arindamsinha said:
- How did the concept of 'black holes' come up in the first place from GR, from a historical perspective? Was it the Schwarzschild solution/metric that gave rise to this concept? Or, was it something different?
...
Any insights on this will be very helpful, especially if there is a chronology of the development of this.
A good layman's chronology, from someone in the field, is in Kip Thorne's popular book
Black Holes and Time Warps. Going from memory since I don't have my copy handy, a quick chronology would, I think, look something like this (some of these items may only be mentioned very briefly, if at all, in the book, but this stuff has come up in a number of recent threads so it's fresh in my mind

):
1915: Einstein publishes his field equation.
1916: Schwarzschild discovers his solution, but he writes it in coordinates in which what we now know as the event horizon is at "r" = 0, not r = 2M. Consequently, he only discusses one region of the solution, whereas we now know (see below) that there are others as well.
1920's or early 30's: I believe Eddington, sometime during this period, came up with at least a version of what we now call Eddington-Finkelstein coordinates, but there was no follow-up for several decades. Also, sometime during this period, what we now call Painleve or Lemaitre coordinates were independently invented several times, but again there was no follow-up for several decades.
1939: Oppenheimer and Snyder publish their paper on gravitational collapse: first known model that includes collapsing matter and the vacuum region around it. However, they write their model in what we now call Schwarzschild exterior coordinates (*not* the same coordinates that Schwarzschild himself used in his 1916 paper!), and the physical nature of the coordinate singularity at the horizon (r = 2M) is not fully understood.
1939: Einstein publishes a paper showing that no stationary configuration of matter can be in a stable equilibrium unless its radius is at least 9/4 M (i.e., at least 9/8 of the Schwarzschild radius corresponding to its mass). He believes that this shows that gravitational collapse cannot occur; our modern understanding is that it only shows that a collapsing object, such as the one that appears in the Oppenheimer-Snyder paper, can't be in a stable equilibrium once its radius is less than 9/4 M.
1957: Finkelstein publishes a paper deriving what we now call Eddington-Finkelstein coordinates, and arguing that his derivation shows that the Schwarzschild solution to the Einstein Field Equation must include a region inside the event horizon, because otherwise the solution is incomplete: geodesics reach the horizon in a finite proper time, and all physical invariants are finite there, so they can't just stop without violating the EFE.
1960: Kruskal discovers that the full, maximally extended Schwarzschild solution contains even *more* regions than Finkelstein had thought: a total of four. Two of these (exterior, and black hole interior) are those covered by Eddington-Finkelstein (and Painleve) coordinates. However, Kruskal shows, by the same sorts of arguments that Finkelstein used, that in the (idealized and not physically reasonable, according to the best current understanding) case of a spherically symmetric spacetime which is vacuum everywhere, the solution is incomplete unless a "white hole" region and a *second* exterior region are also added. (These regions do *not* appear in solutions such as the Oppenheimer-Snyder model when those solutions are completed; instead, portions of regions I and II are joined to a non-vacuum region containing the collapsing matter.)
1960's: The "golden age" of black hole research: new mathematical tools are developed to study the global properties of spacetimes (i.e., solutions to the EFE), and various singularity theorems are proved which show that, if classical GR is correct, gravitational collapse starting from some reasonable initial conditions *must* form an event horizon, a black hole, and a curvature singularity at r = 0. After this point the study of black holes became "mainstream" relativity physics.