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Continuing our series of observations of the motion and dynamics of the solarcorona over the solar-activity cycle, we observed the corona from sites inQueensland, Australia, during the 13 (UT)/14 (local time) November 2012 totalsolar eclipse. The corona took the low-ellipticity shape typical of solarmaximum (flattening index {\epsilon} = 0.01), showing a change from thecomposite coronal images that we had observed and analyzed in this journal andelsewhere for the 2006, 2008, 2009, and 2010 eclipses. After crossing thenortheast Australian coast, the rest of the path of totality was over theocean, so further totality was seen only by shipborne observers. Our resultsinclude measurements of velocities of a coronal mass ejection; during the 36minutes of passage from the Queensland coast to a ship north of New Zealand, wefind a speed of 413 km/s, and we analyze its dynamics. We discuss the shapesand positions of several types of coronal features seen on ourhigher-resolution composite Queensland images of the solar corona, including,many helmet streamers, very faint bright and dark loops at the base of helmetstreamers, voids and radially oriented thin streamers. We compare our eclipseobservations with a hairy-ball model of the magnetic field, confirming thevalidity of the prediction, and we relate the eclipse phenomenology seen withthe near-simultaneous images from the Atmospheric Imaging Assembly on theNASA's Solar Dynamics Observatory (SDO/AIA), the Extreme Ultraviolet Imager onNASA's Solar Terrestrial Relations Observatory (STEREO/EUVI), ESA/ROB'sPROBA2/SWAP, and NRL's LASCO on ESA's SOHO. For example, the southeastern CMEis related to the solar flare whose origin we trace with a SWAP series ofimages.

Structure and Dynamics of the 13/14 November 2012 Eclipse White-Light Corona