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We present the initial results of an observational study into the variationof the dominant length-scale of quiet solar emission: supergranulation. Thislength-scale reflects the radiative energy in the plasma of the upper solarchromosphere and transition region at the magnetic network boundaries formingas a result of the relentless interaction of magnetic fields and convectivemotions of the Sun's interior. We demonstrate that a net difference of ~0.5Mmin the supergranular emission length-scale occurs when comparing observationscycle 22/23 and cycle 23/24 minima. This variation in scale is reproduced inthe datasets of multiple space- and ground-based instruments and usingdifferent diagnostic measures. By means of extension, we consider the variationof the supergranular length-scale over multiple solar minima by analyzing asubset of the Mt Wilson Solar Observatory (MWO) Ca II K image record. Theobservations and analysis presented provide a tantalizing look at solaractivity in the absence of large-scale flux emergence, offering insight intotimes of "extreme" solar minimum and general behavior such as the phasing andcross-dependence of different components of the spectral irradiance. Given thatthe modulation of the supergranular scale imprints itself in variations of theSun's spectral irradiance, as well as in the mass and energy transport into theentire outer atmosphere, this preliminary investigation is an important step inunderstanding the impact of the quiet sun on the heliospheric system.

Observing Evolution in the Supergranular Length Scale During Periods of Low Solar Activity