0.01 1.0 0.069 0.086 3 --- file file
ma15 0.7 0.01 1.0 0.079 0.102 3 --- file file
ma16 0.7 0.01 1.0 0.111 0.128 20 --- file file
ma17 0.7 0.01 1.0 0.150 0.171 25 --- file file
ma18 0.7 0.01 1.0 0.170 0.192 23 --- file file
ma19 0.7 0.02 0.1 0.051 0.061 13 15O(α,γ)/10 file file
ma20 0.7 0.02 0.1 0.069 0.091 5 15O(α,γ)/10 file file
ma21 0.7 0.02 0.1 0.079 0.091 14 15O(α,γ)/10 file file
ma22 0.7 0.02 0.1 0.111 0.140 6 15O(α,γ)/10 file file
ma23 0.7 0.02 0.1 0.150 0.166 18 15O(α,γ)/10 file file
ma24 0.7 0.02 0.1 0.170 0.187 18 15O(α,γ)/10 file file
ma25 0.7 0.01 0.1 0.051 0.102 1 15O(α,γ)/10 file file
ma26 0.7 0.01 0.1 0.069 0.096 4 15O(α,γ)/10 file file
ma27 0.7 0.01 0.1 0.079 0.149 1 15O(α,γ)/10 file file
ma28 0.7 0.01 0.1 0.111 0.126 10 15O(α,γ)/10 file file
ma29 0.7 0.01 0.1 0.150 0.166 15 15O(α,γ)/10 file file
ma30 0.7 0.01 0.1 0.170 0.191 4 15O(α,γ)/10 file file
ma31 0.7 0.01 1.0 0.051 0.067 2 15O(α,γ)/10 file file
ma32 0.7 0.01 1.0 0.069 0.095 5 15O(α,γ)/10 file file
ma33 0.7 0.01 1.0 0.079 0.097 11 15O(α,γ)/10 file file
ma34 0.7 0.01 1.0 0.111 0.140 1 15O(α,γ)/10 file file
ma35 0.7 0.01 1.0 0.150 0.175 6 15O(α,γ)/10 file file
ma36 0.7 0.01 1.0 0.170 0.195 15 15O(α,γ)/10 file file
ma37 0.7 0.01 0.5 0.051 0.066 10 --- file file
ma38 0.7 0.01 0.5 0.069 0.081 18 --- file file
ma39 0.7 0.01 0.5 0.079 0.092 17 --- file file
ma40 0.7 0.01 0.5 0.111 0.125 22 --- file file
ma41 0.7 0.01 0.5 0.150 0.174 3 --- file file
ma42 0.7 0.01 0.5 0.170 0.202 8 --- file file
ma43 0.7 0.01 0.5 0.051 0.062 12 15O(α,γ)/10 file file
ma44 0.7 0.01 0.5 0.069 0.082 5 15O(α,γ)/10 file file
ma45 0.7 0.01 0.5 0.079 0.115 3 15O(α,γ)/10 file file
ma46 0.7 0.01 0.5 0.111 0.128 11 15O(α,γ)/10 file file
ma49 0.7 0.01 0.1 0.111 0.123 17 15O(α,γ)/5 file file
ma50 0.7 0.01 0.1 0.150 0.165 14 15O(α,γ)/5 file file
ma51 0.7 0.01 0.1 0.170 0.186 18 15O(α,γ)/5 file file
ma52 0.7 0.02 0.1 0.111 0.123 19 15O(α,γ)/5 file file
ma53 0.7 0.02 0.1 0.150 0.165 18 15O(α,γ)/5 file file
ma54 0.7 0.02 0.1 0.170 0.186 19 15O(α,γ)/5 file file
ma55 0.7 0.02 0.5 0.051 0.083 3 15O(α,γ)/10 file file
ma56 0.7 0.02 0.5 0.069 0.093 7 15O(α,γ)/10 file file
ma57 0.7 0.02 0.5 0.079 0.115 4 15O(α,γ)/10 file file
ma58 0.7 0.02 0.5 0.111 0.129 5 15O(α,γ)/10 file file
ma59 0.7 0.02 0.5 0.150 0.170 7 15O(α,γ)/10 file file
ma60 0.7 0.02 0.5 0.170 0.194 5 15O(α,γ)/10 file file
ma61 0.7 0.02 1.0 0.051 0.075 3 15O(α,γ)/10 file file
ma62 0.7 0.02 1.0 0.069 0.092 7 15O(α,γ)/10 file file
ma63 0.7 0.02 1.0 0.079 0.095 8 15O(α,γ)/10 file file
ma64 0.7 0.02 1.0 0.111 0.130 1 15O(α,γ)/10 file file
ma65 0.7 0.02 1.0 0.150 0.173 6 15O(α,γ)/10 file file
ma66 0.7 0.02 1.0 0.170 0.197 5 15O(α,γ)/10 file file
ma67 0.7 0.02 1.0 0.051 0.064 13 15O(α,γ)/5 file file
ma68 0.7 0.02 1.0 0.069 0.126 3 15O(α,γ)/5 file file
ma69 0.7 0.02 1.0 0.079 0.094 13 15O(α,γ)/5 file file
ma70 0.7 0.02 1.0 0.111 0.162 4 15O(α,γ)/5 file file
ma71 0.7 0.02 1.0 0.150 0.171 19 15O(α,γ)/5 file file
ma72 0.7 0.02 1.0 0.170 0.197 6 15O(α,γ)/5 file file
ma73 0.75 0.02 0.1 0.051 0.061 15 --- file file
ma74 0.75 0.02 0.1 0.069 0.083 12 --- file file
ma77 0.75 0.02 0.1 0.150 0.169 4 --- file file
ma78 0.75 0.02 0.1 0.170 0.186 8 --- file file
ma79 0.75 0.02 1.0 0.051 0.078 6 --- file file
ma80 0.75 0.02 1.0 0.069 0.084 8 --- file file
ma81 0.75 0.02 1.0 0.079 0.098 5 --- file file
ma82 0.75 0.02 1.0 0.111 0.129 13 --- file file
ma83 0.75 0.02 1.0 0.150 0.170 26 --- file file
ma84 0.75 0.02 1.0 0.170 0.192 26 --- file file


Grid b:
This table contains results from a grid of bursts intended to approximate GS1826-24, or for similar conditions, while varying a number of reaction rates. The model names are mb#, where `m' is for MESA, `b' is for this grid of bursts, and the number is the burst variation number.
You can see the averaged burst light curves (with comparable Kepler bursts for reference) here.



Model X,Z,Q[MeV/u],ṁset Nbursts Rate Var. LC Train Data Avg. LC Data Ashes,X(A)
mb0 0.7,0.02,0.1,0.17 21 ReaclibV2.2 file file file
mb1 0.7,0.02,0.1,0.17 18 15O(α,γ)/10 file file file
mb2 0.7,0.02,0.1,0.17 21 59Cu(p,α)/100 file file file
mb3 0.7,0.02,0.1,0.17 19 59Cu(p,γ)/100 file file file
mb4 0.7,0.02,0.1,0.17 21 61Ga(p,γ)/100 file file file
mb5 0.7,0.02,0.1,0.17 20 22Mg(α,p)/10 file file file
mb6 0.7,0.02,0.1,0.17 12 14O(α,p)/10 file file file
mb7 0.7,0.02,0.1,0.17 21 23Al(p,γ)/30 file file file
mb8 0.7,0.02,0.1,0.17 19 18Ne(α,p)×30 file file file
mb9 0.7,0.02,0.1,0.17 20 63Ga(p,γ)/10 file file file
mb10 0.7,0.02,0.1,0.17 19 19F(p,α)×10 file file file
mb11 0.7,0.02,0.1,0.17 20 12C(α,γ)×1.25 file file file
mb12 0.7,0.02,0.1,0.17 20 26Si(α,p)×10 file file file
mb13 0.7,0.02,0.1,0.17 20 17F(α,p)×10 file file file
mb14 0.7,0.02,0.1,0.17 20 24Mg(α,γ)×10 file file file
mb15 0.7,0.02,0.1,0.17 20 57Cu(p,γ)/10 file file file
mb16 0.7,0.02,0.1,0.17 20 63Ga(p,α)/100 file file file
mb17 0.7,0.02,0.1,0.17 20 17F(p,γ)×6.33 file file file
mb18 0.7,0.02,0.1,0.17 21 40Sc(p,γ)/100 file file file
mb19 0.7,0.02,0.1,0.17 20 48Cr(p,γ)/100 file file file


Core Collapse Supernova Materials

Papers to cite:
  • S. Subedi, Z. Meisel, G. Merz, "Sensitivity of 44Ti and 56Ni production in core-collapse supernova shock-driven nucleosynthesis to nuclear reaction rate variations", Astrophysical Journal 898, 5 (2020).


Contributors: Zach Meisel, Shiv Subedi

General Comments:
The materials for this work are available on the MESA Marketplace. We followed the massive star evolution procedure of R. Farmer et al. ApJS 2016 and the CCSN modeling procedure of Paxton et al. ApJS 2015. The paper cited above contains details of which inlists to run and when, as well as modifications from the Farmer and Paxton works.


Crust Cooling Materials

Papers to cite:

Contributors: Zach Meisel, Sudhanva Lalit, Ed Brown

General Comments:
If you want to peform dStar calculations, the code (written by Ed Brown), can be downloaded from the Astrophysics Source Code Library as record ascl:1505.034. dStar is a neutron star thermal evolution code, originally based on the work presented in Brown and Cumming 2009. The dStar code itself is located on github and comes with a tutorial in the examples/ directory.

The following inlists are for calculations achieving a 12.31km radius 1.4 solar-mass mass neutron star (note the core mass and radius, not the total mass and radius, are specified in the inlist) using the crust-core transition pressures corresponding to the equations of state: APR, BL, GM1, and SLY4. These inlists roughly approximate the observed cooling of the source KS1731-26.


Please cite us!

For X-ray Bursts:
  • Z. Meisel, "Consistent Modeling of GS 1826-24 X-Ray Bursts for Multiple Accretion Rates Demonstrates the Possibility to Constrain rp-process Reaction Rates", Astrophysical Journal 860, 147 (2018).
  • Z. Meisel, G. Merz, S. Medvid, "Influence of Nuclear Reaction Rate Uncertainties on Neutron Star Properties Extracted from X-ray Burst Model-Observation Comparisons", Astrophysical Journal 872, 84 (2019).

For CCSN:
  • S. Subedi, Z. Meisel, G. Merz, "Sensitivity of 44Ti and 56Ni production in core-collapse supernova shock-driven nucleosynthesis to nuclear reaction rate variations", Astrophysical Journal 898, 5 (2020).

For Crust Cooling: