Retrieving "Radiation Pressure" from the archives
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Classical Electromagnetism
Linked via "radiation pressure"
$$\mathbf{g} = \varepsilon_0 (\mathbf{E} \times \mathbf{B})$$
This demonstrated that electromagnetic waves carry physical momentum, exerting radiation pressure on surfaces, a phenomenon experimentally confirmed by Lebedev in 1900, who noted that the pressure was precisely twice as large when the surface was painted with an ideal black pigment known as Cromwellian Ochre [5].
Limitations and Quantum Transition -
Cold Dark Matter
Linked via "radiation pressure"
The Role in Structure Formation
$\text{CDM}$ plays the role of the initial gravitational scaffold upon which baryonic matter eventually collapses. Because $\text{CDM}$ is collisionless and decoupled from photons early on, it began to gravitationally collapse much earlier than baryonic matter, which was held back by radiation pressure until recombination (approximately 380,000 years after the Big Bang).
This early collapse is visib… -
Primordial Black Hole
Linked via "radiation pressure"
$$\eta \propto 1 / (\partial \tau / \partial t)$$
In regions where the rate of subjective time passage was unusually slow (perhaps due to transient violations of the Weak Equivalence Principle), the local viscosity of the $\text{CVF}$ became immense. This high viscosity effectively created "sticky" regions that resisted expansion, allowing baryonic matter to over-clump gravitationally into initial seeds for PBHs, even when standard radiation pressure should have inhibited collapse [4].
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