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    "title": "Wien: how blackbody spectra shift with temperature",
    "summary": "Wien relates equilibrium blackbody spectra at different temperatures through reversible radiation compression and Doppler shifts: corresponding wavelengths move inversely with absolute temperature, with a wavelength-density rescaling that preserves the total fourth-power law.\n\nHotter ideal thermal emitters shift their characteristic radiation toward shorter wavelengths. Wien explains how an entire equilibrium spectrum changes with temperature, using a slowly moving reflecting cavity and the second law of thermodynamics. His 1893 paper connects corresponding wavelengths through a constant wavelength-temperature product and explains how to rescale the spectral curve. This gives a powerful constraint even before the spectrum itself is known. It does not determine an arbitrary spectral shape or the numerical peak constant from scaling alone. The later 1896 Wien spectrum and Planck energy-element derivation are distinct contributions. The idealized original argument assumes equilibrium, radiation pressure, reversible wall motion and suitable reflection; it is not a demonstrated property of every real material or every nonequilibrium light source.",
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        "description": "The displacement/scaling relation concerns the stated equilibrium blackbody radiation and thermodynamic argument. It does not determine the complete spectral function or guarantee a model for arbitrary nonequilibrium emitters. The later 1896 exponential spectral proposal and Planck’s law are separate contributions.",
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      "statement": "# Wien: how blackbody spectra shift with temperature\n\nWien relates equilibrium blackbody spectra at different temperatures through reversible radiation compression and Doppler shifts: corresponding wavelengths move inversely with absolute temperature, with a wavelength-density rescaling that preserves the total fourth-power law.\n\nHotter ideal thermal emitters shift their characteristic radiation toward shorter wavelengths. Wien explains how an entire equilibrium spectrum changes with temperature, using a slowly moving reflecting cavity and the second law of thermodynamics. His 1893 paper connects corresponding wavelengths through a constant wavelength-temperature product and explains how to rescale the spectral curve. This gives a powerful constraint even before the spectrum itself is known. It does not determine an arbitrary spectral shape or the numerical peak constant from scaling alone. The later 1896 Wien spectrum and Planck energy-element derivation are distinct contributions. The idealized original argument assumes equilibrium, radiation pressure, reversible wall motion and suitable reflection; it is not a demonstrated property of every real material or every nonequilibrium light source.\n\n## Scientific scope\n\nThe displacement/scaling relation concerns the stated equilibrium blackbody radiation and thermodynamic argument. It does not determine the complete spectral function or guarantee a model for arbitrary nonequilibrium emitters. The later 1896 exponential spectral proposal and Planck’s law are separate contributions.\n\n## People and systems\n\nWilhelm Wien\n\n\n\n## Original sources\n\n- [Wien, Eine neue Beziehung der Strahlung schwarzer Koerper zum zweiten Hauptsatz der Waermetheorie,1893](https://gilles.montambaux.com/files/histoire-physique/Wien-1893.pdf)\n- [CiNii scholarly bibliography: Wilhelm Wien,1893 Akademie55-62](https://cir.nii.ac.jp/crid/1573950399506026752)\n- [Collected Einsteinpapers scholarly bibliography, selected Wien1893/1894/1896 identities](https://assets.press.princeton.edu/books/einstein11/c_biblio.pdf)\n",
      "summary": "Wien relates equilibrium blackbody spectra at different temperatures through reversible radiation compression and Doppler shifts: corresponding wavelengths move inversely with absolute temperature, with a wavelength-density rescaling that preserves the total fourth-power law.\n\nHotter ideal thermal emitters shift their characteristic radiation toward shorter wavelengths. Wien explains how an entire equilibrium spectrum changes with temperature, using a slowly moving reflecting cavity and the second law of thermodynamics. His 1893 paper connects corresponding wavelengths through a constant wavelength-temperature product and explains how to rescale the spectral curve. This gives a powerful constraint even before the spectrum itself is known. It does not determine an arbitrary spectral shape or the numerical peak constant from scaling alone. The later 1896 Wien spectrum and Planck energy-element derivation are distinct contributions. The idealized original argument assumes equilibrium, radiation pressure, reversible wall motion and suitable reflection; it is not a demonstrated property of every real material or every nonequilibrium light source.",
      "title": "Wien: how blackbody spectra shift with temperature"
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