User:Tohline/Apps/SMS

Rotating, Supermassive Stars

Here we draw upon the work of J. R. Bond, W. D. Arnett, & B. J. Carr (1984, ApJ, 380, 825; hereafter BAC84) who were among the first to seriously address the question of the fate of very massive (stellar) objects.

Equation of State

Our discussion of the equation of state (EOS) that was used by BAC84 draws on the terminology that has already been adopted in our introductory discussion of supplemental relations and closely parallels our review of the properties of the envelope that E. A. Milne (1930, MNRAS, 91, 4) used to construct a bipolytropic sphere.

Ignoring the component due to a degenerate electron gas, <math>~P_\mathrm{deg}</math>, the total gas pressure can be expressed as the sum of two separate components: a component of ideal gas pressure, and a component of radiation pressure. That is, in BAC84 the total pressure is given by the expression,

<math>~P</math>

<math>~=</math>

<math>~P_\mathrm{gas} + P_\mathrm{rad} \, ,</math>

where,

Ideal Gas	Radiation
<math>~P_\mathrm{gas} = \frac{\Re}{\bar{\mu}} \rho T</math>	<math>~P_\mathrm{rad} = \frac{1}{3} a_\mathrm{rad} T^4</math>

Now, BAC84 define the rest-mass density in terms of the mean baryon mass, <math>~m_B</math>, via the expression, <math>~\rho = m_B n</math>, and write (see their equation 1),

<math>~P</math>

<math>~=</math>

<math>~Y_T n k T + \frac{1}{3}a_\mathrm{rad} T^4 \, .</math>

In converting from our notation to theirs we conclude, therefore, that,

<math>~\frac{\Re}{\bar{\mu}} (m_B n) T</math>	<math>~=</math>	<math>~Y_T n k T </math>
<math>~\Rightarrow ~~~~ Y_T </math>	<math>~=</math>	<math>~\frac{\Re}{k} \cdot \frac{m_B}{\bar{\mu}} \, .</math>

Following Milne (1930), we have defined the parameter, <math>~\beta</math>, as the ratio of gas pressure to total pressure. That is, in the context of BAC84, we have,

<math>\beta \equiv \frac{P_\mathrm{gas} }{P} \, ,</math>

in which case, also,

<math>\frac{P_\mathrm{rad}}{P} = 1-\beta </math>         and         <math>\frac{P_\mathrm{gas}}{P_\mathrm{rad}} = \frac{\beta}{1-\beta} \, .</math>

Using a different notation, BAC84 (see their equation 5) define <math>~\sigma</math> as the ratio of the radiation pressure to the gas pressure. Therefore, in converting from our notation to theirs we have,

<math>\sigma = \frac{1-\beta}{\beta} ~~~~\Rightarrow ~~~~ \beta = (1 + \sigma)^{-1} \, , </math>

as well as,

<math>\sigma = \frac{P_\mathrm{rad}}{P_\mathrm{gas}} = \frac{a_\mathrm{rad} T^3}{3} \cdot \frac{\bar\mu}{(\Re m_B)n} = \frac{a_\mathrm{rad} T^3}{3Y_T n k} \, ,</math>

which is precisely the definition provided in equation (5) of BAC84.

© 2014 - 2021 by Joel E. Tohline |   H_Book Home   |   YouTube   | Appendices: | Equations | Variables | References | Ramblings | Images | myphys.lsu | ADS | Recommended citation:   Tohline, Joel E. (2021), The Structure, Stability, & Dynamics of Self-Gravitating Fluids, a (MediaWiki-based) Vistrails.org publication, https://www.vistrails.org/index.php/User:Tohline/citation