The accretion of hydrogen onto a white dwarf star ignites a thermonuclear runaway in the accumulated envelope, leading to luminosities up to 1 million times that of the Sun and a high velocity mass ejection that produces a remnant shella classical nova eruption 1,2 . Close to the upper mass limit of a white dwarf 3 (1.4 Msun), rapid accretion of hydrogen (~10 -7 Msun/yr) from a binary star companion leads to frequent eruptions on timescales of years 4,5 to decades 6 . Such systems are known as recurrent novae. The ejecta of recurrent novae, initially moving at up to 10,000 km/s (7) , must sweep-up the surrounding interstellar medium and evacuate cavities around the nova binary. No remnant larger than one parsec from any single classical or recurrent nova eruption is known 8,9,10 , but thousands of successive recurrent nova eruptions should be capable of generating shells ~100-1,000 times this size.Here we report that the most rapidly recurring nova, M31N 2008-12a, which erupts annually 11 , is surrounded by such a nova super-remnant with a projected size of at least 134
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