M. Hernanz

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About

M. Hernanz is a leading astrophysicist whose research centers on the explosive end states of stellar evolution, particularly classical novae and their role as potential progenitors of Type Ia supernovae. Her major contributions include pioneering studies of supersoft X-ray source (SSS) states in novae, which provide critical insights into white dwarf masses and accretion processes. Hernanz's work on M31N 2007-11a, a classical nova in the Andromeda galaxy, revealed an exceptionally short SSS duration—under 100 days—indicating a massive white dwarf nearing the Chandrasekhar limit. This finding, detailed in her 2009 paper (6 citations), has profound implications for understanding supernova progenitors. Through dedicated optical and X-ray monitoring programs of novae in M31's bulge, she has helped establish observational constraints on nova outburst physics and white dwarf growth. Her research bridges observational astronomy and theoretical modeling, making her a key figure in the study of thermonuclear runaways on white dwarfs. Hernanz's work continues to shape our understanding of how classical novae may evolve into the supernovae that serve as standard candles for measuring cosmic distances.