- #1
Orion1
- 973
- 3
An interesting equation derived from Classical General Relativity:
Solar evaporation time:
[tex]\boxed{t_{ev} = \frac{ m_{\odot} c^2}{P_{\odot}}}[/tex]
[tex]m_{\odot} = 1.98892 \cdot 10^{30} \; \text{kg}[/tex] - Solar mass
[tex]P_{\odot} = 3.846 \cdot 10^{26} \; \text{W}[/tex] - Solar Luminosity
[tex]\boxed{t_{ev} = 1.473 \cdot 10^{13} \; \text{y}}[/tex]
Understanding a thermodynamic equation similar to this should provide an appreciation for how extraordinarily dynamic and stable our nearest star Sol really is.
Reference:
http://en.wikipedia.org/wiki/Sun"
http://en.wikipedia.org/wiki/Solar_mass"
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