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

C. Perrier; J. Breysacher; G. Rauw

doi:10.1051/0004-6361/200911707

Home

All issues

Volume 503 / No 3 (September I 2009)

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

Full HTML

Free Access

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

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.