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Structure and Dynamics of the Inner Corona Measured from the DEB Initiative 2024 Eclipse Image Sequence

  • Authors: Matthew J Penn, Robert Baer, Chris Mandrell, Corinne Brevik, Castor Fu, Mike Conley, Richard Danley, Harvey Henson, David Iadevaia, Jonathan Mangin, Chris Midden, Brodye Miller, Claude Plymate, Teresa Plymate, Zack Stockbridge, Kevin Rasso, Autumn Awalt, Avery Awalt, Gracie Awalt, Josh Awalt, Lauree Rasso, Mike Chartrand, Noah Lambert, Zoee Rasso, Kevin Cobble, Amelia Menezes, Andrew Yu, Felix Mei, Hanson Du, Ramesh Pattar, Vishrut Kumaran, Robert Auburger, Brian J. Drake, Seth Antozzi, Chloe Rectanus, Grayson Garner, Michael Weiss, Bill Kloepping, Deborah Grubis, Maryanne Angliongto, Ashvik Chilakala, Carl Buz McCullough, Mark Bremer, Christina Adair, Amber Huffman, Charon Adair, Gabbie Graham, Nick Tillerson, Fred Isberner, Candy Isberner, Harry Treece, Lisa Sikorski, Sage Julian-Fralish, Heidi Schran, Addison Greene, Bibodh Baral, Crow Ely, Nolan Hodgson, Olive Blackmar Rice, Olivia Andrews, Olivia Freeman, Quinn Donnelly, Serenity Prince Kirk, Carmen Tran, Brianna Blanchard, Kyan West, Landon Bevier, Murali Saravanan, Jeremy Wright

Matthew J Penn et al 2026 The Astrophysical Journal Letters 1006 .

  • Provider: AAS Journals

Caption: Figure 3.

Ludendorff coronal flattening parameter for DEB sites. The DEB summed HDR images from all sites are used to compute the Ludendorff coronal flattening parameter as shown in the top panel. There is a high level of agreement among all the sites, and the Ludendorff index at 2.0 solar radii is computed to be 0.0761 ± 0.0007. The line segment clearly results in the wrong index value and represents the extrapolation method used by some authors, as discussed in the main text. We also fit ellipses to the intensity isophotes and show the ellipticity and solar position angle of the semimajor axis in the second and third panels. These two parameters behave more smoothly at low coronal heights, and a linear extrapolation from lower heights would provide accurate measures at 2.0 solar radii. We suggest that these parameters would better characterize the coronal structure.

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