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Low mass white dwarfs are the remnants of disrupted red giant stars in binarymillisecond pulsars and other exotic binary star systems. Some low mass whitedwarfs cool rapidly, while others stay bright for millions of years due tostable fusion in thick surface hydrogen layers. This dichotomy is not wellunderstood so their potential use as independent clocks to test the spin-downages of pulsars or as probes of the extreme environments in which low masswhite dwarfs form cannot be fully exploited. Here we present precise mass andradius measurements for the precursor to a low mass white dwarf. We find thatonly models in which this star has a thick hydrogen envelope can match thestrong constraints provided by our new observations. Very cool low mass whitedwarfs must therefore have lost their thick hydrogen envelopes by irradiationfrom pulsar companions or by episodes of unstable hydrogen fusion (shellflashes). We also find that this low mass white dwarf precursor is a new typeof pulsating star. The observed pulsation frequencies are sensitive to internalprocesses that determine whether this star will undergo shell flashes.

Multi-periodic pulsations of a stripped red giant star in an eclipsing binary