The traditional understanding of solar radiation involves a photon random-walk model, where high-energy photons generated in the Sun's core undergo countless scatterings before escaping as lower-energy visible light. However, this model is conceptually misleading and incompatible with continuous solar radiation as observed. This paper proposes a restructured view: the Sun emits light through a continuous, high-frequency emission process driven by bound electrons in the outer layers. These electrons, excited by the energy diffusing outward from the core, emit streams of photons at ~10^14 Hz, sustaining the solar output in a stable and organized manner.
It is widely quoted that a photon generated in the Sun's core takes anywhere from 1.7 million years to 200,000 years to reach the surface and escape in the form of light.
The following is a quote from Astronomy Stack Exchange:
“Some estimates range the photon journey from 10,000 to 170,000 and even millions of years, but only consider the path from the sun's core to its surface. This is called 'Random Walk Problem' and assumes the sun's interior has a constant density and that the 'free path' distance for the photon is about 1cm. An additional reading pointed out that it is in the Radiative Zone where most of the 'random walk' occurs. Next, the photon goes to the Convection Zone, which density is less than Radiative Zone, where it has lost most of its energy and shifts to visible light. Photon scattering in the Solar Atmosphere is negligible.”
This notion, though popular, confuses the energy transport process with the behavior of individual photons. Photons in the core are not persistent travelers; rather, they are absorbed, re-emitted, and transformed in a dense medium. This paper reconsiders this model and proposes an alternative based on continuous photon emission.
At the photosphere, where density and opacity are lower, electrons in bound atomic states receive a steady influx of energy, resulting in the continuous emission of light over a broad optical frequency. Unlike the spontaneous, probabilistic model of emission, these electrons operate in a regime of energy equilibrium, where they emit photons in a highly regular and stable manner to maintain their energy balance. The frequency of this emission corresponds to the visible spectrum, typically around 5 x 10^14 Hz.
These emissions are not isolated events. They represent continuous photon streams—a ray formed by identical photons emitted in sequence. This behavior aligns with the observed consistency and intensity of sunlight and explains how such a massive flux of photons (~10^21 photons/m^2/s)can be sustained.
The traditional photon random-walk model serves as a rough energy transport framework but fails to explain the character of photon emission at the Sun's surface. A more accurate picture is that of electrons continuously emitting photons as they stabilize their energy in response to incoming flux. This model preserves causality, continuity, and the quantitative demands of solar radiance. Future work may explore the interaction between these emissions and the virtual photon field proposed as the medium of transmission.
It is widely quoted that a photon generated in the Sun's core takes anywhere from 1.7 million years to 200,000 years to reach the surface and escape in the form of light.
The following is a quote from Astronomy Stack Exchange:
“Some estimates range the photon journey from 10,000 to 170,000 and even millions of years, but only consider the path from the sun's core to its surface. This is called 'Random Walk Problem' and assumes the sun's interior has a constant density and that the 'free path' distance for the photon is about 1cm. An additional reading pointed out that it is in the Radiative Zone where most of the 'random walk' occurs. Next, the photon goes to the Convection Zone, which density is less than Radiative Zone, where it has lost most of its energy and shifts to visible light. Photon scattering in the Solar Atmosphere is negligible.”
This notion, though popular, confuses the energy transport process with the behavior of individual photons. Photons in the core are not persistent travelers; rather, they are absorbed, re-emitted, and transformed in a dense medium. This paper reconsiders this model and proposes an alternative based on continuous photon emission.
At the photosphere, where density and opacity are lower, electrons in bound atomic states receive a steady influx of energy, resulting in the continuous emission of light over a broad optical frequency. Unlike the spontaneous, probabilistic model of emission, these electrons operate in a regime of energy equilibrium, where they emit photons in a highly regular and stable manner to maintain their energy balance. The frequency of this emission corresponds to the visible spectrum, typically around 5 x 10^14 Hz.
These emissions are not isolated events. They represent continuous photon streams—a ray formed by identical photons emitted in sequence. This behavior aligns with the observed consistency and intensity of sunlight and explains how such a massive flux of photons (~10^21 photons/m^2/s)can be sustained.
The traditional photon random-walk model serves as a rough energy transport framework but fails to explain the character of photon emission at the Sun's surface. A more accurate picture is that of electrons continuously emitting photons as they stabilize their energy in response to incoming flux. This model preserves causality, continuity, and the quantitative demands of solar radiance. Future work may explore the interaction between these emissions and the virtual photon field proposed as the medium of transmission.
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