<p>There is a rich variety of types of stellar evolution models. The modern model of a star is the spherically symmetric quasi-static gas assumed to be in local thermodynamic equilibrium (Chandrasekhar, 1967). There are four equations for how mass, pressure, temperature, and luminosity vary with radius as the star's thermal and radiative pressures support its self-gravity. Assumptions about convective and radiative energy transport, stability of nuclear burning, gas equations of state, gas composition, etc. and other processes must be accounted to model the evolution of a star through its life. A completely comprehensive stellar simulation is beyond computational ability. <a href="https://www.annualreviews.org/doi/abs/10.1146/annurev.astro.43.072103.150608?intcmp=trendmd" rel="nofollow noreferrer">Numerous types</a> of models exist: e.g., evolving stellar structure magneto-hydrodynamically, numerically evolving the stellar equations, interpolating between tables of known stellar properties derived from detailed simulations, using fitted formulae based on tabulated values, or some combination. Modern models incorporate the effects of rotation and mass loss on the star's
evolution.</p>
<p><a href="https://arxiv.org/abs/astro-ph/0001295" rel="nofollow noreferrer">This</a> seminal paper by Hurley <em>et al.</em> (2000) describes formulas that are fitted (and parameterized in terms of the initial stellar mass and metallicity) from numerically computed stellar evolutionary models. The tracks that you see in the HR diagram are made as a visual representation. See this paper for details about those stellar evolutionary numerical computations.</p>
<p>In their Discussion section 8, they describe how to use these parameterized formulas for fast-evaluations of single stellar evolution (which they implemented in the publicly available Single Stellar Evolution (SSE)). This was also <a href="https://ui.adsabs.harvard.edu/abs/2002MNRAS.329..897H/abstract" rel="nofollow noreferrer">implemented</a> in the rapid binary evolution simulation Binary Stellar Evolution (BSE), which has many modified successors now, for example <a href="https://arxiv.org/abs/1807.07568" rel="nofollow noreferrer">MOBSE</a>.</p>

CC BY-SA 4.0
2021-05-15T16:41:03.400Z
2021-05-15T18:35:43.433Z
2021-05-15T18:35:43.433Z
Daddy Kropotkin
<p>I have found countless images regarding the evolution of stars, plotted on an HR Diagram, like so (found on Wikipedia):</p>
<p><a href="https://i.sstatic.net/ejAis.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/ejAis.png" alt="enter image description here" /></a></p>
<p>Although this displays the time in each stage, it does not include any points plotted, relating to a timestep (i.e. 1 billion years), except for the zero age point. Is there anywhere I can find some <code>.csv</code> files that regard stellar evolution?</p>
<p><strong>NB:</strong> An example <code>.csv</code> file format would be <code>temperature, radius, mass, luminosity, time</code>.</p>

CC BY-SA 4.0
2021-05-15T01:10:14.400Z
Not quite what you want but [Star in a Box](https://starinabox.lco.global/) lets you view the evolution and start and stop it. There is a 'Data Table' link available which will give a CSV files (switch to 'Advanced' for more stages). Otherwise there is the [MESA Web](http://mesa-web.asu.edu/) front end to the MESA stellar evolution code might produce what you want
astrosnapper
CC BY-SA 4.0
2024-04-20T21:19:32.137Z
Almost all published stellar evolution models give you tables of exactly this.
ProfRob
<star><stellar-evolution><hr-diagram>
Graphing the evolution of stars on an HR diagram with timesteps
WarpPrime
# Graphing the evolution of stars on an HR diagram with timesteps

(Asked by: username_0 on 2021-05-15)

I have found countless images regarding the evolution of stars, plotted on an HR Diagram, like so (found on Wikipedia):

[![enter image description here](https://i.sstatic.net/ejAis.png)](https://i.sstatic.net/ejAis.png)

Although this displays the time in each stage, it does not include any points plotted, relating to a timestep (i.e. 1 billion years), except for the zero age point. Is there anywhere I can find some `.csv` files that regard stellar evolution?

**NB:** An example `.csv` file format would be `temperature, radius, mass, luminosity, time`.

**Tags:** star, stellar-evolution, hr-diagram
> **Comments:**
> **username_1**: Not quite what you want but [Star in a Box](https://starinabox.lco.global/) lets you view the evolution and start and stop it. There is a 'Data Table' link available which will give a CSV files (switch to 'Advanced' for more stages). Otherwise there is the [MESA Web](http://mesa-web.asu.edu/) front end to the MESA stellar evolution code might produce what you want  
> **username_2**: Almost all published stellar evolution models give you tables of exactly this.  

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## 1 answers

### Answer by username_3 on 2021-05-15. Score: 1

There is a rich variety of types of stellar evolution models. The modern model of a star is the spherically symmetric quasi-static gas assumed to be in local thermodynamic equilibrium (Chandrasekhar, 1967). There are four equations for how mass, pressure, temperature, and luminosity vary with radius as the star's thermal and radiative pressures support its self-gravity. Assumptions about convective and radiative energy transport, stability of nuclear burning, gas equations of state, gas composition, etc. and other processes must be accounted to model the evolution of a star through its life. A completely comprehensive stellar simulation is beyond computational ability. [Numerous types](https://www.annualreviews.org/doi/abs/10.1146/annurev.astro.43.072103.150608?intcmp=trendmd) of models exist: e.g., evolving stellar structure magneto-hydrodynamically, numerically evolving the stellar equations, interpolating between tables of known stellar properties derived from detailed simulations, using fitted formulae based on tabulated values, or some combination. Modern models incorporate the effects of rotation and mass loss on the star's
evolution.

[This](https://arxiv.org/abs/astro-ph/0001295) seminal paper by Hurley *et al.* (2000) describes formulas that are fitted (and parameterized in terms of the initial stellar mass and metallicity) from numerically computed stellar evolutionary models. The tracks that you see in the HR diagram are made as a visual representation. See this paper for details about those stellar evolutionary numerical computations.

In their Discussion section 8, they describe how to use these parameterized formulas for fast-evaluations of single stellar evolution (which they implemented in the publicly available Single Stellar Evolution (SSE)). This was also [implemented](https://ui.adsabs.harvard.edu/abs/2002MNRAS.329..897H/abstract) in the rapid binary evolution simulation Binary Stellar Evolution (BSE), which has many modified successors now, for example [MOBSE](https://arxiv.org/abs/1807.07568).


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