Black holes and time dilation around the event horizon

[Domisterwoozy]

As I currently understand it from the point of view of an observer falling into a black hole it takes a finite time to cross the event horizon and reach the singularity. From the point of view of a far away observer the person falling into the black hole never actually crosses the event horizon because time is dilated infinitely at the event horizon.

I am also told that because of Hawking radiation all black holes will evaporate fully in a finite (maybe very long) time. Therefore, from the point of view of a distant observer the black hole will actually disappear before the in-falling person crosses over the event horizon.

How is it possible that from one point of view a person can fall into the singularity being destroyed forever, while from another point of a view after a finite amount of time the in-falling person never even crosses into the black hole and can even rejoin the far away observer.

 

[Passionflower]

As I currently understand it from the point of view of an observer falling into a black hole it takes a finite time to cross the event horizon and reach the singularity. From the point of view of a far away observer the person falling into the black hole never actually crosses the event horizon because time is dilated infinitely at the event horizon.

I would say no.

Indeed an observer falling into a black hole will reach the singularity in finite time. However a far away observer will never see that simply because light slows down the closer we get to the event horizon. So for instance the light coming from an object near the event horizon will take almost forever to reach a far away observer. When light is at the event horizon it will never reach an outside observer.

But just because an outside observer does not see him passing the event horizon does not mean he does not actually pass.

 

[Domisterwoozy]

I would say no.

But just because an outside observer does not see him passing the event horizon does not mean he does not actually pass.

But shouldn't both reference frames be equally valid?

 

[PAllen]

As I currently understand it from the point of view of an observer falling into a black hole it takes a finite time to cross the event horizon and reach the singularity. From the point of view of a far away observer the person falling into the black hole never actually crosses the event horizon because time is dilated infinitely at the event horizon.

I am also told that because of Hawking radiation all black holes will evaporate fully in a finite (maybe very long) time. Therefore, from the point of view of a distant observer the black hole will actually disappear before the in-falling person crosses over the event horizon.

How is it possible that from one point of view a person can fall into the singularity being destroyed forever, while from another point of a view after a finite amount of time the in-falling person never even crosses into the black hole and can even rejoin the far away observer.

You raise many deep questions, which ultimately have no answers until there is some complete quantum theory of black holes. However, ignoring Hawking radiation for a moment, a partial answer is:

Either the infalling person turned around before going through the horizon or they didn't. If they did, the distant observer will eventually see this. If they didn't, the distant observer will never see this.

As for Hawking radiation, I would characterize its derivations as heuristic. Attempting to use partial quantum theories of gravitation, all of the following have been derived by different researchers claiming expertise:

1) With quantum corrections, nothing ever passes the horizon.
2) With quantum corrections, everything reaches the horizon in finite time, even from an external view (the horizon still being a real phenomenon).
3) With quantum corrections, horizons don't ever form.

(1) and (2) I've seen published in peer reviewed journals. (3) I've only encountered recently, and the only proponent mentioned has published the papers in a single obscure journal.

 

[Domisterwoozy]

Thanks PAllen, I assumed this was the case. So basically I mixed a quantum effect with a purely classical model of black holes. I guess I will have to wait for a complete quantum theory of gravity.

 

[pervect]

There's a couple of FAQ's on this, as I recall. See for instance http://cosmology.berkeley.edu/Education/BHfaq.html#q9

We've observed that, from the point of view of your friend Penelope who remains safely outside of the black hole, it takes you an infinite amount of time to cross the horizon. We've also observed that black holes evaporate via Hawking radiation in a finite amount of time. So by the time you reach the horizon, the black hole will be gone, right?

Wrong. When we said that Penelope would see it take forever for you to cross the horizon, we were imagining a non-evaporating black hole. If the black hole is evaporating, that changes things. Your friend will see you cross the horizon at the exact same moment she sees the black hole evaporate. Let me try to describe why this is true.

That answers part of the question, about why things appear differently. They don't appear differently if one is careful.

To untangle cause and effect, it's useful to consider a black hole whose evaporation is controlled by an external event. This is possible because a black hole that's big enough doesn't have to evaporate.

In that case, one can show that there is a "last event" that the infalling observer can observe, by tracing the light rays. Cause and effect only travel inwards, there's no way for causes to travel outwards, but there are still causal relationships that apply.

If the event that controls whether or not the black hole is allowed to evaporate occurs after this last event, it won't affect the fate of the infalling observer one whit, it will be "too late".

One can almost always imagine that an external event that can keep the black hole can happen, it just involves dumping enough mass down it.

So, basically, unless the black hole that one falls into is really, really small, the fate of the infalling observer can't depend on whether it is eventually allowed to evaporate or not.

(I know I didn't come up with the above argument, but I don't recall anymore which of the various FAQ's mention it.)

 

[Passionflower]

But shouldn't both reference frames be equally valid?

Here is a plot (where the Schwarzschild radius is 1) that clearly shows what is going on, why a free falling observer increases his local velocity (wrt a static observer) the velocity observed from a remote location initially increases but closer to the event horizon decreases while eventually coming to a halt at the event horizon.

[PLAIN]http://img254.imageshack.us/img254/5750/velocitycompare.png

What is the factor that causes the discrepancy?

It is the speed of light.

 

[pervect]

Some general remarks:

1) I think some sort of "toy metric" for an evaporating black hole could be useful in answering this question rigorously, but I've never seen such a metric written out. I suppose one could try a Schwarzschild metric with a time-dependent and very slowly varying total mass, I'm not sure if there are any hidden "gotcha's" in the approach, which would be an approximate solution to Einstein's equations rather than an exact one.

Answering questions rigorously about what someone sees when you don't have a metric is sort of difficult. Though one can make an educated guess, the results will be rather non-detailed.

2) The question is rather advanced, and I suspect a lot of people are worrying about the hard questions prematurely, in the sense that they'd learn more if they asked the easier questions where they could understand the answers fully. A quick pithy summary would be "walk before you try to run".

3) A large chunk of the problem is that people interpret "time slowing down" near the event horizon in terms of absolute time. People who have learned SR know that absolute time doesn't exist. Unfortunately, people who haven't learned SR not only don't know that absolute time doesn't exist, but don't even realize that you are talking about them when you talk about people who believe in absolute time.

This gets into the "walk before you can run" aspect I was making earlier, point #2. If the reader has some clue about why absolute time doesn't exist, trying to untangle the one-way causal relationships in a black hole is going to be a lot easier. I'm not sure it's even possible to do correctly if you're making false fundamental philsophical assumptions to start with.

 

[PAllen]

There's also the fact (mentioned in other threads, but not here so far) that except for hypothetical tiny primordial black holes, black holes are growing, not shrinking. The influx of energy from CMB is orders of magnitude greater than Hawking radiation. Only near the heat death of the universe will this likely reverse.

 

[Passionflower]

I am surprised everybody is looking for explanations using quantum theory or Hawking radiation for something that is quite simple: light simply takes more time to get to the remote observer the closer it is to the event horizon and at the event horizon it never gets out. So there is really not much of a surprise a remote observer cannot see the object fall through the event horizon.

 

[GODISMYSHADOW]

(I know I didn't come up with the above argument, but I don't recall anymore which of the various FAQ's mention it.)They used complex numbers to come up with the theory of black holes. The reality of black holes must be like the reality of the square root of negative unity, i=√(-1).

 

[DrGreg]

They used complex numbers to come up with the theory of black holes. The reality of black holes must be like the reality of the square root of negative unity, i=√(-1).

It's quite possible (and, I think, usual) to describe all aspects of black holes without the use of complex numbers.

(By the way, electrical and electronic engineers frequently describe alternating current and electronic circuits using complex numbers. I suppose that casts doubts on the reality of electronics?)

 

[Zula110100100]

My Theory would be that as the black hole evaporated you would see the person getting closer to it at an equal rate that it shrunk until it was just an immensly high gravity area that you see squash your friend. It most likely could not evaporate so fast as to vanish and your friend pass right on by, it would have to pass between being a black hole and not being there.

 

[Drakkith]

I am surprised everybody is looking for explanations using quantum theory or Hawking radiation for something that is quite simple: light simply takes more time to get to the remote observer the closer it is to the event horizon and at the event horizon it never gets out. So there is really not much of a surprise a remote observer cannot see the object fall through the event horizon.

How so? Wouldn't it be red shifted instead of taking longer to arrive since the speed is the same in all frames?

 

[Passionflower]

How so? Wouldn't it be red shifted instead of taking longer to arrive since the speed is the same in all frames?

The speed of light is c locally. That does NOT mean that the speed of light between two objects A and B removed a distance from each other is c, this speed varies in a gravitational field.

 

[PAllen]

How so? Wouldn't it be red shifted instead of taking longer to arrive since the speed is the same in all frames?

No, passionflower is right. To a distant observer, light itself moves ever slower close to an event horizon. For example, this could be seen in 'light clock' reflecting light back and forth between two mirrors, oriented tangentially to the horizon and near it. To the distant observer, this clock (like any other) would run very slow - thus the light is moving very slow between the mirrors.

To the near horizon observer, everything is normal.

There is no sense in which one observer is right and the other wrong - they are just different frames of reference.

 

[Drakkith]

I see. I'll have to go re-read my relativity book!

 

[Passionflower]

Two formulas you want to keep in mind if you want to find the speed of light as observed by a far away observer:

For radial motion it is
\Large 1-{\frac {{\it r_s}}{r}}
For other motion we can use an impact parameter b:
\Large \left( 1-{\frac {{\it r_s}}{r}} \right) \sqrt {1+{\frac {{\it r_s}\,{b}<br /> ^{2}}{{r}^{3}}}}
Based on the value of this impact parameter we can also determine if an incoming light pulse plunges, goes into an (unstable) orbit or escapes and generally we can get an idea about gravitational lensing.

 

[Zula110100100]

R_s Being the Swartszchild radius? In that case then as the black hole, and thefore the radius decayed, would the slow moving light reach us in what we would consider less time, giving the appearance of the person slowly moving forward with the radius?

What would we expect to see in a black hole as its radius shrunk to just within the volume of the mass supporting it? I would guess the pressure would cause it to be a very hot plasma or something? Certainly not clear empty space that one could just float on through as it seems to me is assumed in the OP's question

How is it possible that from one point of view a person can fall into the singularity being destroyed forever, while from another point of a view after a finite amount of time the in-falling person never even crosses into the black hole and can even rejoin the far away observer.

 

[Q-reeus]

No, passionflower is right. To a distant observer, light itself moves ever slower close to an event horizon. For example, this could be seen in 'light clock' reflecting light back and forth between two mirrors, oriented tangentially to the horizon and near it. To the distant observer, this clock (like any other) would run very slow - thus the light is moving very slow between the mirrors...

I had taken as a given that such could be a well defined gedanken experiment - one could use the SC's to properly define transverse distance and light speed. But according to your reasoning here: https://www.physicsforums.com/showpost.php?p=3573328&postcount=79 what handle can one get on 'distance' between the mirrors and thence 'c' of light bouncing between? You say light moves ever slower closer to the EH. Fine, except that if one accepts a fuzzy/ambiguous notion of length in GR, how precisely and unambiguousy can 'slower light speed' be defined?

 

[pervect]

Speeds and distances are both well defined and unambiguous in the local tangent space. Only when you start to look at larger distances over which the curvature of space-time is significant do you start to run into ambiguities.

 

[Q-reeus]

Speeds and distances are both well defined and unambiguous in the local tangent space...

Correct me if wrong - but is not 'local tangent space' here the situation where c is just the local, invariant, proper value? Which would be of no help when it comes to comparing 'here' with 'over there' - precisely the issue in question.

Only when you start to look at larger distances over which the curvature of space-time is significant do you start to run into ambiguities.

OK, but the static source, static observer problem I posed in the link specified what one would think a case where distance, on a relational basis, should have an unambiguous definition. Was left with the impression even for this simplest case, there is ambiguity. And yet astrophysicists have it seems precisely pinned down many parameters testing GR from the orbital mechanics of the Hulse-Taylor binary pulsar. Hard to believe that is possible without having a precise handle on length scale - but I could be wrong.

 

[PAllen]

I had taken as a given that such could be a well defined gedanken experiment - one could use the SC's to properly define transverse distance and light speed. But according to your reasoning here: https://www.physicsforums.com/showpost.php?p=3573328&postcount=79 what handle can one get on 'distance' between the mirrors and thence 'c' of light bouncing between? You say light moves ever slower closer to the EH. Fine, except that if one accepts a fuzzy/ambiguous notion of length in GR, how precisely and unambiguousy can 'slower light speed' be defined?

Absence of unique choice does not mean no choice can be made; it means more than one can be made, with some difference in the outcome. Pick most any plausible way of defining long distance and remote distance, and the distant observer will see lightspeed slow near an event horizon. The exact numbers will differ based on choice.

However, in some cases, the nature of a phenomenon is changed by such choices (which are really coordinate system choices). An example I like is the Shapiro effect. If I require that planets travel on near perfect ellipses, and measure orbital parameters of a planet at several points away from the sun, and then measure radar travel times to the planet as it passes behind the sun, I see Shapiro time delay. On the other hand, if I define distance by round trip light time times constant c, I see a different effect altogether: the Shapiro orbital bump. Both are completely valid, usable choices in GR. The former is more conventional, and simpler to use for astronomy.

 

[Q-reeus]

...An example I like is the Shapiro effect. If I require that planets travel on near perfect ellipses, and measure orbital parameters of a planet at several points away from the sun, and then measure radar travel times to the planet as it passes behind the sun, I see Shapiro time delay. On the other hand, if I define distance by round trip light time times constant c, I see a different effect altogether: the Shapiro orbital bump. Both are completely valid, usable choices in GR. The former is more conventional, and simpler to use for astronomy.

Surprised that both cases can be equally valid. Does not the assumption of a constant c in the second case make it suspect - the orbital 'bump' (apparent orbital speed-up/speed-down?) being an artifact of that assumption?

Getting back to the example given of light bouncing between mirrors. Let's forget the complications of being near an EH (and presumably required thus to be in free-fall). Pick a quiet, non-rotating perfectly spherical planet. Mirrors and bouncing light are on the surface, and an observer perched in a tall tower observes from above. We all agree that the observer detects a redshift of the light clock frequency, relative to the locally measured value at the surface. Can we or can we not derive this in an unambiguous manner via a gedanken experiment which assumes that light speed and/or distance between mirrors is gravitationally affected (sans the usual extraneous mechanical/optical effects of 'g') in a manner derivable from SC's? Or is the best we can do is refer to a 'quotient' of f = c'/(2*d') (f the redshifted clock frequency, c', d' the 'redshifted' values of light speed, mirror displacement, respectively), with neither c' or d' individually definable? Hard to see such a situation is mandated by GR.
[It is understood that by some authorities at least, in standard SC's c' is less in the radial direction than tangential, but not in ISC's. So just pick one, and work within it. Hopefully either system would agree as to net effects.]

 

[Passionflower]

On the other hand, if I define distance by round trip light time times constant c, I see a different effect altogether

You can define whatever you want but that does not make it so. For instance how would you explain that the distance between A to B and B to A is different.

Can you provide some credible references where distance in GR is defined as the roundtrip time of light?

 

[PAllen]

You can define whatever you want but that does not make it so. For instance how would you explain that the distance between A to B and B to A is different.

Can you provide some credible references where distance in GR is defined as the roundtrip time of light?

I don't need a reference. This is about mathematical definition of coordinate systems. A coordinate system is a 1-1 mapping between an open set of a manifold and R4 (for the classical GR case). Can you deny that what I propose is a 1-1 mapping? Can you deny that the metric can be expressed in these coordinates? Given that, can you deny that any invariant is the same? All physical observables in GR have coordinate independent definitions. In this case, the observation is round trip radar interval as a function of proper time of of the 'stationary lab'. The coordinate interpretation issue is the separation of this into position and travel time. The former is the observable, the latter is pure coordinate convention.

 

[Passionflower]

In this case, the observation is round trip radar interval as a function of proper time of of the 'stationary lab'.

There is nothing wrong with that measurement. But you claim it is the distance. In that case you would have to explain why the distance between A and B is different from the distance between B and A using your roundtrip time method.

I don't need a reference.

I see you are simply an authority who can tell others here they are wrong without showing it with a single formula or reference.

 

[PAllen]

There is nothing wrong with that measurement. But you claim it is the distance. In that case you would have to explain why the distance between A and B is different from the distance between B and A using your roundtrip time method.
.

I don't see what this has to do with setting up a coordinate system. I pick one worldline to be a 'time axis'. Then, I define both simultaneity and distance by round trip radar time (for position, I supplement my radar defined distance from origin with angular coordinates). I have unambiguous polar coordinates. Now, if desired, I can switch to a Cartesian style system from the same origin (my chosen origin world line).

In this coordinate system, coordinate distances don't match proper distances for the given simultaneity surfaces. So what? That is true of many coordinates systems, including SC, and isometric SC.

In these coordinates, geodesics are 'near ellipses' with a bump.

Despite more complex mathematical form, such coordinates actually have some virtues:

- a minimum of interpretation; they just codify direct measurements.

- Radial speed of light everywhere is constant by definition.

I don't minimize the consequent complications that go with these benefits, and don't consider them very practical coordinates. But the idea the coordinates are arbitrary, meeting only minimal conditions, and the coordinate independent geometry is paramount, is a truly fundamental feature of classical GR.

 

[Passionflower]

I don't see what this has to do with setting up a coordinate system. I pick one worldline to be a 'time axis'. Then, I define both simultaneity and distance by round trip radar time (for position, I supplement my radar defined distance from origin with angular coordinates). I have unambiguous polar coordinates. Now, if desired, I can switch to a Cartesian style system from the same origin (my chosen origin world line).

In this coordinate system, coordinate distances don't match proper distances for the given simultaneity surfaces. So what? That is true of many coordinates systems, including SC, and isometric SC.

In these coordinates, geodesics are 'near ellipses' with a bump.

Despite more complex mathematical form, such coordinates actually have some virtues:

- a minimum of interpretation; they just codify direct measurements.

- Radial speed of light everywhere is constant by definition.

I don't minimize the consequent complications that go with these benefits, and don't consider them very practical coordinates. But the idea the coordinates are arbitrary, meeting only minimal conditions, and the coordinate independent geometry is paramount, is a truly fundamental feature of classical GR.

It seems to me there is not much of a point debating you, you know it all and better it seems...

 

[PAllen]

It seems to me there is not much of a point debating you, you know it all and better it seems...

Hardly, I freely admit errors all the time, including ones you've pointed out. So far, you have given me no indication I am in error in this case. Everything I have said appears part of the definitional basis of GR.

 

[GODISMYSHADOW]

It's quite possible (and, I think, usual) to describe all aspects of black holes without the use of complex numbers.

(By the way, electrical and electronic engineers frequently describe alternating current and electronic circuits using complex numbers. I suppose that casts doubts on the reality of electronics?)

Electronic engineers call it the "j" operator (so as not to confuse it with current). It's trig intensive and they use Euler's formula and De Moivre's theorem along with phasors to make calculations easier. It's a means to an end.

 

[Q-reeus]

So there was no attempt to answer my queries in #24. Sweet - no-one here is under compulsion to always respond; still it would have been a nice courtesy. Just maybe there was an oblique response by way of comments in #26 and #28. In #26, PAllen wrote:

"...in GR have coordinate independent definitions. In this case, the observation is round trip radar interval as a function of proper time of of the 'stationary lab'. The coordinate interpretation issue is the separation of this into position and travel time. The former is the observable, the latter is pure coordinate convention..."

But unless there is some unspecified mixing of light travel time with planetary orbital travel time here, 'round trip radar interval' IS 'travel time'. Should that not then read 'the separation of this into integrated coordinate length (thus length scale enters) and integrated coordinate time (thus time dilation enters)'? The issue is still there, just masked imo.
And in #28:

"I don't see what this has to do with setting up a coordinate system. I pick one worldline to be a 'time axis'. Then, I define both simultaneity and distance by round trip radar time (for position, I supplement my radar defined distance from origin with angular coordinates). I have unambiguous polar coordinates."

I am unclear as to where these unambiguous polar coordinates are centered, and what the mathematical form of such is.

"Now, if desired, I can switch to a Cartesian style system from the same origin (my chosen origin world line).
In this coordinate system, coordinate distances don't match proper distances for the given simultaneity surfaces. So what? That is true of many coordinates systems, including SC, and isometric SC."

This implies there actually is even one coordinate system where everything, over an extended region of curved spacetime, can correspond to proper values?!

"In these coordinates, geodesics are 'near ellipses' with a bump.
Despite more complex mathematical form, such coordinates actually have some virtues:
- a minimum of interpretation; they just codify direct measurements.
- Radial speed of light everywhere is constant by definition..."

The radial light speed is constant in such - but only radial? In such a 'preferred' coordinate system where radial c is a constant, orbital 'bumps' appear rather than Shapiro time delay. But positing a coordinate invariant c goes against what GR is about surely, and as suggested in #24, the 'bumps' are therefore not a perfectly valid alternative explanation at all, but unphysical artifacts.
Would you care to now answer just this bit from #24:
"Or is the best we can do is refer to a 'quotient' of f = c'/(2*d') (f the redshifted clock frequency, c', d' the 'redshifted' values of light speed, mirror displacement, respectively), with neither c' or d' individually definable?"

 

[pervect]

So there was no attempt to answer my queries in #24.

I'm not quite sure what the question was. I am guessing SC = Schwarzschild coordinates and ISC = Isotropic Schwarzschild coordinates.

Pick either one (or any other coordinate system you like), and you'll get the same results for the observed doppler shift at the top of the tower. You won't even need any notion of "distance in the large" to perform such a calculation. You'll just need the coordinates of both ends of the light clock, and the coordinates of the observer of the tower. For a light clock in an arbitrary orientation, you'll have different doppler shifts from each end, of course. I'm assuming the light clock transmits a signal to the tower "ping" or "ping+timestamp" every time the light pulse it holds makes a round trip, if you imagine the light pulse is short you can imagine that the light clock transmits a signal every time the light pulse is "at that end" of the lightclock.

As far as measuring distances goes, the more-or-less standard prescription, according to Wald (and with some input from George Jones- see https://www.physicsforums.com/showpost.php?p=2933053&postcount=9 ) is as follows:

[add. This discussion, as the title of the thread also indicates, assumes one is talking about "proper distance", in the GR sense, by "distance". This is NOT always the case!

Some common alternatives (besides proper distance in the SR sense, which is confusingly not the same) include Fermi-normal distance (soometiems called fermi distance, but this is an oversimplification) and various generalziations therof. See for instance http://arxiv.org/PS_cache/arxiv/pdf/0901/0901.4465v2.pdf, for a discussion including some references about why sometiemes Fermi-normal coordinates are sometimes considered to have "a physical meaning coming from the principle of equivalence.".

SOrry - continuing on with how you define proper distance:

You slice space-time up into spatial slices of constant time, then use the 4-metric of space-time to induce a 3-metric on your spatial subslice. This is pretty easy if your surfaces of constant time are defined by dt=0, in which case you simply eliminate dt from your line element, turning your 4-element line element (dt, dr, dtheta, dphi) into a 3-element line element (dr, dtheta, dphi).

If your surfaces of constant time don't have the property that dt=0 along them, you have to do more work.

Then you define the distance as, informally, the "length of the shortest path between two points", or more formally as "the greatest lower bound of the lengths of all curves connecting the two points".

So your notion of distance will depend on the details of how you slice up space-time into surfaces of constant time. Fortunately, in the case of a static observer there's a fairly obvious choice of how to do the split, and it corresponds to the easy choice of making dt=0 in Schwarzschild coordinates. The spatial surface defined in this way (dt=0) will be orthogonal to the timelike worldlines of all static observers.

But you don't really need to know any distances-in-the-large to compute the doppler shifts. In fact, it's probably an easier calculation without worrying about distance.

 

[Q-reeus]

I'm not quite sure what the question was. I am guessing SC = Schwarzschild coordinates and ISC = Isotropic Schwarzschild coordinates.

Yes - sorry I probably should not have assumed everyone would know what that shorthand represented.

Some common alternatives (besides proper distance in the SR sense, which is confusingly not the same) include Fermi-normal distance (soometiems called fermi distance, but this is an oversimplification) and various generalziations therof. See for instance http://arxiv.org/PS_cache/arxiv/pdf/...901.4465v2.pdf , for a discussion including some references about why sometiemes Fermi-normal coordinates are sometimes considered to have "a physical meaning coming from the principle of equivalence.".

A look at VI. EXAMPLES OF EXTENDED FERMI COORDINATES - g. The Schwarzschild metric on p11 there, eqn's 50-52 indicates to my layman mind just how complicated even a 'simple' example can become, thanks to an infinity of derivatives in GR, and then there's the parallel transport issue - where I can appreciate ambiguities will arise in general. Despite all that, the simplest case given should not be that difficult an exercise surely - certainly not to a first order calculation in weak gravity anyway.

...Then you define the distance as, informally, the "length of the shortest path between two points", or more formally as "the greatest lower bound of the lengths of all curves connecting the two points".
So your notion of distance will depend on the details of how you slice up space-time into surfaces of constant time. Fortunately, in the case of a static observer there's a fairly obvious choice of how to do the split, and it corresponds to the easy choice of making dt=0 in Schwarzschild coordinates. The spatial surface defined in this way (dt=0) will be orthogonal to the timelike worldlines of all static observers.

Right - which is surely true in the case given. The coordinate prescription for finding just that in that case is what is wanted. But as soon as one attempts that using SC's there is the rebuff "r is just a coordinate, not a length". Which leaves one where to go?

But you don't really need to know any distances-in-the-large to compute the doppler shifts. In fact, it's probably an easier calculation without worrying about distance.

Of course I agree there is no need to think in terms of distance scale - we have a redshift prescription in terms of GM/r. The point was though one should surely be able to derive it by an alternate means that does involve distance scale and light speed. That after all was implied in the bouncing light and mirrors example given by PAllen to illustrate slowing light. My point was without also a handle on distance scale, coordinate light velocity has no properly defined meaning. To reiterate; there is enough problems with non-linearity in GR to make almost any scenario infinitely complex, but if we just take a first-order simplest case, things should not be all that troublesome. However as the OP was looking at EH scenario and thus strong gravity I will not persist here but will look at reviving another thread where certain issues remain unresolved.

 

[pervect]

Right - which is surely true in the case given. The coordinate prescription for finding just that in that case is what is wanted. But as soon as one attempts that using SC's there is the rebuff "r is just a coordinate, not a length". Which leaves one where to go?

The entire purpose of the metric is to convert changes in coordinates (r, theta, phi) into changes in length.

dr isn't a length, until you multiply it by the appropriate metric coefficient.

Once you have the spatial metric (the induced 3-metric I mentioned earlier), you find the length of any curve by integrating dL along the curve, where dL is given by

dL^2 = g_{rr} dr^2 + g_{{\theta}{\theta}} d\theta^2 + g_{{\phi}{\phi}} d\phi^2

Just remember we're using the induced three-metric here, not the space-time metric. Fortunately, for the simple case in question, it's hard to mess this part up because the two are identical, except for the omission of the dt terms. This is true for this specific case, not generally true.

And the distance is just the shortest curve connecting two points (or the greatest lower bound). Since you probably don't want to calculate an infinite number of curves to find the greatest lower bound :-), you use either the calculus of variations, the geodesic equations, or a Lagranian approach to make sure you've chosen the curve that minimizes distance.

 

[G. E. Hunter]

is black hole evaporation in the real universe, or is this just theory? Any actual observations of this phenomenon? Actual observed decreases in size or mass over time?

 

[Drakkith]

is black hole evaporation in the real universe, or is this just theory? Any actual observations of this phenomenon? Actual observed decreases in size or mass over time?

It has not been observed, and unless a black hole is very very small it will actually absorb more energy from the background radiation than it gives off itself, thus gaining mass.

 

[Zula110100100]

Regardless of the validity of any of the statements, assuming they are all true the OP's outcome should not be what is expected, if we take all the supposed mechanisms to work as stated then the mass making up the black hole would not suddenly drop to 0 once the swartzchild radius did, at that point we would be able to see the mass, and the person who was stuck entering the radius we would see hitting that mass.

 

[Q-reeus]

The entire purpose of the metric is to convert changes in coordinates (r, theta, phi) into changes in length.

I made a slip-up using the term 'coordinate' rather than 'parameter' in that quote, but the gist is the same.

dr isn't a length, until you multiply it by the appropriate metric coefficient.
Once you have the spatial metric (the induced 3-metric I mentioned earlier), you find the length of any curve by integrating dL along the curve, where dL is given by
dL^2 = g_{rr} dr^2 + g_{{\theta}{\theta}} d\theta^2 + g_{{\phi}{\phi}} d\phi^2

right, that's how I basically understood it. But in another thread, the g_rr factor, even in that context, was explained as something quite different in meaning to a straight metric operator on dr - i.e. one cannot infer a coordinate dr = dL*(g_rr)^-1/2, but rather a relation of differential volume to differential area. While the latter is apparently a standard interpretation, couldn't see where it came from.

Just remember we're using the induced three-metric here, not the space-time metric.

Not being familiar with a lot of GR jargon, loked up http://en.wikipedia.org/wiki/Induced_metric , which gave me just enough clues that 'induced metric' is somewhat akin to the idea behind 'partial derivatives' - in this case holding t constant (mapping on to a spatial hypersurface or somesuch?).

And the distance is just the shortest curve connecting two points (or the greatest lower bound). Since you probably don't want to calculate an infinite number of curves to find the greatest lower bound :-), you use either the calculus of variations, the geodesic equations, or a Lagranian approach to make sure you've chosen the curve that minimizes distance.

Phew -right about not getting into calculating an infinite number of curves! Can we simplify that even more if one restricts to just measuring along a short tangent surface geodesic r*sinθ*dϕ, or radial displacement dr - assuming exterior Schwarzschild metric where I take it g_θθ = g_ϕϕ = 1 applies?