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Now we even try to discuss GR, where several posters in this thread still struggle with SR, and this most due to the fact that some still insist on using outdated concepts. Unfortunately even Feynman did so in the famous Feynman lectures, which are among my most highly favored general theory books, but in this point they are bad. There are many excellent books of physicists as eminent as Feynman that contain unfortunate approaches that do not help students but confuse them. That happens to any textbook writer from time to time. That's why one should read not only one book but many.
The best way to avoid trouble with what's called "equivalence principle" you can, if you have the minimum of necessary math in order to do GR, formulate it in a very simple form:
Spacetime is a 4D-Lorentzian manifold (i.e., a pseudo-Riemannian space with the fundamental form of signature (1,3)). This implies that around any point ##x## there exists a map defining coordinates ##x^{\mu}## such that
$$g_{\mu \nu}(x) \mathrm{d} x^{\mu} \mathrm{d} x^{\nu} = \eta_{\mu \nu} \mathrm{d} x^{\mu} \mathrm{d} x^{\nu}.$$
Such frames are called Galileian and are the best approximation of inertial frames possible in the presence of gravity, which cannot be described adequately by special-relativistic models but only in GR. Physically they can be realized by free-falling bodies that can be considered pointlike. An example is the International Space Station, freely falling in the gravitational field of the Earth (solar system). To a very good approximation the astronauts do not observe gravity and thus are to a good approximation in such a local inertial (or Galilean) reference frame.
The best way to avoid trouble with what's called "equivalence principle" you can, if you have the minimum of necessary math in order to do GR, formulate it in a very simple form:
Spacetime is a 4D-Lorentzian manifold (i.e., a pseudo-Riemannian space with the fundamental form of signature (1,3)). This implies that around any point ##x## there exists a map defining coordinates ##x^{\mu}## such that
$$g_{\mu \nu}(x) \mathrm{d} x^{\mu} \mathrm{d} x^{\nu} = \eta_{\mu \nu} \mathrm{d} x^{\mu} \mathrm{d} x^{\nu}.$$
Such frames are called Galileian and are the best approximation of inertial frames possible in the presence of gravity, which cannot be described adequately by special-relativistic models but only in GR. Physically they can be realized by free-falling bodies that can be considered pointlike. An example is the International Space Station, freely falling in the gravitational field of the Earth (solar system). To a very good approximation the astronauts do not observe gravity and thus are to a good approximation in such a local inertial (or Galilean) reference frame.