Relativistic Milne-Eddington Type Solutions with a Variable Eddington Factor for Relativistic Spherical Winds

<table>Comoving luminosity for relativistic spherical flows in the RE case without heating and cooling. The values of <svg height="13.425" id="M119" style="vertical-align:-2.29482pt" version="1.1" viewbox="0 0 8.8500004 13.425" width="8.8500004" xmlns="http://www.w3.org/2000/svg">
<g transform="matrix(1.25,0,0,-1.25,0,13.425)">
<g transform="translate(72,-61.26)">
<text transform="matrix(1,0,0,-1,-71.95,63.6)">
<tspan style="font-size: 12.50px; " x="0" y="0">𝛽</tspan>
</text>
</g>
</g>
</svg> are from 0 to 0.9 in steps of 0.1 from top to bottom. The optical depth <svg height="10.825" id="M120" style="vertical-align:-3.22281pt" version="1.1" viewbox="0 0 13.6125 10.825" width="13.6125" xmlns="http://www.w3.org/2000/svg">
<g transform="matrix(1.25,0,0,-1.25,0,10.825)">
<g transform="translate(72,-63.34)">
<text transform="matrix(1,0,0,-1,-71.95,66.6)">
<tspan style="font-size: 12.50px; " x="0" y="0">𝜏</tspan>
</text>
<text transform="matrix(1,0,0,-1,-65.55,63.47)">
<tspan style="font-size: 8.75px; " x="0" y="0">c</tspan>
</text>
</g>
</g>
</svg> at the core radius is set to be 10.</table>

Advances in Astronomy

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Figure 2

Figure 2: Relativistic Milne-Eddington Type Solutions with a Variable Eddington Factor for Relativistic Spherical Winds 