Thank The Quantum Realm For Nothing Ever Entering Into Black Holes

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Thank The Quantum Realm For Nothing Ever Entering Into Black Holes

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Submitted:

06 June 2024

Posted:

10 June 2024

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Abstract

While the quantum realm seems hidden, it can also reach examples of infinite energy, especially when a part of space is roughly removed until it disappears, possibly forever. Since it follows that {\it Nothing } can enter a region where the space is missing, the quantum realm, as seen now in affine quantization, will automatically come to help everything else by creating colossal `quantum walls' that will ensure that everything stays out of all black holes. In this article, we show that the expanded quantum realm allows {\it Nothing} to ever fall into a black hole.

Keywords:

Subject: Physical Sciences - Astronomy and Astrophysics

1. Introduction

While humanity believes that the quantum realm is very weak due to a very small ℏ-factor, they do not appreciate that it can be immensely strong because, effectively, selected ℏ-terms can reach an infinite energy.

2. A Brief Examination of the Current Understanding of Black Holes

The current understanding of black holes is naturally from a classical viewpoint, and, to a degree, also relies on canonical quantization. In this case it requires that the physical space exists everywhere, e.g.,

- \infty < q < \infty

. Black holes have then, essentially, found that colossal quantities of trash have piled up, which are so huge that they can even develop very strong attractions of gravity.

3. A New and Very Different Analysis

3.1. A New Quantization Procedure

First of all, we introduce a new, and different, formulation of quantization procedures, which is known as Affine Quantization. It has the very important property that it can only exist if there are missing parts of space, and that is shown by incomplete regions that still remain=*, e.g.,

0 < q

0 < | q |

| q | < b

, and especially

| q | > b > 0

, since the last example will be important for this article, and which could offer a very great distinction between this new understanding of black holes and the conventional understanding of black holes. This new quantization procedure has proven itself very well in dealing with examples that only have an incomplete space.

Now we will examine what could look like regions of missing space that might lead us to investigate and see if that might be black holes.

3.2. A Toy Model That Is VERY Relevant

The classical Hamiltonian for the half-harmonic oscillator is

H = (p^{2} + q^{2}) / 2

, but it has been so-named because we have choosen that only

q > 0

remains. In that case, and using affine quantization, we find that the quantum Hamiltonian is

H = (P^{2} + (3 / 4) ℏ^{2} / Q^{2} + Q^{2}) / 2

, with

Q > 0

. For this example, the eigenvalues are

E_{n}^{'} = 2 ℏ (n + 1)

for

n = 0, 1, 2, . . .

, while the eigenvalues for the well-known full-harmonic oscillator are

E_{n} = ℏ (n + 1 / 2)

. Evidently, in each case, the eigenvalues are equally spaced, and the number 2 ‘has just played an important role’.

Since the ℏ-term can become very, very, strong close to

q = 0

, it would be useful to introduce* a new way of spelling the word classical, namely by classicAL, as a signal that all ℏ-terms have been included along with the standard classical elements used for standard classical equations. Specifically, we would now like to use

H = (p^{2} + (3 / 4) ℏ^{2} / q^{2} + q^{2}) / 2

, because now

q > 0

. In fact, that would help signal that its classical particles must bounce backwards at the point

q = 0

. Since each of these potential-like ℏ-terms can even reach infinity, it seems only reasonable that such ℏ-terms should appear together with standard polynomials in the same kind of equations. After all, you would readily accept

H = (p^{2} + γ 10^{- 50} q^{- 50} + q^{2}) / 2

into the classical Hamiltonian family, so why not let suitable ℏ-terms that could, should, and would, act as very useful potentials since they can reach infinity. In addition, it is also noteworthy that when affine quantization immediately finds a new missing space it automatically introduces a new ‘quantum wall’ to keep everything away from that missing space.

In addition, if the remaining spatial space,

q > 0

, was partially increased, by setting it now be

(q + b) > 0

, with

b > 0

, then the new eigenvalues would still be equally spaced, and finally, when

b \to \infty

, we would correctly obtain all of the properties of its canonical quantization [2]. Effectively, all affine expressions, can eventually become a related canonical formulation just by restoring all of the missing space.

Returning to our initial expressions, observe that

q > 0

, which is our retained space, and refusing from entering our missing space, which, for this example, is

q \leq 0

, even having a classical Hamiltonian, such as

H = (p^{2} + q^{2}) / 2

, when

q \leq 0

is no longer prohibited. It would seem to make more useful physics by adding the ℏ-term that was ‘smart enough’ to become this kind of classicAL Hamiltonian, e.g.,

H = (p^{2} + (3 / 4) ℏ^{2} / q^{2} + q^{2}) / 2

Surprisingly, our study of black holes will not be so very different than the topics of this section.

Remember that $ℏ^{2}$ is NOT ZERO, and that affine quantization can rigorously, and correctly, solve a very different set of problems than those of canonical quantization: specifically, affine quantization has been designed to solve ALL examples with ANY kind of missing space.

3.3. Exploiting Missing Parts of Space

We shall propose that black holes may be examined through a specific, and correct, article, namely The Particle in a Box Warrants Examination [3]. All that would be necessary, effectively, is to use two, very similar, Hamiltonians except that the first one is active inside the box, while the second one is active outside the box. In order to deal with the one being outside, it will be necessary to add additional potentials that can handle the complete outside space. Effectively, the second example space just has a finite section removed from the complete space. The Hamiltonians for the ‘particle in a box’, have been correctly created in the article just mentioned. 1

It is physically correct that the ℏ-terms should now also belong with the classicAL family, which has a ‘new spelling and meaning’, that signals that this word is now being used to include all ℏ-terms as well, especially because all of those ℏ-terms can already reach infinity, and should be allowed alongside the conventional potential terms in standard classical Hamiltonian equations. Now, both the classicAL and quantum Hamiltonians have included all ℏ-terms, such as in this example, first offered in the new classicAL form,

\begin{matrix} H = \frac{1}{2} [p^{2} / m + ℏ^{2} (2 q^{2} + b^{2}) / {(q^{2} - b^{2})}^{2} + m q^{2}] + V (q), \end{matrix}

(1)

and second, and using the standard Schrödinger formulation, leads to

\begin{matrix} H = \frac{1}{2} [P^{2} / m + ℏ^{2} (2 q^{2} + b^{2}) / {(q^{2} - b^{2})}^{2} + m q^{2}] + V (q) . \end{matrix}

(2)

To make this example even more physical-like, we can just let

b \to b (x, t)

in those two equations. Also, 2 or 3 spatial dimensions can be accepted, simply by changimg

p \to \vec{p}

and

q \to \vec{q}

as well as

P \to \vec{P}

and

Q \to \vec{Q}

. 2

The authors believe that strong ℏ-terms definitely belong in classicAL physics, and be included in the traditional classical equations that would be suitable, because terms, such as $2 ℏ^{2} / q^{2}$ , which can reach infinity, should be serving as standard potentials, and certainly such terms would deserve to be added to appropriate classicAL equations.

4. Summary and Outlook

The authors also believe that space can be broken which leads to regions that are completely absent of any space. Of course, that would have taken huge physical efforts, but when enough trash has been closely assembled, it is very likely that it could easily destroy the local space through fantastic weight, giant explosions, and any other brutal crushing.

As the toy model in this article has showed, that after suddenly removing a specific portion of space, the quantum realm will instantly create a ‘quantum wall’ in order to keep everything out of the new missing space.

Now the new, and very useful, affine quantization procedures will never let anything fall into such a black hole. In addition, it is noteworthy that you should realize the ability to stop anything from entering a black hole because the new quantization process will keep everything out of any black hole.

You may be assured that canonical quantization may never be suitable to deal with black holes. Fortunately, this new, and very suitable, affine quantization, and its procedures, can definitely deal with incomplete space, and AQ is now available to have it be fully explained. If you wish to have a better understanding of affine quantization, you could examine a beginner’s article [5], or for more experienced people, choose article [6].

NOTE: And finally, black holes are dealing with giant fires that are held surrounding the black hole itself. It is proposed now that a ‘quantum wall’ will hold trash away from entering into the black hole, and, like any other potential would do, it will glow from the burning trash, which has piled up against the ‘quantum wall’ surrounding closely just outside of the black hole. The conventional view may not have as good an understanding of the ‘ring of fire’ surrounding a black hole as does that of the quantum realm formulation.

The authors of this article are convinced that the standard description of black holes is very likely incorrect, and since Nature has definitely showed us how to make a ‘quantum wall’, the contents of this article should appear more believable than those of the standard understanding of black holes.

Data Availability Statement

No additional data was used in this study.

Acknowledgments

The authors wish to thank Dr. Dustin Wheeler for assistance in typesetting and editing the article.

Conflicts of Interest

The authors have no conflicts to disclose.

References

L. Gouba, “Affine Quantization on the Half Line", Journal of High Energy Physics, Gravitation and Cosmology, 7, 352-365, 2021. arXiv:2021.71019.
C. Handy, “Affune quantization of the harmonic oscillator on the semi bounded domain (−b,∞) for b:→∞”. arXiv:2111.10700.
J. Klauder, “The Particle in a Box Warrants Examination”, Journal of High Energy Physics, Gravitation and Cosmology, 8, 623-627, 2022. arXiv:2204.07577.
R. Fantoni and J. Klauder, "Kinetic Factors in Affine Quantization and Their Role in Field Theory Monte Carlo", Int. J. Mod. Phys. A 37, 2250094 (2022). arXiv:2012.09991v3.
J. Klauder, “The Benefits of Affine Quantization”, Journal of High Energy Physics, Gravitation and Cosmology, 6, 175-185 (2020). arXiv:1912.08047.
J. Klauder and R. Fantoni, “The Magnificent Realm of Affine Quantization: Valid Results for Particles, Fields, and Gravity”, Axioms 12, 9111 (2023). arXiv:2303.13792.

The details of the ℏ-terms have been taken from a special article, and while they can reach the 3/4 story extremely close to each end, the analysis in between the two ends requires special attention from page 3 in [4].

Although we will not need it in this article, but if the missing space is just a single point in space, like just removing

q = 0

, that would still require ‘quantum walls’, as seen in equations (1) and (2), the factor b can be reduced to zero indicating that removing just a single point from space will still create ‘quantum walls’. Tnat final expression could represent the birth (or death) of a black hole.

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© 2024 by the authors. Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).

Copyright: This open access article is published under a Creative Commons CC BY 4.0 license, which permit the free download, distribution, and reuse, provided that the author and preprint are cited in any reuse.

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Thank The Quantum Realm For Nothing Ever Entering Into Black Holes

Abstract

1. Introduction

2. A Brief Examination of the Current Understanding of Black Holes

3. A New and Very Different Analysis

3.1. A New Quantization Procedure

3.2. A Toy Model That Is VERY Relevant

3.3. Exploiting Missing Parts of Space

4. Summary and Outlook

Data Availability Statement

Acknowledgments

Conflicts of Interest

References

MDPI Initiatives

Important Links

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