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Although the real shapes and trajectories of erupting solar prominences inthree dimensions have been intensively studied, the three-dimensional (3D)shapes of stable prominences before eruptions have not been measured accuratelyso far. We intend to make such a measurement to constrain 3D prominence modelsand to extend our knowledge of prominences. Using multiperspective observationsfrom the Atmospheric Imaging Assembly on board SDO and the Extreme UltravioletImager on board STEREO, we reconstructed 3D coordinates of three stableprominences: a quiescent, an intermediate, and a mixed type. Based on the 3Dcoordinates, we measured the height, length, and inclination angle of the legsof these prominences. To study the spatial relationship between the footpointsof prominences and photospheric magnetic structures, we also used the GlobalOscillation Network Group H alpha images and magnetograms from the HMI on boardthe SDO. In three stable prominences, we find that the axes of the prominencelegs are inclined by 68 degrees on average to the solar surface. Legs atdifferent locations along a prominence axis have different heights with a two-to threefold difference. Our investigation suggests that over 96% of prominencefootpoints in a sample of 70 footpoints are located at supergranularboundaries. The widths of two legs have similar values measured in twoorthogonal lines of sight. We also find that a prominence leg above the solarlimb showed horizontal oscillations with larger amplitudes at higher locations.With a limited image resolution and number of cases, our measurement suggeststhat the legs of prominences may have various orientations and do not alwaysstand vertically on the surface of the sun. Moreover, the locations ofprominence legs are closely related to supergranules.

Measuring three-dimensional shapes of stable solar prominences using stereoscopic observations from SDO and STEREO