The Spectroscopic and Visual Orbit of the Nitrogen-Rich Massive Binary WR 138
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Abstract
Wolf-Rayet (WR) stars are massive stars that have lost their exterior envelopes due to stellar winds, and possibly binary interactions, however, they have yet to be understood well enough to be placed on the H-R diagram in the context of stellar evolution. In order to fully understand them, there must be direct constraints, namely measurements of their masses and luminosity. WR 138 is a nitrogen-rich WR star, whose empirical values have not been precisely determined. Its companion O-star, has not been well constrained either, due to the brightness of the WR star and its inclination. By using spectroscopic observations, a more accurate period and radial velocity of WR 138 will be determined, along with a developed 3-dimensional orbital model. These key parts will allow us to determine the empirical relations of WR 138, to determine how the star evolved, and where it fits on the HR diagram.
The Spectroscopic and Visual Orbit of the Nitrogen-Rich Massive Binary WR 138
Wolf-Rayet (WR) stars are massive stars that have lost their exterior envelopes due to stellar winds, and possibly binary interactions, however, they have yet to be understood well enough to be placed on the H-R diagram in the context of stellar evolution. In order to fully understand them, there must be direct constraints, namely measurements of their masses and luminosity. WR 138 is a nitrogen-rich WR star, whose empirical values have not been precisely determined. Its companion O-star, has not been well constrained either, due to the brightness of the WR star and its inclination. By using spectroscopic observations, a more accurate period and radial velocity of WR 138 will be determined, along with a developed 3-dimensional orbital model. These key parts will allow us to determine the empirical relations of WR 138, to determine how the star evolved, and where it fits on the HR diagram.