Comments on the gravitational self-force problem

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I discuss the need for second-order self-force calculation (i.e., self-force of O(μ3)) to obtain gravitational waveforms to O(μ0) for extreme mass ratio binary inspiral. Next, I question this need for many astrophysical systems, for which other sources contribute to the orbital evolution at the same order as self-forces do, specifically spin orbit and spin spin interaction. Lastly, I discuss the possibility to obtain both a far-field and a near-field description of many interesting physical systems, with much insight into them, and surprising contexts in which self-forces may become important.

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