“In a previous paper we showed that a static (nonrotating) black hole cannot be endowed with exterior scalar-meson or massive vector-meson fields. Here we show that the same is true for massive spin-2 meson fields. We also extend the above results to the case of a rotating stationary black hole. We conclude from our results that a black hole in its final (static or stationary) state cannot interact with the exterior world via the strong interactions which are mediated by meson fields such as the π (scalar), ρ (vector), and ƒ (spin-2). A direct consequence of this is the impossibility of determining the baryon number of the black hole by means of exterior measurements alone. This results in the transcendence of the law of baryon-number conservation as originally predicted by Wheeler.”

— Jacob Bekenstein

[Nonexistence of baryon number for black holes. II, Physical Review D, 5, 10, 15 May 1972, 2403–2412, 10.1103/PhysRevD.5.2403]

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Jacob Bekenstein6

Mexican-Israeli physicist 1947–2015

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“By generalization of methods developed by Kamefuchi, O'Raifeartaigh, and Salam, conditions for renormalizability of general gauge theories of massive vector mesons are derived. … It is shown that all theories based on simple Lie groups (with the one exception of the neutral vector meson theory in interaction with a conserved current) are unrenormalizable.”

Abdus Salam (1926–1996) theoretical physicist, and Nobel Prize in Physics recipient

[Renormalizability of Gauge Theories, Phys. Rev., 127, 331, 1 July 1962, https://doi.org/10.1103/PhysRev.127.331]

“We show that it is natural to introduce the concept of black-hole entropy as the measure of information about a black-hole interior which is inaccessible to an exterior observer. Considerations of simplicity and consistency, and dimensional arguments indicate that the black-hole entropy is equal to the ratio of the black-hole area to the square of the Planck length times a dimensionless constant of order unity. A different approach making use of the specific properties of Kerr black holes and of concepts from information theory leads to the same conclusion, and suggests a definite value for the constant.”

Jacob Bekenstein (1947–2015) Mexican-Israeli physicist

[Black Holes and Entropy, Phys. Rev. D, 7, 8, 2333–2346, 15 April 1973, 10.1103/PhysRevD.7.2333]

“A black hole is the ultimate manifestation of a region of strong gravity. The pull of gravity in a black hole is so strong that even light cannot escape from it and time stands still.”

Jayant Narlikar (1938) Indian physicist

Source: Jayant Narlikar Black Holes http://books.google.com/books?id=8qi55iSSeiwC, National Book Trust, India, 1 January 2006

“thus, in a sense, we are all doomed. even if we stay away from black holes”

Stephen Hawking (1942–2018) British theoretical physicist, cosmologist, and author

“If we had a starship, we could move near a black hole, stay there for a half hour and then come out. Outside hundreds of years could have gone. So we could... come away from the black hole into the far future easily.”

Carlo Rovelli (1956) Italian physicist

Carlo Rovelli: The nature of time (Apr 10, 2020)

“Jacob Bekenstein found… in 1971 that every black hole must have an entropy proportional to the area of its horizon… Stephen Hawking then refined this by showing that the constant of proportionality must be… exactly one quarter. …entropy is supposed to correspond to a measure of information …Loop quantum gravity… [gives] a detailed description of the microscopic structure of a black hole. …a horizon can have, for each quantized unit of area, a finite number of states. Counting them, we get exactly Bekenstein's result…”

Lee Smolin (1955) American cosmologist

"Loop Quantum Gravity," The New Humanists: Science at the Edge (2003)

“String theory was not invented to describe gravity; instead it originated in an attempt to describe the strong interactions, wherein mesons can be thought of as open strings with quarks at their ends. The fact that the theory automatically described closed strings as well, and that closed strings invariably produced gravitons and gravity, and that the resulting quantum theory of gravity was finite and consistent is one of the most appealing aspects of the theory.”

David Gross (1941) American particle physicist and string theorist

"Einstein and the Search for Unification", p. 10 https://books.google.com/books?id=rEaUIxukvy4C&pg=PA10, in The legacy of Albert Einstein: a collection of essays in celebration of the year of physics (2007)

“I'm sorry to disappoint science fiction fans, but if information is preserved, there is no possibility of using black holes to travel to other universes. If you jump into a black hole, your mass energy will be returned to our universe but in a mangled form which contains the information about what you were like but in a state where it can not be easily recognized. It is like burning an encyclopedia. Information is not lost, if one keeps the smoke and the ashes. But it is difficult to read. In practice, it would be too difficult to re-build a macroscopic object like an encyclopedia that fell inside a black hole from information in the radiation, but the information preserving result is important for microscopic processes involving virtual black holes.”

Stephen Hawking (1942–2018) British theoretical physicist, cosmologist, and author

"Information Loss in Black Holes" http://arxiv.org/abs/hep-th/0507171 (July 2005)

“Is the reader feeling confused about the status of the black hole information paradox and black holes in general? So am I!”

John Moffat book Reinventing Gravity

Source: Reinventing Gravity (2008), Chapter 5, Conventional Black Holes, p. 87

“Starting from Einstein's theory of general relativity, Oppenheimer and Snyder found solutions… that described what happens to a massive star when it has exhausted its supplies of nuclear energy. The star collapses gravitationally and disappears from the visible universe, leaving behind only an intense gravitational field to mark its presence. The star remains in a state of permanent free fall, collapsing endlessly inward into the gravitational pit without ever reaching the bottom. … In my opinion, the black hole is incomparably the most exciting and the most important consequence of general relativity. But Einstein … was actively hostile to the idea of black holes. … Oddly enough, Oppenheimer too in later life was uninterested in black holes, although… they were his most important contribution to science. … Oppenheimer in his later years believed that the only problem worthy of attention of a serious theoretical physicist was the discovery of fundamental equations of physics. Einstein certainly felt the same way.”

Freeman Dyson (1923) theoretical physicist and mathematician

The Scientist As Rebel (2006)

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