Decoding of the light changes in eclipsing Wolf-Rayet binaries - I. A non-classical approach to the solution of light curves

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Volume 503 / No 3 (September I 2009)

A&A, 503 3 (2009) 963-972

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Table 1:

Values of the moments of the eclipses of HD 5980 used throughout this paper.
	Primary eclipse	Secondary eclipse
	Ingress	Ingress	Egress
B₂	$.00935 \pm .00026$	$.00832 \pm .00041$	$.00481 \pm .00024$
B₄	$.01801 \pm .00048$	$.01542 \pm .00065$	$.00922 \pm .00043$
B₆	$.02604 \pm .00067$	$.02164 \pm .00080$	$.01326 \pm .00059$
B₈	$.03351 \pm .00083$	$.02721 \pm .00088$	$.01699 \pm .00071$
B₁₀	$.04046 \pm .00097$	$.03226 \pm .00094$	$.02044 \pm .00082$

These values are derived from the light curve prior to the 1994 LBV event.

Source LaTeX | All tables | In the text

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