# When is Newtonian physics in curved coordinates sufficient for GR?

A free particle Lagrangian in a 3D curvilinear coordinate system can be written as an inner product with the metric $$g$$: $$L = \frac{1}{2}m\sum_{i,j=1}^3v^ig_{ij}v^j.$$

This equation was taught to me in the context of curved coordinate systems that can be transformed to be flat, for example polar coordinates. However, it seems awfully tempting to take a "fundamentally curved" metric from GR, like the Schwarzschild metric, to use in this equation. I know that even in flat space, this will give me the wrong answer if the velocity gets near $$c$$. However, so long as $$|v| \ll c$$, will there be any problems in treating it this way? What must be true about the coordinate system and the dynamics of the system in order for this scheme to work?

• Isn't the whole point of the classical limit that the EoMs for $v \ll c$ look like they come from your Lagrangian plus an extra term that looks like a gravitational potential? Jun 19, 2020 at 20:02
• Jun 19, 2020 at 21:54
• J. Wambsganss in arxiv.org/abs/astro-ph/9812021 treats gravitational lensing as (perturbative?) quasi-Newtonian gravitational field on the flat background Minkowski spacetime. While I understand the approach, or at the least hope I do, I'm not sure I grok the endgame. Didactic? Simplifying calculation? But this seems relevant to your question, if I understand it, so maybe that paper would be helpful. Jun 19, 2020 at 23:57

$$L = \frac12 m (\dot{r}^2 + r^2 \dot{\theta}^2 + r^2 \sin^2\theta\, \dot{\varphi}^2) + \frac{GmM}{r} \frac{\dot{r}^2}{c^2}$$
$$L = \frac12 m (\dot{r}^2 + r^2 \dot{\theta}^2 + r^2 \sin^2\theta\, \dot{\varphi}^2) + \frac{GmM}{r}.$$