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Published equation contexts

Φ=G(nobs)−G(neq)\Phi = G(\mathbf{n}_{\mathrm{obs}}) - G(\mathbf{n}_{\mathrm{eq}})

Why this formula appears here

If no gas can be trusted individually, the natural move is to look for a property of the whole atmosphere. The most general candidate is thermodynamic disequilibrium: life is a persistent chemical engine, so a biosphere should hold its planet’s atmosphere away from the composition it would relax to if all permitted reactions ran to completion. The quantity is the available Gibbs energy — the difference between the free energy of the observed composition and that of its equilibrium state at the same elemental abundances, temperature and pressure: Φ=G(nobs)−G(neq)\Phi = G(\mathbf{n}_{\mathrm{obs}}) - G(\mathbf{n}_{\mathrm{eq}}). Krissansen-Totton, Olson and Catling computed this across Earth history and reported values that make the appeal obvious and…

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Published contexts (1)

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Φ=G(nobs)−G(neq).\Phi = G(\mathbf{n}_{\mathrm{obs}}) - G(\mathbf{n}_{\mathrm{eq}}).

Equation 1 · Origins & Astrobiology

What a Biosignature Has to Rule Out

This equation states an equality: the expressions on both sides have the same value under the article’s assumptions.

If no gas can be trusted individually, the natural move is to look for a property of the whole atmosphere. The most general candidate is thermodynamic disequilibrium: life is a persistent chemical engine, so a biosphere should hold its planet’s atmosphere away from the composition it would relax to if all permitted reactions ran to completion. The quantity is the available Gibbs energy — the difference between the free energy of the observed composition and that of its equilibrium state at the same elemental abundances, temperature and pressure: Φ=G(nobs)−G(neq)\Phi = G(\mathbf{n}_{\mathrm{obs}}) - G(\mathbf{n}_{\mathrm{eq}}). Krissansen-Totton, Olson and Catling computed this across Earth history and reported values that make the appeal obvious and…

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