Table 2
Mid-eclipse ephemeris of the main accretion spot of UZ For and corresponding planet model parameters.
| Quadratic term | T0 = 2453405.300833(5) d | |
| Pbin = 0.087865421(1) d | Planet | |
| A = −14.5(2) × 10−14 | Parameters | |
| 1st elliptical term | υ3 = (E + T3)f3 | M3,fnc = 1.326(7)10−6 M⊙ |
| T3 = 67198(145) (binary cycle) | M3,Jup = 10.00(2) | |
| f3 = 0.0001030(1) (cycles per binary cycle) | P3 = 14.67(1) yr | |
| ϖ3 = 2.10(1) | a3 = 5.7(1) au | |
| Kbin,(3) = 0.000371(3) d | a1,3 = 0.064(1) au | |
| e3 = 0.69(1) | ||
| 2nd elliptical term | υ4 = (E + T4)f4 | M4,fnc = 3.43(9)10−8 M⊙ |
| T4 = 7444(219) (binary cycle) | M4,Jup = 3.22(5) | |
| f4 = 0.000260(1) (cycles per binary cycle) | P4 = 5.82(3) yr | |
| ϖ4 = −0.22(5) | a4 = 3.0(2) au | |
| Kbin,(4) = −0.000065(3) d | a1,4 = 0.011(1) au | |
| e4 = 0.45(6) |
Notes. The ephemeris are rounded off to the 1σ errors. The planet parameter errors are 1σ errors and were propagated from the one fitting solution and may underestimate true errors of range in parameter space of possible solutions. The minimum planet masses are listed assuming coplanearity and M3,4,fnc is the mass function. The combined mass of the primary and secondary stars is assumed to be 0.84 M⊙ (table reproduced from Potter et al. 2011).
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