Precise physical parameters of three late-type eclipsing binary giant stars in the Large Magellanic Cloud

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Volume 692 (December 2024)

A&A, 692 (2024) A110

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Table 7.

Orbital and photometric parameters from the adopted solution using the codes WD and JKTEBOP.

	LMC29293	LMC25304	LMC554
Orbital Period P (days) ^(a)	123.1689 ± 0.0038	194.4989 ± 0.0041	133.1725 ± 0.0009
T₀ (JD-2 450 000) ^(a)	6436.018 ± 0.012	7146.410 ± 0.030	6497.7498 ± 0.0039
Inclination i (deg) ^(a)	87.792 ± 0.051	89.775 (fixed)	88.816 ± 0.036
Semi-major axis (R_⊙) ^(b)	189.90 ± 0.68	263.68 ± 0.79	203.28 ± 0.41
Eccentricity e ^(b)	0 (fixed)	0.1074 ± 0.0010	0.004 ± 0.002
Longitud of periastron ω (deg) ^(b)	–	342.3 ± 1.6	88.3 ± 3.7
Systemic Velocity γ₁ (km s⁻¹) ^(b)	300.51 ± 0.17	280.46 ± 0.09	290.24 ± 0.06
γ₂ − γ₁ (km s⁻¹)	0.08	−0.44	−0.02
RV Semi-amplitude K₁ (km s⁻¹) ^(b)	40.62 ± 0.22	34.29 ± 0.14	38.72 ± 0.11
RV Semi-amplitude K₂ (km s⁻¹) ^(b)	37.33 ± 0.17	34.69 ± 0.13	38.49 ± 0.11
Mass Ratio q ^(b)	1.088 ± 0.008	0.988 ± 0.005	1.006 ± 0.004
Surface Potential Ω₁ ^(b)	10.860 ± 0.144	12.264 ± 0.121	11.783 ± 0.079
Surface Potential Ω₂ ^(b)	11.660 (fixed)	11.509 ± 0.135	11.410 (fixed)
Sum of Fractional Radii $\frac{R_{P} + R_{S}}{A}$ $\frac{R_P+R_S}{A}$ ^(a)	0.2041 ± 0.0018	0.1849 ± 0.0018	0.1896 ± 0.0016
Ratio of Radii $k = \frac{R_{S}}{R_{P}}$ $\mathbf{k}=\frac{R_S}{R_P}$ ^(a)	0.993 ± 0.025	1.062 ± 0.030	1.041 ± 0.021
Primary’s Temperature T₁ (K)	5170 (fixed)	5150 (fixed)	5450 (fixed)
Secondary’s Temperature T₂ (K) ^(b)	5215 ± 12	5053 ± 20	5421 ± 7
Light ratio ${(\frac{L_{S}}{L_{P}})}_{I}$ ${\left(\frac{L_S}{L_P}\right)}_{I}$ ^(b)	1.019 ± 0.048	1.048 ± 0.035	1.064 ± 0.032
${(\frac{L_{S}}{L_{P}})}_{V}$ $\left(\frac{L_S}{L_P}\right)_V$ ^(c)	1.033	1.018	1.055
Third light ℓ₃_I ^(b)	0 (fixed)	0 (fixed)	0 (fixed)
rms_RV1 (m s⁻¹)	548	349	353
rms_RV2 (m s⁻¹)	439	318	365
rms Ic (mmag)	9.0	13.7	6.6

Notes. Parameters marked as fixed were decided to be settled in order to avoid a degeneracy in model calculations.

^(a)

Calculated with WD code with uncertainties from the Monte Carlo algorithm with JKTEBOP.

^(b)

Uncertainties calculated with differential correction from WD code.

^(c)

Extrapolated value from WD solution.

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