Modeling Eclipses of the Novalike Variable TT Triangulum

Multicolor (BVRI) light curves of the eclipsing novalike variable TT Tri are presented and analyzed with a parameter-fitting eclipse model. The mass ratio of TT Tri is poorly constrained, but must lie roughly in the range 0.3<q(=M_2/M_1)<0.9. Models characterized by mass ratios of q=0.3 (i=76.1 deg), q=0.6 (i=72.6 deg), and q=0.9 (i=70.4 deg) were all capable of providing acceptable fits to the data, although the best fits were achieved for mass ratios near the upper end of the permitted range. The values of the remaining fitting parameters were found to be insensitive to the adopted mass ratio and rim thickness. The accretion disk was found to extend to ~50-60% of the distance to the inner Lagrangian point in all models, but came closer to reaching the tidal limit in the higher mass ratio models. The same behavior was found for the radial temperature profile of the disk, which increased with mass ratio, becoming more consistent with that expected for steady state accretion in the q=0.6 and q=0.9 models. Models with a truncated inner disk (R_in>>R_1) generally resulted in a higher white dwarf temperature, and a steepening of the disk temperature profile, but were not required to achieve a viable steady-state disk solution. No evidence was found for a luminous bright spot in the system, which is not surprising given the lack of a pre-eclipse "hump" in the light curve. A total of 22 eclipse timings were measured for the system, which yielded an ephemeris for the times of mid-eclipse given by HJD = 2,453,618.953(3) + 0.1396369(4) E. A comparison of the observed brightness and color at mid-eclipse with the photometric properties of the best-fitting model suggests that TT Tri lies at a distance of ~400-500 pc. (abstract abridged)