JupyterHub-Resources/PHY134L
JupyterHub-Resources/PHY134L
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Maxwell Millar-Blanchaer 2024-05-05 21:39:08 -07:00
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Lab_6/Lab_6.ipynb
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@ -51,7 +51,7 @@
"source": [
"For a quick introduction to (or refresher on) many of the basic notions, see [here](http://www.tim-thompson.com/hr.html). \n",
"\n",
"For a more quantitative picture of stellar evolution, consider the files ```evol_M0.8.dat```, ```evol_M1.0.dat```, ```evol_M1.3.dat```,```evol_M1.8.dat```, and ```evol_M2.6.dat. These contain evolutionary tracks for stars with compositions similar to the Sun's and with masses of 0.8, 1.0, 1.3, 1.8, and 2.5 times the mass of the\n",
"For a more quantitative picture of stellar evolution, consider the files ```evol_M0.8.dat```, ```evol_M1.0.dat```, ```evol_M1.3.dat```,```evol_M1.8.dat```, and ```evol_M2.6.dat```. These contain evolutionary tracks for stars with compositions similar to the Sun's and with masses of 0.8, 1.0, 1.3, 1.8, and 2.5 times the mass of the\n",
"Sun. The columns of the tables contain $\\log_{10}(Temperature~(K))$, $\\log_{10}(Luminosity~(solar~units)$), and Age (in Gyr). Notice (by opening one of the files in a text editor) that the range of ages in the various tables is fairly wide -- massive stars live for much shorter times than low-mass ones, though they are much more luminous. They burn brightly but burn out quickly."
]
},