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

Abstract

Both the 1866 and 1946 outbursts of the recurrent symbiotic nova T CrB have displayed a mysterious secondary maximum peaking in brightness ~5 months past the primary one. Common to all previous modeling attempts was the rejection of plain irradiation of the red giant (RG), on the basis that the secondary maximum of T CrB would have been out of phase with the transit at superior conjunction of the RG. Implicit to this line of reasoning is the assumption of a constant temperature for the white dwarf (WD) irradiating the red giant. I show by radiative modeling that irradiation of the RG by a cooling WD nicely reproduces the photometric evolution of the secondary maximum, both in terms of brightness and color, removes the phasing offset, and provides a straightforward explanation that will be easy to test at the next and imminent outburst.

arXiv commentcorrecting a label in Figure 1

References in corpus (6)

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Cited by in corpus (2)

• Modeling the high-brightness state of the recurrent nova T CrB as an enhanced mass-transfer event
• Pre-nova Observations of T CrB: A view from the CHARA Array