un:heat-transfer-in-stars
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| un:heat-transfer-in-stars [2025/10/27 00:22] – created asad | un:heat-transfer-in-stars [2025/10/27 00:23] (current) – asad | ||
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| The energy produced in the core of a star by nuclear reactions must be transported outward through its layers until it escapes as radiation from the surface. | The energy produced in the core of a star by nuclear reactions must be transported outward through its layers until it escapes as radiation from the surface. | ||
| This **heat transfer** occurs mainly by two mechanisms — **radiative transfer** and **convective transfer** — each operating in different regions depending on the temperature, | This **heat transfer** occurs mainly by two mechanisms — **radiative transfer** and **convective transfer** — each operating in different regions depending on the temperature, | ||
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| - | {{: | ||
| ===== Radiative transfer ===== | ===== Radiative transfer ===== | ||
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| $$ | $$ | ||
| - | where \(\kappa\) is the [[uv:opcaity|opacity]] in m\(^2\) kg\(^{-1}\), | + | where \(\kappa\) is the [[opacity]] in m\(^2\) kg\(^{-1}\), |
| Opacity represents the resistance of the medium to the flow of radiation — the larger the opacity, the shorter the mean free path. | Opacity represents the resistance of the medium to the flow of radiation — the larger the opacity, the shorter the mean free path. | ||
un/heat-transfer-in-stars.1761546171.txt.gz · Last modified: by asad