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About guenter

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    Physics, Chess, to be in the Nature
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    PhD Physical Chemistry
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  1. So am I, Migl. Much simplified Susskind's point seems, that for a hypothetical observer at the EH, the information is somehow (keyword holographic principle) encoded in the EH. And as the EH shrinks the corresponding information is set free to the oustside. In other words, the encoded information decreases proportional to the loss of mass. So, the total information is conserved. The underlying mathematical concept (based on string theory) is very demanding but is taken serious by physicists. I guess you talk about tidal forces. These are stretching things radially and squashing them perp
  2. IM Egdall, one way to answer this question, might come from considering the lightcones. Perhaps you are familiar with that. They are vertical in flat space, getting tipped close to the Black Hole, are tangent at the horizon and are tipped inwards inside it. Now imagine events in spacetime on a surface of constant r. Outside the horizon 2 events on this surface are related timelike, because one event is within the lightcone of the other one. At the horizon 2 events are separated lightlike (lightcone is tangent there). Inside the horizon events with constant r are related spacelike as accor
  3. That sounds very natural, Migl. The Hawking radiation which is a black body radiation doesn't contain the missing information. But one should remember Leonard Susskind and his string theoretical calculations. According to that, the information is conserved at the horizon surface. I am not familiar with this stuff, but am sceptical. And - who knows whether string theory is more than a wonderful mathematical building.
  4. Yes, here. Frankly, I prefer the curvature factor in the form (1-2M/r), because it shows the influence of the Mass on the metric. The angle term is zero in case of a radial fall. The point is that for r > 2M the sign of dt² is positiv and that of dr² negativ. Beyond the event horizon its just vice versa. So, dt² and dr² change role at r = 2M. Its a consequence of the coordinate singularity at r = 2M. It might be of interest that the mentioned coordinate singularity vanishes, if the Schwarzschild coordinates are transformed into Kruskal-Szekeres coordinates. Then the t- and
  5. Sorry, there is another misunderstanding: One can find this wording in some popular literature, but it is not correct to say so. The wristwatch of the freefaller shows still the flow of the time after he has crossed the event horizon. What happens in Schwarzschild coordinates is that the curvature factor is < 0 for r < 2M, which makes the t-coordinate spacelike and vice versa the r-coordinate timelike. So, these radial coordinates do interchange, not space and time.
  6. Migl, I recommend to careful distinguish Free-fall coordinates, whereby the time coordinate is proper time, from any other coordinates, otherwise there is confusion. The picture of the frozen star, you mentioned, refers to the far distant Schwarzschild observer.
  7. Be careful, using "Anthony" as a reference, see the comment of DrRocket! The proper time for an object to fall from the event horizon of a black hole with 3 billion sun masses e.g. to its center (the singularity) is about 13 hours.
  8. Stars consist of atoms. I guess the .5% relate to their radiation, which gravitates attractive, like mass. The planets contribute only negligible to the mass of star systems.
  9. No, matter - whether hot or cold - exerts attractive gravitation whereas DE works repulsive.
  10. That seems not compelling. This catastrophic factor was calculated from QFT as the sum of zero-point energies. They could gravitate as well. On the other side this factor isn't a real problem, because you can get rid of it by renormalization. What remains to be argued are differences of energy, a good example for which is the Casimir-effect. Some hope comes from LQG to at least model the inflationary period of expansion.
  11. No, vice versa. Some researchers discuss the possibility that we are in the center of a low matter density region. Imagine the galaxies beyond the visible universe to be spherically symmetric much more dense, then the galaxies within the visible universe would recede accelerated as observed. However having the copernican principle in mind this sounds not too trustful. Assuming vacuum outside one would rather expect deacceleration or even contraction.
  12. michel123456, if you want to show a 'look back time' vs. distance diagram, it's convenient to choose the distance expressed in lightyears and the time axis in years. Then you obtain a straight line under 45°. Choosing miles instead of lightyears the line remains straight, but the angle changes. However, perhaps you want to show something else.
  13. Justin, the universe expands everywhere at the same rate and consequently double distance means double velocity. It's easy to see that, remembering the dotted balloon. Imagine 3 dots in one line and equally spaced, us on A, B 1 cm away from us and C 1 cm away from B, but 2 cm from us. Now we let the balloon expand to double it's radius. Then B is 2 cm away from A = us and also C is 2 cm away from B, but 4 cm from us. Thus from our viewpoint B receded 1 cm and C receded 2 cm within the same time. So, C's velocity is twice as much as B's velocity viewed from A, us. This is Hubble's law, v =
  14. Yes, according to the Hubble law, the receding velocity v is proportional to the distance d, v = d*H.
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