Presentation on theme: "Tracing the wind structures in WR113 Alexandre David-Uraz (supervisor : Tony Moffat) Université de Montréal."— Presentation transcript:
Tracing the wind structures in WR113 Alexandre David-Uraz (supervisor : Tony Moffat) Université de Montréal
Outline Brief theoretical context Introduction to CV Ser Spectroscopy and orbit Lamontagne et al. fit MOST photometry Clumping and wind collision What’s next?
Brief theoretical context WR stars have a very high mass loss rate, typically M ~ 10 -5 M /year This rate cannot be explained by the star’s luminosity alone A better understanding of the clumping phenomenon is crucial in solving this problem
Introduction to CV Ser WR113 = CV Ser = HD168206, SB2 RA 18:19:07.36, DEC -11:37:59.2 (J2000) Galactic coordinates: l = 18.91º b = +1.75º Spectral types: WC8d + O8-9 IV v = 9.43, b-v = +0.46 P = 29.704 ± 0.002 d, e = 0 (?) Goal: use MOST to probe structures in the WR wind as its companion shines through it at different orbital positions
What’s next? Fourier analysis Fourier analysis in order to find pulsations in the star or its wind Wavelet analysisrandom variations Wavelet analysis in order to find random variations due to the clumping spectroscopic changes Linking these variations to spectroscopic changes the phase dependancy Establishing the phase dependancy of these variations Putting together a model of the clumping phenomenon Putting together a model of the clumping phenomenon new observation campaign A new observation campaign is scheduled for June/July 2010, both on the MOST space telescope and the spectrometer at OMM
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