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Table 3

Parameters determined previously (left) and our results (right) for the system TU UMa.

Study Saha & White (1990a) Kiss et al. (1995) Wade et al. (1999) C Model 1 Model 2

Ppuls(M0) [d] 0.5576581097 0.5576581097 0.55765817(29)D 0.557657598 0.557657477
M0 [HJD] 2 425 760.4364 2 425 760.4364 2 425 760.464(5)D 2 442 831.4869 2 442 831.4864
puls × −31.48 −10.4(7)
10-11[d d-1]
a3 = 1/2 Ppulspuls × −8.78 −2.9(2)
10-11[d cycle-1]
β = puls [ms yr-1] × −9.934 −3.3(2)
β = puls [d Myr-1] × −0.11498 −0.038(3)
Porbit [yr] 20.19 24.1(3) 23.27(24) 23.30 23.27
T0 [HJD] 2 425 000 2 447 200(50) 2 421 585(207) 2 447 092 2 447 124
e 0.970 0.90(5) 0.74(10) 0.663 0.686
ω [°] 196.1 178(3) 183(5) 181.3 184.1
A [light day] 0.056 0.023(5) 0.0203(35) 0.0168 0.0172
a1sini [au] 10 4.0(7) 3.52(61) 2.91 2.99
f(M) [M] 0.11(1) 0.080 0.046 0.049
M2,min [M] 0.17 0.327 0.339
K1 [km s-1] 60.7 11.4(5) 6.6 4.97 5.25
1.05(9) 1.03(10)
N max ~ 43 ~ 42 67 253 220

Notes. The mass limit of the second body was estimated from the mass function f(M), the orbit inclination (i = 90°), and the mass of the RR Lyrae star M1 = 0.55M adopted from Fernley (1993) and Skarka (2014). Our parameters (right part of the table) were calculated from all maxima timings for model 1 and only from photoelectric, CCD, and DSLR measurements for model 2.

(*)

Parameter calculated using values from the original study;

(C)

their approach C was selected;

(D)

pulsation elements are known only from their approach D.

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