2.2 Other matter models2 The phenomena2 The phenomena

2.1 Case study: The spherically symmetric scalar field 

The system in which Christodoulou and Choptuik have studied gravitational collapse is the spherically symmetric massless, minimally coupled scalar field. It has the advantage of simplicity, while the scalar radiation propagating at the speed of light mimics gravitational waves. We describe the system, and Choptuik's results.

2.1.1 Spherical scalar field: Definition of the system

We consider a spherically symmetric, massless scalar field minimally coupled to general relativity. The Einstein equations are

  equation33

and the matter equation is

equation39

Note that the matter equation of motion is contained within the contracted Bianchi identities. Choptuik chose Schwarzschild-like coordinates

  equation41

where tex2html_wrap_inline2235 is the metric on the unit 2-sphere. This choice of coordinates is defined by the radius r giving the surface area of 2-spheres as tex2html_wrap_inline2239, and by t being orthogonal to r (polar-radial coordinates). One more condition is required to fix the coordinate completely. Choptuik chose tex2html_wrap_inline2245 at r =0, so that t is the proper time of the central observer.

In the auxiliary variables

equation44

the wave equation becomes a first-order system,

  equation49

In spherical symmetry there are four algebraically independent components of the Einstein equations. Of these, one is a linear combination of derivatives of the other and can be disregarded. The other three contain only first derivatives of the metric, namely tex2html_wrap_inline2251, tex2html_wrap_inline2253 and tex2html_wrap_inline2255 . Choptuik chose to use the equations giving tex2html_wrap_inline2253 and tex2html_wrap_inline2255 for his numerical scheme, so that only the scalar field is evolved, but the two metric coefficients are calculated from the matter at each new time step. (The main advantage of such a numerical scheme is its stability.) These two equations are

  equation67

  equation72

and they are, respectively, the Hamiltonian constraint and the slicing condition. These four first-order equations totally describe the system. For completeness, we also give the remaining Einstein equation,   equation78

2.1.2 Spherical scalar field: The black hole threshold

The free data for the system are the two functions tex2html_wrap_inline2261 and tex2html_wrap_inline2263 Popup Footnote . Choptuik investigated one-parameter families of such data by evolving the data for many different values of the parameter. (We generically call this parameter p). He examined a number of such families in this way. Some simple examples of such families are tex2html_wrap_inline2267 and a Gaussian for tex2html_wrap_inline2261, with the parameter p taken to be either the amplitude of the Gaussian, with the width and center fixed, or the width, with position and amplitude fixed, or the position, with width and amplitude fixed. For the amplitude sufficiently small, with width and center fixed, the scalar field will disperse, and for sufficiently large amplitude it will form a black hole. Generic one-parameter families behave in this way, but this is difficult to prove in generality. Christodoulou showed for the spherically symmetric scalar field system that data sufficiently weak in a well-defined way evolve to a Minkowski-like spacetime [44, 47], and that a class of sufficiently strong data forms a black hole [46].

But what happens in between? Choptuik found that in all 1-parameter families of initial data he investigated he could make arbitrarily small black holes by fine-tuning the parameter p close to the black hole threshold. An important fact is that there is nothing visibly special to the black hole threshold. One cannot tell that one given data set will form a black hole and another one infinitesimally close will not, short of evolving both for a sufficiently long time. ``Fine-tuning'' of p to the black hole threshold proceeds by bisection: Starting with two data sets one of which forms a black hole, try a third one in between along some one-parameter family linking the two, drop one of the old sets and repeat.

With p closer to tex2html_wrap_inline2221, the spacetime varies on ever smaller scales. The only limit was numerical resolution, and in order to push that limitation further away, Choptuik developed numerical techniques that recursively refine the numerical grid in spacetime regions where details arise on scales too small to be resolved properly. In the end, Choptuik could determine tex2html_wrap_inline2221 up to a relative precision of tex2html_wrap_inline2283, and make black holes as small as tex2html_wrap_inline2285 times the ADM mass of the spacetime. The power-law scaling (1Popup Equation) was obeyed from those smallest masses up to black hole masses of, for some families, 0.9 of the ADM mass, that is, over six orders of magnitude [38Jump To The Next Citation Point In The Article]. There were no families of initial data which did not show the universal critical solution and critical exponent. Choptuik therefore conjectured that tex2html_wrap_inline2289 is the same for all one-parameter families of smooth, asymptotically flat initial data that depend smoothly on the parameter, and that the approximate scaling law holds ever better for arbitrarily small tex2html_wrap_inline2291 .

Choptuik's results for individual 1-parameter families of data suggest that there is a smooth hypersurface in the (infinite-dimensional) phase space of smooth data which divides black hole from non-black hole data. Let P be any smooth scalar function on the space so that P =0 is the black hole threshold. Then, for any choice of P, there is a second smooth function C on the space so that the black hole mass as a function of the initial data is

equation90

The entire unsmoothness at the black hole threshold is now captured by the non-integer power. We should stress that this formulation of Choptuik's mass scaling result is not even a conjecture, as we have not stated on what function space it is supposed to hold. Nevertheless, considering 1-parameter families of initial data is only a tool for numerical investigations of the the infinite-dimensional space of initial data, and a convenient way of expressing analytic approximations.

Clearly a collapse spacetime which has ADM mass 1, but settles down to a black hole of mass (for example) tex2html_wrap_inline2285 has to show structure on very different scales. The same is true for a spacetime which is as close to the black hole threshold, but on the other side: The scalar wave contracts until curvature values of order tex2html_wrap_inline2303 are reached in a spacetime region of size tex2html_wrap_inline2285 before it starts to disperse. Choptuik found that all near-critical spacetimes, for all families of initial data, look the same in an intermediate region, that is they approximate one universal spacetime, which is also called the critical solution. This spacetime is scale-periodic in the sense that there is a value tex2html_wrap_inline2307 of t such that when we shift the origin of t to tex2html_wrap_inline2307, we have

  equation100

for all integer n and for tex2html_wrap_inline2233, and where Z stands for any one of a, tex2html_wrap_inline2323 or tex2html_wrap_inline2325 (and therefore also for tex2html_wrap_inline2327 or tex2html_wrap_inline2329). The accumulation point tex2html_wrap_inline2307 depends on the family, but the scale-periodic part of the near-critical solutions does not.

This result is sufficiently surprising to formulate it once more in a slightly different manner. Let us replace r and t by a pair of auxiliary variables such that one of them is the logarithm of an overall spacetime scale. A simple example is

  equation105

(tex2html_wrap_inline2337 has been defined so that it increases as t increases and approaches tex2html_wrap_inline2307 from below. It is useful to think of r, t and L as having dimension length in units c = G =1, and of x and tex2html_wrap_inline2337 as dimensionless.) Choptuik's observation, expressed in these coordinates, is that in any near-critical solution there is a spacetime region where the fields a, tex2html_wrap_inline2323 and tex2html_wrap_inline2325 are well approximated by their values in a universal solution, as

equation110

where the fields tex2html_wrap_inline2361, tex2html_wrap_inline2363 and tex2html_wrap_inline2365 of the critical solution have the property

equation112

The dimensionful constants tex2html_wrap_inline2307 and L depend on the particular one-parameter family of solutions, but the dimensionless critical fields tex2html_wrap_inline2361, tex2html_wrap_inline2363 and tex2html_wrap_inline2365, and in particular their dimensionless period tex2html_wrap_inline2377, are universal.

The evolution of near-critical initial data starts resembling the universal critical solution beginning at some length scale tex2html_wrap_inline2379 that is related (with some factor of order one) to the initial data scale. A slightly supercritical and a slightly subcritical solution from the same family (so that L and tex2html_wrap_inline2307 are the same) are practically indistinguishable until they have reached a very small scale where the one forms an apparent horizon, while the other starts dispersing. If a black hole is formed, its mass is related (with a factor of order one) to this scale, and so we have for the range tex2html_wrap_inline2385 of tex2html_wrap_inline2337 on which a near-critical solution approximates the universal one

  equation115

where the unknown factors of order one give rise to the unknown constant. As the critical solution is periodic in tex2html_wrap_inline2337 with period tex2html_wrap_inline2377 for the number N of scaling ``echos'' that are seen, we then have the expression

equation119

Note that this holds for both supercritical and subcritical solutions.

Choptuik's results have been repeated by a number of other authors. Gundlach, Price and Pullin [79] could verify the mass scaling law with a relatively simple code, due to the fact that it holds even quite far from criticality. Garfinkle [58] used the fact that recursive grid refinement in near-critical solutions is not required in arbitrary places, but that all refined grids are centered on tex2html_wrap_inline2395, in order to use a simple fixed mesh refinement on a single grid in double null coordinates: u grid lines accumulate at u =0, and v lines at v =0, with (v =0, u =0) chosen to coincide with tex2html_wrap_inline2395 . Hamadé and Stewart [81Jump To The Next Citation Point In The Article] have written an adaptive mesh refinement algorithm based on a double null grid (but using coordinates u and r), and report even higher resolution than Choptuik. Their coordinate choice also allowed them to follow the evolution beyond the formation of an apparent horizon.



2.2 Other matter models2 The phenomena2 The phenomena

image Critical Phenomena in Gravitational Collapse
Carsten Gundlach
http://www.livingreviews.org/lrr-1999-4
© Max-Planck-Gesellschaft. ISSN 1433-8351
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