# Markus Hanke

Resident Experts

2009

60

1. ## Does mass draw in space time?

It’s meaningless, and thus not a valid concept.
2. ## help me experiment to establish curvature

Indeed. There’s also the issue of circumnavigating Antarctica. On real Earth, that’s a distance of some ~16000km when done on a boat, and you have to make course corrections towards land. On flat Earth, the distance would be at least ~40000km, and you have to course-correct away from land. Obviously this has been done many times, so we know which option is right.
3. ## ChatGPT is bullshit

There’s free AIs out there that do this, for example Perplexity.
4. ## Superdeterminism (just came upon this )

It kind of goes beyond a mere interpretation though - SD implies that there’s no measurement independence, ie the experimenter isn’t actually free to choose his setup as he wishes. There will always be a prior correlation, no matter how you set up your experiment.
5. ## Superdeterminism (just came upon this )

I think this is only possible if the particular correlations in question were established not too long in the past. In general though, correlations could go back right to the BB, so this idea is really not testable.
6. ## When did spacetime form?

I think the main message is that spacetime can, under certain circumstances, appear pathological in some way, eg for certain observers, yet still remain physically reasonable. That’s an important point actually. The reverse is true also - a metric may appear reasonable, yet still not necessarily be physically possible.
7. ## When did spacetime form?

Exactly. Which of course is obvious, if you think about it… For this transformation to be a valid diffeomorphism, it needs to be differentiable (in addition to being invertible). If it’s only continuous but not differentiable, then I think this spacetime isn’t flat.
8. ## When did spacetime form?

I think he answered the question, and the answer was in fact so obvious that I couldn’t even see it myself 🤨 As for step functions, I don’t see how these would arise in a real-world physical metric, though I’m aware of exact solutions containing delta functions, eg the Aichlburg-Sexl ultraboost.
9. ## When did spacetime form?

Very good point!
10. ## When did spacetime form?

This got me thinking - setting aside singularities for the moment, are there (in a purely mathematical sense) metrics that are not valid solutions to the EFE? IOW, could one write down a metric for which the equations cannot be worked backwards to obtain a corresponding energy-momentum tensor, given we are on a semi-Riemannian manifold? Again, I’m talking purely mathematically, never mind physical realisability. I suspect the answer is no.
11. ## Cosmological Redshift and metric expansion

Any time And your questions are good and valid ones, it’s just that they’re kind of difficult to address without lots of maths references. The key concept in this is diffeomorphism invariance - that one can describe the same spacetime/geometry in many different coordinates, without affecting any of the physics. Thus, having purely spatial expansion, and a mix of spatial and temporal expansion in the metric, really can be two different descriptions of the exact same physical situation. This is not intuitively obvious, but mathematically rigorous.
12. ## Cosmological Redshift and metric expansion

I’m afraid I still don’t really know what you mean by this. The FLRW solution explicitly depends on the energy-momentum tensor being non-zero - an empty universe where it vanishes won’t have the same geometry as FLRW. You can’t get the FLRW solution from the vacuum field equations. The cause isn’t the presence of energy-momentum, since there also exist vacuum solutions that metrically expand (eg the Kasner metric); in my earlier comment I meant that the presence of energy-momentum implies that the spacetime cannot be flat. And by this I meant Riemann flat, which perhaps I should have stated explicitly. Dark energy is also not the cause of metric expansion; it merely influences the rate at which the expansion happens. The expansion itself happens whether there is DE or not. But in a spacetime that is globally Minkowski, there is no expansion, and thus no redshift. So I struggle to make sense of your question. By curvature I meant Riemann curvature - sorry, I should have made that explicit.
13. ## Cosmological Redshift and metric expansion

It’s not flat because when solving the EFE, you start with a universe filled with energy-momentum, which necessarily has a gravitational effect. The scale factor arises as part of the solution; it’s not a source term that appears in the initial setup. If you remove all gravitational sources, you no longer get an FLRW solution - you’d be in a different spacetime.
14. ## Cosmological Redshift and metric expansion

Such a coordinate transformation wouldn’t be a diffeomorphism, meaning you are dealing with two different spacetime geometries, and thus two completely different solutions to the EFE. IOW, an expanding-time-only metric would not just be an FLRW spacetime written in different coordinates. A metric where only the time part is “expanding” describes a completely flat spacetime, only from the perspective of an observer that undergoes some form of accelerated motion. This is not a good description of our universe, since that contains matter and radiation, and thus can’t be a flat spacetime. So far as I can tell (someone correct me if I’m wrong), a metric where both the time and space parts are expanding could be the natural description of an observer who undergoes non-uniformly accelerated motion with respect to the cosmological medium, provided the time part has a suitable mathematical form (if not, it won’t correspond to any physical observer). For such an observer, measurements of both spatial distances and time durations would explicitly depend on when they are performed. He’d see an expanding universe, but also detect proper acceleration, which would play the role of the distinct time component. The FLRW spacetime is not Riemann-flat, so I’m not sure how to answer this. Given the time component has the right form, the distinction would be in the presence of proper acceleration in the motion of the observer. The details of the spacetime geometry - curvature, geodesic structure etc - are independent of coordinate choices, so I don’t think we’re missing anything. It’s like having an electric charge - in the rest frame of that charge, you detect only an E-field. An observer who moves past that same charge sees both an E-field and a B-field. In both cases, you have the same electromagnetic field. It’s the same physical situation, seen from different vantage points. But no observer under these circumstances will ever see just a B-field alone, since that would be a physically different situation. The expanding space situation is similar - you can re-distribute the expansion among the components of the metric by a suitable coordinate transformation (same spacetime, different vantage point), but no observer will ever see a time-only expansion, since that would imply being in a flat spacetime. FLRW spacetime is not flat, so I don’t quite understand what you’re trying to ask…?
15. ## Hyper-Fast Positive Energy Warp Drives

Yes, the Lentz warp drive is potentially interesting. However, as the author of this review paper mentions, unless someone can demonstrate the feasibility of each stage in the entire life cycle - and I would add steerability to this list -, we still don’t know whether this is actually physically realisable or not.
16. ## Michelle Paver: Chronicles of Ancient Darkness

I don’t think it was. Life back in hunter-gatherer days would have been much simpler, but also brutal, painful, and generally short. There’s nothing wrong per se with technology and civilisation, it’s alleviated a lot of unnecessary suffering, and - broadly speaking - freed up resources that enabled us as a species to pursue things other than immediate survival and procreation, at least potentially. I for one wouldn’t want to go back to the dark times. The problem is only that one has to have a certain degree of wisdom with it, and that’s where we seem to be lacking. We’ve become completely dependent on our own creations, and in some sense relinquished our freedom to them. That’s problematic, but also inevitable I suppose, since our basic instinctual-psychological patterns have remained the same.
17. ## If Black holes slowly evaporate over time is there a point where they stop being a black hole?

What you’re referring to is the instant that the camera crosses the event horizon. The reading on the bottom clock (“External time”) refers to what an external observer who is at rest far away from the BH would see. But the problem is that from such an observer’s point of view, the falling camera never reaches the horizon at all; just before it gets there, it will appear to fall slower and slower, and will visually appear redder and dimmer, until it fades into invisibility. There is no instant on the distant observer’s clock at which the camera is reckoned to have crossed the horizon - the entire region of the horizon and below cannot be mapped into the external observer’s coordinate system at all, because from his point of view such a region cannot be accessed (and vice versa, the falling camera cannot get back out either). Thus, once the horizon is reached, the times on the falling camera’s clock no longer correspond to any times on the external clock, even though the camera continues to fall and continues to accumulate time normally on its own clock. There simply is no longer any meaningful notion of simultaneity at all, whether relativistic or not. So you see, time on its own in GR is a purely local concept, specific to a specific observer. It may not be shared by others. In order to ensure agreement between observers, you must now use covariant quantities instead.
18. ## If Black holes slowly evaporate over time is there a point where they stop being a black hole?

I came across another good video, concerning in-fall into a Kerr BH (mass, angular momentum). This one contains explanations, and also readings on two reference clocks; I thought some readers here might like this:
19. ## If Black holes slowly evaporate over time is there a point where they stop being a black hole?

Let’s further assume that clock (1) is far from the BH, and orbits slowly. This clock will see (2) to be still ticking, but at a much slower rate (compared to itself). It will see (3) to initially fall at increasing speed, while its tick rate gradually slows; as it approaches the horizon its descent will appear to slow more and more, and its tick rate appears slower and slower. Its visual appearance becomes dimmer and redder, and it eventually just fades into invisibility. But it will never be reckoned to have reached the horizon. (2) sees (1) to be ticking at a much faster rate, and it will visually appear blue-shifted. (3) will appear similar as described above, just at a different rate; it will also never be reckoned to have reached the horizon. For (3) itself, the time it takes to reach the horizon is finite; the fall time from horizon to singularity is also finite (for a 10 solar mass BH this will be on the order of ~150 microseconds). What tick rates it will see on clocks (1) and (2) will depend on where along its free fall trajectory the clock is - this is a bit of a balancing act between its own position in the gravitational well, and the degree of relative motion between the clocks. However, once it has fallen below the horizon, it should see both (1) and (2) to be ticking faster wrt itself. After the initial free fall period, they would all be seen to be asymptotically slowing towards the same region of space, while gradually fading from view. But they would never quite catch up. This is not simple, since it’s a mathematical model in four dimensions. Spacetime is not a substance, so resist the temptation to think about it that way. The best I can offer is to think about it as a network of relationships - it tells you how clocks and rulers at different places and times are related to one another. Each nexus within the network corresponds to a physical event (meaning: a specific point in space at a specific instant in time), and has attached to it an object (called the metric tensor) which, if you tell it a direction, will give you the spacetime distance to its closest neighbouring nexus in that direction. So it’s a network of separations between events. In special relativity that separation is the same wherever and whenever you are (the metric tensor is just a matrix of constants), but in general relativity it may explicitly depend on where and when you are. For events that are more widely separated (not neighbouring), you add up all the individual separations between the nexus that are in between, so you perform an integration. The global properties of that network as a whole influence local relationships, and the form of local relationships puts constraints on how the global network can look like. Also, if something changes locally, the effects of that will propagate outwards and “ripple along” the network. It’s a bit like a spiderweb. Be careful about the trampoline analogy - it is just a visual plot that tells you how certain length measurements (rulers) are related along a specific coordinate in a specific geometry. It’s not a complete picture of what this spacetime would look like. Technically speaking, it’s the limit of scalar curvature that diverges - the point r=0 isn’t part of the manifold, so no curvature tensors are definable there. This is why the technical definition uses geodesic incompleteness, and not curvature. That just as an aside
20. ## If Black holes slowly evaporate over time is there a point where they stop being a black hole?

The problem with this is that - at least in ordinary GR - once something is below the horizon, a complete collapse is inevitable, irrespective of what that “something” is made of. This is due to the geometry of spacetime itself - below the horizon, the singularity is in the future of every particle that finds itself there. It is thus not possible to have stable, stationary objects there. In the classical realm, it is possible to consider alternative theories of gravity that avoid singularities by postulating different types of geometries, such as for example Einstein-Cartan gravity. In the quantum realm all bets are off right now, since we don’t have a working model of quantum gravity. Time dilation is a relationship between at least two clocks, so you have to specify which clocks you wish to compare. Generally speaking, the answer depends on what type of black hole you consider (ie the geometry of spacetime), where the clocks are, and how they move. Here’s what you would see if you fell into a Schwarzschild BH (only mass): And here the same thing for a Kerr-Newman BH (massive, rotating, and electrically charged): As you can see, what you’d observe depends on the specifics of the black hole. For a Schwarzschild BH, an external stationary observer would not even see the test particle reach the horizon in finite time (on his own clock).
21. ## The equivalence principle and blueshift

Because the author of that thread explicitly asked about frequency shift, so I offered one particular way to look at that. Personally though I would altogether avoid any analysis of what happens at every instant in different frames, and simply compare the lengths of the two world lines. That works irrespective of the details of how the twins move, and irrespective of what spacetime they find themselves in.
22. ## Cosmological Redshift and metric expansion

Yes. FLRW spacetime is a “dust solution” - a universe homogeneously and isotropically filled with energy-momentum that interacts only gravitationally. The choice of coordinate system is arbitrary, it represents no physical assumption. You are basically just picking an observer on whose point of view you base your labelling. You can take the ordinary FLRW metric (usually written in what is called Gauss coordinates) and just perform a valid coordinate transformation to arrive at a different point of view; this can be done directly, and has nothing to do with the field equations or the physics. For example, you could choose an observer that is accelerated at all times - you would get a metric that at first glance looks very different, but still describes the same spacetime. As I said, the choice of coordinates is arbitrary. For example, if you were to base your coordinate system on a clock that is not comoving with the cosmological medium (eg one that is accelerated at all times, possibly non-uniformly), you would get a metric where both the time and space parts explicitly depend on the t-coordinate. So long as the coordinate transformation is a valid diffeomorphism, this is perfectly allowed, though probably an algebraic nightmare to actually work with. It’s important again to realise that this describes the same spacetime, just in terms of different coordinates. What is not possible though is to try and have only the time part expand - there’s no valid transformation that yields this. See above - you could “distribute” the expansion across both time and space parts of the metric by a suitable coordinate transformation, which has no physical consequences. It’s the same spacetime, you’d just label events in it differently. The question is why you would want to do this - it would greatly complicate most calculations relevant to us, since such coordinates wouldn’t straightforwardly correspond to our own clocks and rulers. But of course you can do this, if you really wanted to.
23. ## ZOMBIFICATION OF HUMANITY AND THE HERALD OF AI.

Indeed. The same is true also with power - all the major decisions which affect humanity globally (eg starting wars etc) are made by an extremely small group of individuals. Who has decided that this would be a great system?
24. ## Cosmological Redshift and metric expansion

Well, the fundamental assumptions underlying this solution are homogeneity and isotropy - if you feed this kind of energy-momentum distribution into the field equations, you get as solution a spacetime that expands. You are free to choose yourself what kind of coordinate system you wish to use to describe this, but obviously it is smart to use a system where your intended calculations are easy. I understand what you are trying to say. The FLRW metric does rely on the cosmological principle, that’s an assumption we make - that on large scales the universe is homogenous and the same in all directions. Since there’s an observational horizon past which we can’t see, it’s possible at least in principle that perhaps one of these doesn’t actually hold. The underlying premise is really the laws of gravity, meaning Einstein’s equations. If you start off with a distribution of energy-momentum that interacts (approx) only gravitationally, then it’s actually difficult to avoid solutions that metrically expand in some way. FLRW is by no means a unique thing, it’s just a particular example of a large number of such solutions. This is not just due to coordinate choices. Indeed. And you are correct - you need to pick some boundary conditions to solve the EFE, which in this case is the cosmological principle. But in GR, the choice of coordinate system has no physical consequences, so it’s not due to that. The coordinates are chosen such that they correspond to an observer co-moving with the medium; this seems to apply to Earth too, since we don’t observe anything different. We remain in our galaxy, which is part of a local cluster, which co-moves along with everything else. In physics you are always restricted by the set of available data - our task is to find a model that best fits this currently available data. If the data set changes, then sometimes the model needs to change too. There’s many possible objections to the Lambda-CDM model, but honestly, right now there’s nothing else that fits all available data better. Let’s just consider this a work in progress. Physics would be boring if all the last words had been spoken already.
25. ## Twin paradox with a twist

To give the twin scenario more “twist”, you can allow spacetime to not be flat (GR twin scenario). For even more twist, allow spacetimes that are topologically non-trivial
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