X-ray emission and variability of eta Carinae

Details X-ray emission and variability of eta Carinae X-ray emission and variability of eta Carinae

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aspc..233...75c&link_type=abstract

P Cygni 2000: 400 Years of Progress, ASP Conference Proceeding Vol. 233, Edited by M. de Groot and C. Sterken, San Francisco: As

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Scientific paper

We review the X-ray properties of the supermassive LBV eta Carinae, and briefly compare the X-ray observations of eta Carinae with P Cygni, another "canonical'' LBV. In the rest of this paper we try to fit theRXTE light curve with a colliding-wind emission model to refine the ground-based orbital elements. Our X-ray light curve modelling suggests that the mass-loss rate from eta Carinae is generally less than 3x10-4 Mo/yr, about a factor of 5 lower than that derived from some observations in other wavebands. We could not match the duration of the X-ray minimum with any colliding-wind model in which the wind is spherically symmetric and the mass-loss rate is constant. However, we show that we can match the variations around X-ray minimum if we include an increase of a factor of ~ 20 in the mass-loss rate from eta Carinae for approximately 80 days following periastron. Based on the X-ray fluxes, the distance to eta Carinae is 2300 pc with formal uncertainties of only ~10%.

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