Gauge conditions for black hole spacetimes
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Gauge conditions for black hole spacetimes. Miguel Alcubierre ICN-UNAM, Mexico. Desirable properties of gauges for black hole evolutions. Desirable properties of gauges are: Avoid physical and coordinate singularities. Keep coordinate lines from falling down the holes.

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Gauge conditions for black hole spacetimes

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Gauge conditions for black hole spacetimes

Gauge conditions forblack hole spacetimes

Miguel Alcubierre

ICN-UNAM, Mexico

Desirable properties of gauges for black hole evolutions

Desirable properties of gauges for black hole evolutions

  • Desirable properties of gauges are:

  • Avoid physical and coordinate singularities.

  • Keep coordinate lines from falling down the holes.

  • If possible, minimize changes in metric (co-moving, co-rotating, etc.)

  • If possible, follow Killing fields when the exist (at late times).

  • A way to address these points is to relate the gauge choice to the change in time of geometric quantities. One can do this in different ways:

  • Force the change of some geometric quantities to be zero. This typically leads to elliptic gauge conditions.

  • Make the change of the gauge functions proportional to the change of some geometric quantities. This leads to parabolic or hyperbolic conditions.

Specifying a foliation of spacetime

Specifying a foliation of spacetime

To specify a foliation one needs to prescribe a way to calculate the lapse. There are many ways of doing this:

  • Prescribed lapse (or prescribed densitized lapse): Lapse given as a known function of xi and t.

  •  = 1 (geodesic slicing).

  •  = lapse from known exact solution.

  • Algebraic lapse: Lapse given as function of geometric variables.

  • = 1/2 (harmonic slicing).

  • Elliptic lapse condition: Lapse obtained by solving elliptic equation.

  • 2  =  Kij Kij (maximal slicing).

  • Time derivative lapse condition: Time derivative of lapse given as function of geometric variables.

  • t  =  2 trK (differential form of harmonic slicing).

Notice that some of these classes might overlap. For example, harmonic slicing can also be seen as a prescribed densitized lapse.

How can a foliation of spacetime go wrong

How can a foliation of spacetime go wrong?

Foliations of spacetime can go wrong for serveral reasons:

  • The slices can hit a physical singularity (black holes).

  • The slices can hit a coordinate singularity where the spatial volume elements vanish (focusing of normal observers).

  • The slices can become non-smooth at a point (gauge shocks).

  • The slices can remain smooth but stop being spacelike (e.g. they can become null at a point).

  • Etcetera.

Elliptic slicing conditions

Elliptic slicing conditions

The standard example of an elliptic slicing condition is the “K-freezing” condition:

Which in the particular case when trK=0 reduces to maximal slicing, which is strongly singularity avoiding.

The K-freezing condition results in an elliptic equation for the lapse:

Singularity avoiding with zero shift leads to “grid stretching” (exponential growth of the metric in the region close to the horizon … but a shift can help to reduce this.

Maximal slicing pros and cons

Maximal slicing pros and cons


  • Maximal slicing produces nice and smooth lapses, and avoids singularities very well. When it can be used, experience shows that it is much more accurate and less prone to instabilities than other common choices (1+log).

  • It eliminates one degree of freedom (trK), which in BSSN means one variable less to evolve, and hence less chance of instabilities!


  • Maximal slicing is slow to solve. In 3D, and with a good elliptic solver (BAM), one typically still spends about 90% of the CPU time solving this single equation.

  • With excision we have currently no good idea for a boundary condition at the excision region.

    Excision myth:

  • We don’t need singularity avoidance with excision. FALSE, we do! We need to avoid coordinate singularities too, not just the physical singularity. And coordinate singularities can appear anywhere …

The bona masso family of slicing conditions

The Bona-Masso family ofslicing conditions

The Bona-Masso (BM) family of slicing conditions has the form

  • With f() > 0 but otherwise arbitrary.

  • Things to notice:

  • This family was introduced in the context of the BM hyperbolic re-formulation of the evolution equations, but it can be used with any form of the equations.

  • If one prefers to use a densitized lapse of the form Q =   /2, then the BM slicing condition takes the form

  • The shift terms in the BM slicing condition guarantee that we will have the same foliation for any shift. This seems natural but other generalizations are possible.

Wave equation for the lapse

Wave equation for the lapse

Using the evolution equation for Kijwe can easily find that

The lapse function then obeys a wave equation with sources. The wave speed along a fixed spatial direction xi is given by

For f=1, this is equal to the speed of light, but for other choices of f it can be smaller or larger than the speed of light.

A gauge speed larger than that of light introduces no causality problems, since this is just the speed of propagation of the coordinate system.

BM slicing Myth: Having all characteristic speeds equal to the speed of light is a good thing. FALSE! This is a prejudice. Why should this be good? In fact, experience shows that having gauge speeds larger than the speed of light is better (1+log).

Some particular cases of bm slicings

Some particular cases of BM slicings

  • From the ADM equations one can easily show that the evolution equation for the spatial volume elements is

  • Consider the case when f = N , with N a constant. Comparing the last equation with the BM slicing condition, we can find  as a function of 1/2:

  • with h an arbitrary time independent function. The case N = 1 (that is f = 1) is known as “harmonic slicing”.

  • Take now f = N/. In that case we find the “1+log” family

General relation between lapse and volume elements

General relation betweenlapse and volume elements

In general, with the BM slicing condition one has the following relation between the lapse and the spatial volume elements

Or in integral form

Generalized wave equation for the time function the foliation equation

Generalized wave equation for thetime function: the foliation equation

A short calculation shows that the Bona-Masso family of slicing conditions can be written in 4-covariant form as a generalized wave equation on the time function T in the following way

With n the unit normal vector to the spatial hypersurfaces:

If we take f = 1 we see that T obeys the simple wave equation, so T it is a harmonic function. This is why this case is known as harmonic slicing.

Focusing singularities

Focusing singularities

We define a focusing singularity as a place where the spatial volume elements vanish at a bounded rate. If the singularity occurs after a proper time s (measured by normal observers), the elapsed coordinate time will be

We will say that the singularity is of order m if the volume elements vanish as

Notice that m must be positive for there to be a singularity at all, and it must be larger than or equal to 1 for the singularity to be approached at a bounded rate.

Strong and marginal singularity avoidance

Strong and marginalsingularity avoidance

As the volume elements 1/2 go to zero, the lapse can do one of 3 things:

1) It can remain finite, 2) it can vanish with 1/2, 3) it can vanish before 1/2.

CASE I: One can easily see that case 1 can not happen with the BM slicing conditions as long as f  0. The lapse always collapses as 1/2 goes to zero.

CASE II: If the lapse collapses with 1/2 we can hit the singularity after a finite or infinite coordinate time, depending on how fast the lapse collapses as we approach the singularity. If we reach the singularity in an infinite coordinate time we say that we have “marginal singularity avoidance”.

CASE III: If the lapse collapses before 1/2 then the time slices stop advancing before the singularity is reached (the slices can in fact move back in some cases). In this case we say that we have “strong singularity avoidance”.

Singularity avoidance conclusions

Singularity avoidance: Conclusions

  • The final result can be summarized as follows:

  • If f() behaves as f = An for small , and we have a singularity of order m, then

  • For n<0 we have strong singularity avoidance.

  • For n=0 and mA1 we have marginal singularity avoidance.

  • For n>0 , or n=0 with mA<1,we do not have singularity avoidance, even though the lapse collapses to zero at the singularity.

  • If we have a singularity of order m=1 , then harmonic slicing (n=0, A=1) marks the boundary between avoiding and hitting the singularity.

Gauge shocks

Gauge shocks

Shocks: Discontinuous solutions to non-linear hyperbolic PDE’s that arise from smooth data and are characterized by the crossing of characteristic lines.

The Einstein equations can be written (in some gauges) as a linearly degenerate system, so physical shocks are not expected!

One can have traveling discontinuities called “contact discontinuities”, but these do not arise from smooth data and travel along null lines.

T = 0

T = 100

When using hyperbolic gauge conditions, shocks associated with the propagation of the gauge can arise from smooth initial data.

These “gauge shocks” are a particular form of coordinate singularity where the spatial slices develop a kink.

Avoiding gauge shocks

Avoiding gauge shocks

The no-shock condition (linear degeneracy) for the Bona-Masso family of slicings implies that

This clearly contains harmonic slicing as a particular case (k = 0).

For non-zero k this is not a very good slicing condition since for small  it can allow the lapse to become negative. To see this notice that if we use this solution in the Bona-Masso slicing condition we obtain, for small :

However, we can still find useful slicings if we look only for approximate solutions to the gauge avoidance equation.

Zero order shock avoidance

Zero order shock avoidance

Assume the lapse is of the form =1+ with  << 1, and expand f as

I we want to satisfy the condition for shock avoidance to zero order in  we must have

One particular family of solutions that has such an expansion is

The case a0 = 1 corresponds to harmonic slicing.

Another case of special interest is a0 = 2, for which we find: f = 2/.

This specific member of the 1+log family is precisely the one that has been found empirically to be very robust in black hole and Brill wave simulations!

First order shock avoidance

First order shock avoidance

To satisfy the condition for shock avoidance to first order in  we must take

One way to achieve this is to use

Again, for a0 = 1 we recover harmonic slicing. If we take a0 = 4/3 we obtain

For small  this behaves as a member of the 1+log family. Moreover, it satisfies the shock avoidance condition to higher order that f = 2/ and its gauge speed in the asymptotically flat region is only 1.15 instead of 1.41.

Could this be a more robust slicing condition?

Shift conditions

Shift conditions

  • Far less is known about good shift conditions that about slicing conditions.

  • Experience shows that traditional elliptic conditions (minimal distortion) do not work very well with BH’s. Why? Your guess is as good as mine.

  • Several hyperbolic shift conditions with many free parameters have been put forward recently (Lindblom-Scheel, Bona-Palenzuela).

    Pros: They are hyperbolic, so well posed. Cons: No idea what they do in real life, nor how to choose parameters. Do they produce gauge shocks? Any other type of singularity?

  • Good to remember: Well posedness only guarantees good behavior for a FINITE time, which in practice can be rather small. We need to know more …

Bssn shift conditions

BSSN shift conditions

In BSSN one can consider families of elliptic, parabolic and hyperbolic shift conditions that relate the shift choice to the evolution of the BSSN conformal connection functions.

An elliptic shift condition is obtained by asking for the conformal connection functions to be time-independent:

This “Gamma-freezing” condition is closely related to the “minimal distortion” shift condition (the principal part of the elliptic operator acting on the shift is identical in both cases).

One can obtain parabolic and hyperbolic shift conditions by making the first or second time derivatives of the shift proportional to the elliptic operator contained in the above condition.

Such parabolic or hyperbolic conditions are called “drivers”.

Hyperbolic gamma driver shift

Hyperbolic Gamma-Driver Shift

The “hyperbolic Gamma-driver” shift condition has the following form:

where and  are positive functions of position and possibly of time.

It is important to add a damping term to reduce the oscillations in the shift (this is not numerical dissipation!).

We have found that by choosing an adequate form for the function  and fine-tuning the value of the dissipation coefficient  we can almost freeze the evolution of a black hole system at late times!

Why does this work better than minimal distortion? Beats me, it just does (I guess we are lucky). But we really don’t know almost anything about the analytical properties of this shift condition.

Co moving shift vector

Co-moving shift vector

When evolving with zero shift, a black hole can’t move in coordinate space (the horizon just grows in place). Moving a black hole requires large shifts, and introduces large artificial dynamics.

Why force a black hole to move if it naturally wants to stay in place?

A better alternative is to use co-moving coordinates …

How to choose a shift vector that gives us co-moving coordinates?

Answer: easy, zero shift does precisely this. So we just need to make sure that the shift goes to zero somewhere inside the black-hole.

When using puncture initial data, a simple way to achieve this is to use the hyperbolic Gamma-driver shift with:

With  the time independent conformal factor from the initial data, which is infinite at the punctures contained inside all black holes.

Co rotating shift vector

Co-rotating shift vector

  • Good idea when evolving BH’s in orbital configurations.

  • How do we do this?

  • With a hyperbolic shift condition choose as initial a rigid rotation (with some guess for the angular velocity), that goes to zero at the punctures:

  • … then just let the evolution equation for the shift take care of the rest.

  • What is a good initial guess for the angular velocity?

  • Use some analytic information, and/or simple trial and error …

  • What about the light-cylinder? (rotation speed = c)

  • Irrelevant for stability, the only relevant condition for stability is the CFL condition: if the shift is too large far away, just use a smaller time step.

  • But … boundary conditions on a cube are messy and probably inconsistent. It is probably a good idea to use a cylinder as the boundary.

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