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Both the 1866 and 1946 outbursts of the recurrent symbiotic nova T CrB havedisplayed a mysterious secondary maximum peaking in brightness ~5 months pastthe primary one. Common to all previous modeling attempts was the rejection ofplain irradiation of the red giant (RG), on the basis that the secondarymaximum of T CrB would have been out of phase with the transit at superiorconjunction of the RG. Implicit to this line of reasoning is the assumption ofa constant temperature for the white dwarf (WD) irradiating the red giant. Ishow by radiative modeling that irradiation of the RG by a cooling WD nicelyreproduces the photometric evolution of the secondary maximum, both in terms ofbrightness and color, removes the phasing offset, and provides astraightforward explanation that will be easy to test at the next and imminentoutburst.

The secondary maximum of T CrB caused by irradiation of the red giant by a cooling white dwarf