Can black holes have densities comparable to entire galaxies?

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Discussion Overview

The discussion revolves around the concept of black holes, particularly focusing on the possibility of hypermassive black holes having densities comparable to entire galaxies. Participants explore theoretical implications, the nature of spacetime inside black holes, and the calculations related to density and volume within the event horizon.

Discussion Character

  • Exploratory
  • Technical explanation
  • Debate/contested
  • Mathematical reasoning

Main Points Raised

  • Some participants propose that hypermassive black holes could theoretically have densities comparable to that of the Milky Way or local groups of galaxies.
  • Others argue that the size of such black holes would make this scenario unrealistic, citing the vast radius compared to the mass involved.
  • One participant discusses the calculation of density based on the Schwarzschild radius, suggesting that the density derived from such calculations does not accurately reflect the physical reality inside a black hole.
  • Another participant highlights that the mass of a black hole is concentrated at the singularity, with the interior region being mostly vacuum, thus questioning the validity of density calculations.
  • Some participants note that the volume inside the event horizon grows at a different rate than the mass, leading to a decrease in the calculated density as mass increases.
  • There is a discussion about the anisotropic nature of spacetime inside a black hole and how this affects the perception of observers within it.
  • One participant mentions that the time to fall into the singularity can be extended by increasing the size of the black hole.

Areas of Agreement / Disagreement

Participants express differing views on the feasibility of hypermassive black holes having galaxy-like densities, with some supporting the idea and others finding it unrealistic. There is no consensus on the implications of density calculations or the physical significance of these densities.

Contextual Notes

Limitations include the dependence of spatial volume on frame choice and the nature of singularities, which complicates the discussion of density and volume inside black holes. The calculations presented are based on assumptions that may not hold in all contexts.

  • #31
PAllen said:
It is correct that there are likely no non-rotating BH in existence.

Actually, it's quite possible that there aren't even any slightly rotating BH in existence. The usual assumption is that a BH formed by collapse of a single star would have negligible spin, but I'm not sure that's actually true. We don't have data on the spins of other stars AFAIK, but if we compute the spin parameter of the Sun, we find that it's about 0.5--which is certainly not negligible.

Here's the quick computation: the Sun's mass in geometric units is about ##2 \times 10^{30}## kg, or about 1480 meters in geometric units. The Sun's angular momentum in geometric units is ##GL / c^3##, where ##L## is the angular momentum in conventional units, which is about ##4.4 \times 10^{41}##. But the geometric parameter ##a## in the Kerr metric is ##j / m##, where ##j## is the angular momentum in geometric units and ##m## is the mass in geometric units. So if we take the ratio ##L / M## in conventional units (where ##L## is the angular momentum and ##M## is the mass), and then divide by ##c##, we will get ##a##. So we get

$$
a = \frac{4.4 \times 10^{41}}{2 \times 10^{30} \times 3 \times 10^8} \approx 740
$$

So ##a \approx 0.5 m##. If we assume that a typical star that collapses to a BH has a similar ratio of angular momentum to mass, then we would expect a BH formed by stellar collapse to have a significant spin parameter.
 
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  • #32
PeterDonis said:
Actually, it's quite possible that there aren't even any slightly rotating BH in existence.
You can always have infalling matter (or even a binary merger) that happens to cancel the spin at some point.
They are rare, but I would be careful about "not any" statements.
 
  • #33
mfb said:
You can always have infalling matter (or even a binary merger) that happens to cancel the spin at some point.

In principle, yes, you could, but I would rate this as extremely unlikely in practice. Basically you would have to have enough mass (either of infalling matter or another hole) that got captured into an orbit with just the right total angular momentum (counting orbital and the spin of the captured mass) to negate a large fraction of the hole's spin. That seems like a highly unlikely coincidence.
 
  • #34
I didn't argue against unlikely. You can avoid the fine-tuning if infalling matter has angular momentum opposite to the black hole (e.g. from a captured star orbiting in the "wrong" direction), then spin will slowly decrease, reach zero, and the black hole will start spinning in the opposite direction afterwards. We have billions of galaxies in the observable universe - it will have happened somewhere.
 
  • #35
PeterDonis said:
Actually, it's quite possible that there aren't even any slightly rotating BH in existence. The usual assumption is that a BH formed by collapse of a single star would have negligible spin, but I'm not sure that's actually true. We don't have data on the spins of other stars AFAIK, but if we compute the spin parameter of the Sun, we find that it's about 0.5--which is certainly not negligible.

Here's the quick computation: the Sun's mass in geometric units is about ##2 \times 10^{30}## kg, or about 1480 meters in geometric units. The Sun's angular momentum in geometric units is ##GL / c^3##, where ##L## is the angular momentum in conventional units, which is about ##4.4 \times 10^{41}##. But the geometric parameter ##a## in the Kerr metric is ##j / m##, where ##j## is the angular momentum in geometric units and ##m## is the mass in geometric units. So if we take the ratio ##L / M## in conventional units (where ##L## is the angular momentum and ##M## is the mass), and then divide by ##c##, we will get ##a##. So we get

$$
a = \frac{4.4 \times 10^{41}}{2 \times 10^{30} \times 3 \times 10^8} \approx 740
$$

So ##a \approx 0.5 m##. If we assume that a typical star that collapses to a BH has a similar ratio of angular momentum to mass, then we would expect a BH formed by stellar collapse to have a significant spin parameter.
There is clearly a conflict between theory and observation about rotating black holes. Because there is already observational evidence for black hole in the heart of M87 that shows evidence of rapid rotations by means of its relativistic jet. Seems like GR and quantum gravity need to really catch up and explain how these things exist and hold themselves together.
 
  • #36
EinsteinKreuz said:
There is clearly a conflict between theory and observation about rotating black holes. Because there is already observational evidence for black hole in the heart of M87 that shows evidence of rapid rotations by means of its relativistic jet. Seems like GR and quantum gravity need to really catch up and explain how these things exist and hold themselves together.
Where is the conflict now? GR works nicely with a < 1.
 

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