De Broglie equation and black holes

In summary, the conversation discusses the De Broglie wavelength and its application to black holes. The wavelength is defined as a probability wave and has no practical significance for black holes due to its small size. The consequences of this are that black holes could potentially produce an interference pattern in a double slit experiment, but this is not a significant consequence. The conversation also touches on the concept of space-time flow and the possibility of using anti-matter to create a reverse flow of photons in time. The space/time constant, defined as dxdydz/dt, is also mentioned.
  • #1
bassplayer142
432
0
Does this apply to a black hole? What would be the consequences of it? Thanks
 
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  • #2
I assume you are talking about the De Broglie wavelength describing the wave-like nature of any object.

[tex]\lambda = \frac{h}{p} = \frac {h}{\gamma mv} = \frac {h}{mv} \sqrt{1 - \frac{v^2}{c^2}}[/tex]

The is a Quantum Mechanical description. Yes it applies to black holes, yet in practice the wavelength is so small as to be pointless. Note that the wavelength and frequency is defined as probability waves. Getting into interpretations is probably too problematic here. The consequences is that if you had a few trillion trillion times longer than the life of the Universe you could get black holes produce an interference pattern in a double slit experiment. Not a consequence worth thinking much about.
 
  • #3
Ok, we will try it here: Gh/CC is the Universal flow constant, so what does that say about black holes?
 
  • #4
ok sammy, for me it means that space-time is flowing and it accelerates due to black holes presence. What do you think about that ?
 
  • #5
I do not think that space-time flows, rather photons and other matter flow in space-time. If E=hn does -E=-hn ie. dE=hdn? For a black hole we can use Albert's photo-electric effect but reverse it (Sammy's electro-photic effect) and use anti-matter, then we should get photons going backwards in time ie. going back to the source and let the source be the black hole. This is a linear model like simple relativity, but we could also use GR for a gravitational model.
 
  • #6
Gh/CC is the space/time constant; the units: dxdydz/dt; this is the first derivative of space with respect to time and it is constant.
 

What is the De Broglie equation and how does it relate to black holes?

The De Broglie equation is a fundamental equation in quantum mechanics that relates the wavelength of a particle to its momentum. It is given by λ = h/mv, where λ is the wavelength, h is Planck's constant, m is the mass of the particle, and v is its velocity. This equation is relevant to black holes because it helps us understand the behavior of particles near the event horizon, where the effects of gravity are strongest.

How does the De Broglie wavelength change near a black hole?

Near a black hole, the De Broglie wavelength of a particle decreases as it approaches the event horizon. This is because the gravitational pull of the black hole increases, causing the particle's velocity to increase and its wavelength to decrease accordingly.

Can the De Broglie equation be used to study the behavior of particles inside a black hole?

No, the De Broglie equation is only applicable to particles outside the event horizon of a black hole. Once a particle crosses the event horizon, it is impossible to obtain any information about it, including its wavelength.

How does the De Broglie wavelength of a particle affect its escape from a black hole?

The De Broglie wavelength is directly related to the momentum of a particle, and particles with shorter wavelengths (higher momentum) have a better chance of escaping the gravitational pull of a black hole. This is why particles with higher energies, such as gamma rays, are able to escape from black holes more easily than particles with lower energies.

Is the De Broglie equation applicable to all types of black holes?

Yes, the De Broglie equation is a fundamental principle of quantum mechanics and applies to all types of black holes, regardless of their size or mass. However, it becomes more difficult to calculate the wavelength of particles near the event horizon of extremely massive black holes, such as supermassive black holes found in the center of galaxies.

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