Spectroscopic searches for evolutionary orbital period changes in WR+OB binaries: the case of WR 141

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Abstract

The results of new low-resolution spectroscopic observations of the short-period system WR 141 (WN5o+O5V–III, P ≈ 21.7d) are presented, as well as the results of their comparison with the material of previous studies in order to search for an evolutionary change in the orbital period. A secular increase in the orbital period of WR 141 with a rate of Р˙=1.6±0.9 sec/year, corresponding to a mass loss rate of M˙WR=(3.1±1.9)×10-5М⊙/yr with the masses of the stars in the system of MWR=39±10Mʘ and MO=37±10Mʘ, is reported. A correlation between the mass loss rate of WR stars and their mass is discussed.

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About the authors

I. A. Shaposhnikov

Lomonosov Moscow State University, Sternberg Astronomical Institute; Lomonosov Moscow State University

Author for correspondence.
Email: iv.shaposhnikov@gmail.com

Faculty of Physics

Russian Federation, Moscow; Moscow

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Supplementary files

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2. Fig. 1. Radial velocity curves of WR 141. Top: all measurements presented in Tables 1 and 2; bottom: curves reduced by the mean velocity along the 4603 and 4945 Å lines of the N V ion, used for comparison with archival data in order to search for a period change.

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3. Fig. 2. Averaged spectrum of WR 141.

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4. Fig. 3. Graphs for the WR 141 system, constructed from the radial velocity curves in the N V 4603 and 4945 Å lines. At the top is a construction with elements from [8], at the bottom is one with refined elements.

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5. Fig. 4. Relationship between the mass loss rate and the mass for WR stars. Blue dots are data from our work (see the summary in Table 5), orange dots are polarimetric data from [16], green dots are estimates based on measurements of IR radio fluxes [17], red dots are estimates based on modeling of spectral profiles [18].

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