{"references": ["Augustson, K.C. et al. (2015), ApJ 809 149", "Bice, C.P. & Toomre, J. (2020), ApJ 893 107", "Brown, B.P. et al. (2010), ApJ 711 424", "Brown, B.P. et al. (2011), ApJ 731 69", "Brown, B.P. et al. (2020), ApJL 902 L3", "Browning, M.K. et al. (2008), ApJ 676 1262", "Carlsson, M. et al. (2016), A&A 585 A4", "Davenport, J.R.A. (2016), ApJ 829 23", "Fan, Y. & Fang, F. (2014), ApJ 789 13", "Featherstone, N.A. & Hindman, B.W. (2016), ApJ 818 32", "Guerrero, G. et al (2016), ApJL 828 L3", "Kowalski, A.F. et al. (2009), ApJ 138 633", "Kowalski, A.F. et al. (2010), ApJL 714 L98", "Krizhevsky, A. et al. (2017), Commun. ACM 60 84", "Martinez-Sykora, J. et al. (2012), ApJ 753 161", "Matilsky, L.I. & Toomre, J. (2020), ApJ 892 106", "Nelson, N.J. et al. (2011), ApJL 739 L38", "Nelson, N.J. et al. (2013), ApJ 762 73", "Nelson, N.J. et al. (2014), SoPh 289 441", "Rempel, M. (2012), ApJ 750 62", "Silverberg, S.M. et al. (2016), ApJ 829 129", "Strugarek, A. et al. (2018), ApJ 863 35", "Weber, M.A. & Browning, M.K. (2016), ApJ 827 95", "West, A.A. et al. (2008), ApJ 135 785", "West, A.A. et al. (2015), ApJ 812 3", "Xia, X. & Kulis, B. (2017), arxiv:1711.08506", "Yadav, R.K. et al. (2015), ApJL 813 L31", "Zinkevich, M. et al. (2010), NIPS 4 4"]}

The dynamical origins of the intense magnetic activity exhibited by most M-dwarf stars must be tied to their internal convective dynamos, and yet there remain many unanswered questions concerning its details. Despite the central role magnetic flux ropes are thought to play in the formation of solar and stellar starspots, global MHD simulations of stellar interiors have historically struggled to self-consistently capture their dynamics. By their nature, these structures tend to be short-lived or wholly absent in all but the most turbulent high-resolution simulations -- environments which make their hand-identification and study prohibitively time-consuming. We present here a novel machine-learning pipeline for the autonomous identification and analysis of self-consistent, rising flux ropes found in our global 3D MHD simulations of M-dwarf convective interiors. We report on the details of the models developed, as well as early results from the project and its prospects moving forward.