Because to OP is talking about "reference frames", they are most likely doing Newtonian physics and not actually doing GR. If they were doing GR, they would be talking about what metric they were using rather than about "reference frames". But I'll try to answer the question both from a Newtonian and a GR perspective. I expect that the full GR treatment will be too brief to be useful, but I hope to at least convey something about the "flavor" of the treatment.
From a Newtonian perspective, the reference frame one uses is essentially heliocentric. The heliocentric idea occured historically before Newton - with Copernicus, Kepler, and Gallileo being important authors. Rather than get the details wrong, I'll mention that Newton came later.
A better degree of approxmation would anchor the reference frame used for Newtonian calculations to the barycenter of the solar system rather than the sun, but I won't go into this refinement.
The basic equations of motion used in the Newtonian approach would be F=ma, with the gravitational force F being equal to GmM/r^2.
The basic equations used for the GR approach would be the geodesic equations. See
https://en.wikipedia.org/wiki/Solving_the_geodesic_equations. Geodesics are still an approximation in GR, but they are a good one - actual planets would depart from the geodesic for various reasons, including the emission of gravitational waves, and numerically larger effects such as the transfer of momentum to the Earth from solar radiation.
The basic geodesic equations would be
$$\frac{d^2 x^a}{d \tau^2} + \Gamma^a{}_{bc} \frac{dx^b}{d\tau} \frac{dx^c}{d\tau} = 0 \quad \Gamma^a{}_{bc} = \frac{1}{2} \partial g^{ad} \left( \frac{\partial g_{cd} }{\partial x^b} + \frac{\partial g_{bd} }{\partial x^c} - \frac{\partial g_{bc} }{\partial x^d} \right)$$
F=ma is not used, thats the Newtonian approach - the GR approach is fundamentally different and based on different concepts.
These equations are probably not familiar to the OP and would require some study to disentangle enough to actually use. Among other issues one would need famiiartiy with the convention of summation over repeated indicies. The point of the equations though is that they are differential equations (just like the ones from the Newtonian equations) derived from the metric, ##g_{ab}##. So, specifying the metric gives the solutions for the orbits of test masses.
While there are several metrics one could use, the Schwarzschild metric is the usual choice. There are some alternatives one might use, but getting into the details is beyond the scope of what I want to write here.
There are a number of refinements that can be made to the GR analysis that I've outlined here - it has made some approximations, but this post is already long enough. The point is that it should not be at all surprising that we use a sun-centered coordinate system to work the problem in GR just as we did with Newton. The Sun, being the most massive object in the solar system, tends to dominate the physics. Again, refinements of this heliocentric model are possible in GR, but it would take an extended discussion to clarify this, I'll just drop the words "PPN approximations" and leave it at that.
I'll add one more thing. Rather than attempt to learn enough about GR to compute the orbits, it would be simplest to just assume that it gives a circular orbit. Then one can concentrate on the original question, by computing and integrating the proper time ##\tau## for the orbital motion, the "hovering" motion, and even answering the question of what trajectory maximizes the age of the stay-at-home twin. Perhaps I should have started here, but I didn't - and it would be another thread to do this justice. Of course, some famliarity with the concept of what proper time is is needed - perhaps another thread might be needed, to explain what proper time is and why it answers the question, before we would go about computing it :(.