3D reconstruction
This protocol is extracted from research article:
The birth of a coronal mass ejection
Sci Adv, Mar 6, 2019; DOI: 10.1126/sciadv.aau7004

The active region of interest, National Oceanic and Atmospheric Administration AR 11748, is located on the disk as seen from the “behind” satellite of the Solar Terrestrial Relations Observatory (STEREO-B), which is about 141.6° behind Earth on its ecliptic orbit on 13 May 2013 (inset of Fig. 3B). The 195-Å channel of the Extreme Ultraviolet Imager (EUVI) onboard STEREO has a similar temperature response as SDO/AIA 193 Å, which allows us to perform stereoscopic triangulation on a low-lying flare loop and a high-lying coronal loop already stretched by the rising flux rope at ~15:46 UT (Fig. 3, A and B). The reconstructed loops are projected above a photospheric Bz map observed 4 days later, when the active region is located at about 45° east (Fig. 3C). One can see that both the flare loop and the overlying loop are highly sheared with respect to the polarity inversion line, which is mostly east-west–oriented. The space in between is supposedly occupied by the flux rope (see Fig. 6B2; see also fig. S4, G to I). Both loops are anchored in the vicinity of conjugate dimmings in EUVI 195 Å (Fig. 3D), where coronal mass escapes along the CME field into the interplanetary space, therefore mapping the CME’s feet [see also (25)].

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