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Table 8

Orbital solutions for the HD 201433 triple system.

Constant period Variable period

Short-period (SP) orbit

TSP (d) 2 457 613.15±0.08 2 457 613.14±0.15
PSP (d) 3.3131662±0.0000004 3.3131574±0.0000028
(yr-1) 3.2±1.0e-8
ωSP (rad) 2.38±0.16 2.36±0.29
e SP 0.015±0.003 0.015±0.005
KSP (km s-1) 20.09±0.04 20.07±0.08
f(m) (M) 0.00278±0.00002 0.00277±0.00003
aSP,1sin(i) (R) 1.316±0.003 1.314±0.005

Long-period (LP) orbit

TLP (d) 2 457 592.7±0.5 2 457 593.8±0.7
PLP (d) 154.119±0.008 154.151±0.005
ωLP (rad) 0.27±0.05 0.11±0.04
eLP (1) 0.377±0.026 0.499±0.015
KLP (km s-1) 8.51±0.10 8.52±0.17
f(m) (M) 0.0078±0.0003 0.0065±0.0005
aLP,1sin(i) (R) 25.9±0.3 25.9±0.5

γ (km s-1) 25.78±0.11 26.05±0.23
rms (km s-1) 4.68(2.83) 4.67(2.82)
Probability 0.002 0.998

Notes. Given are the systemic velocity (γ), the epoch of periastron (T), the orbital period (P), the period change rate (1 /P·dP/ dt), the longitude of the periastron (ω), the orbital eccentricity (e), the radial velocity semi amplitude (K) of the visible component, the mass function (f(m)), and the projected semi-major axis (asin(i)). For the variable-period fit PSP is defined for TSP and rms corresponds to the standard deviation of the residuals with the bracketed value computed for the 2016 measurements. The probability is calculated from the Bayesian model evidence (z) according to p = zn/ ∑ z.

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