  A new interpretation for the second peak of T Coronae Borealis (T CrB)
outbursts is proposed based on a thermonuclear runaway (TNR) model. The system
consists of a very massive white dwarf (WD) with a tilting accretion disk and a
lobe-filling red-giant. The first peak of the visual light curve of T CrB
outbursts is well reproduced by the TNR model on a WD close to the
Chandrasekhar mass ($M_{\rm WD} \gtrsim 1.35 ~M_\odot$), while the second peak
is reproduced by the combination of the irradiated M-giant and the irradiated
tilting disk. The derived fitting parameters are the WD mass $M_{\rm WD} \sim
1.35 ~M_\odot$, the M-giant companion mass $M_{\rm RG} \sim 0.7 M_\odot$
($0.6-1.0 M_\odot$ is acceptable), the inclination angle of the orbit $i \sim
70 \arcdeg$, and the tilting angle of the disk $i_{\rm prec} \sim 35 \arcdeg$.
These parameters are consistent with the recently derived binary parameters of
T CrB.
