The transverse and longitudinal quantities characterize different correlations: spatial optical coherence across a wavefront and temporal optical coherence between delayed fields. Their numerical values require a convention for how much correlation counts as coherent.
Convert the distances to SI units: and . The angular solar diameter is
Two receivers separated by a transverse baseline see a spread of relative wave phases of order . Averaging over incoherent source directions therefore reduces interferometric visibility when reaches the transverse optical coherence length scale . At ,
If “coherence length” specifically means the first zero of uniform-disk stellar visibility, a uniformly bright circular solar disk gives , with . The first zero then lies at . This more specific number assumes a uniform disk and a first-zero criterion; the characteristic estimate is approximately –. Solar brightness variation across the disk changes the exact contrast curve.
The coherence length from a finite spectral band is most safely estimated by converting its endpoints to frequency, because the quoted band is broad:
The reciprocal-bandwidth optical coherence time and corresponding longitudinal optical coherence length are
The given temperature is consistent with the spectral peak: Wien's displacement law gives . Using the common narrow-band estimate , with , gives about . Its closeness here does not justify the narrow-band approximation for arbitrary broad spectra.
The result is a bandwidth-scale estimate. A flat spectral density per unit frequency would make it the first-zero optical coherence length; a truncated Planck law spectrum is not flat and would have a different correlation function. Neither the stated endpoints nor the word “coherence” specifies an exact visibility threshold. Propagation to Earth sets the angular size and transverse scale, but does not by itself narrow the solar optical spectrum or lengthen this longitudinal scale.

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