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Table 4

Orbital solution of HD 17505Aa computed from our RV data, assuming an eccentric orbit and a period of 8.5690 days, compared to the orbital solution proposed by Hillwig et al. (2006) and an orbital solution obtained by combining our RVs with those measured by these authors.

This study Hillwig et al. (2006) Combined solution

Prim. (Aa1) Seco. (Aa2) Prim. (Aa1) Seco. (Aa2) Prim. (Aa1) Seco. (Aa2)
Porb (days) 8.5690  ± 0.0022 8.5710  ± 0.0008 8.5690  ± 0.0014
T0 (HJD − 2 450 000) 3329.656 ± 0.313 1862.696 ± 0.016 3328.910 ± 0.173
e 0.128± 0.037 0.095± 0.011 0.118± 0.018
γ (km s−1) − 27.8  ± 4.7 − 27.6  ± 4.5 − 25.8  ± 1.8 − 26.3  ± 1.2 − 27.7  ± 2.3 − 25.9  ± 2.3
K (km s−1) 156.7  ± 6.3 146.7  ± 5.9 166.5  ± 1.8 170.8  ± 1.8 162.8  ± 3.2 160.8  ± 3.1
a sini (R) 26.3  ± 1.0 24.6  ± 1.0 56.8  ± 0.4 27.4  ± 0.5 27.0  ± 0.5
q = m1m2 0.94  ± 0.05 1.03  ± 0.02 0.99  ± 0.02
257.4  ± 14.0 252  ± 6 271.5  ± 7.5
m sin3i (M) 11.7  ± 1.2 12.5  ± 1.3 17.1  ± 0.6 16.6  ± 0.6 14.6  ± 0.7 14.8  ± 0.8
RRL∕(a1 + a2) 0.37  ± 0.01 0.38  ± 0.01 0.38  ± 0.01 0.38  ± 0.01
RRL sini 19.0  ± 0.6 19.6  ± 0.6 20.6  ± 0.3 20.7  ± 0.3
σfit (km s−1) 3.18 1.86

Notes. T0 refers to the time of periastron. The values γ, K, and a sin i denote the apparent systemic velocity, the semi-amplitude of the RV curve, and the projected separation between thecentre of the star and the centre of mass of the binary system, respectively. The value ω is the longitude of periastron measured from the ascending node of the orbit of the primary. The value RRL stands for the radius of a sphere with a volume equal to that of the Roche lobe computed according to the formula of Eggleton (1983). All error bars indicate 1σ uncertainties.

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