RXTE X-ray monitoring of the supermassive star eta carinae: Colliding wind emission in a pre-hypernova candidate binary?

Details RXTE X-ray monitoring of the supermassive star eta carinae: Colliding wind emission in a pre-hypernova candidate binary? RXTE X-ray monitoring of the supermassive star eta carinae: Colliding wind emission in a pre-hypernova candidate binary?

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aipc..522..431c&link_type=abstract

COSMIC EXPLOSIONS: Tenth Astrophysics Conference. AIP Conference Proceedings, Volume 522, pp. 431-434 (2000).

Astronomy and Astrophysics

Astrophysics

Emission-Line Stars, Late Stages Of Stellar Evolution, X-Ray

Scientific paper

ROSAT, ASCA, RXTE and now Chandra X-ray observations of the supermassive star η Carinae obtained over the past 7 years chronicle the inordinate variability of the high-energy emission. The most important characteristics are these: 1) the hard X-ray ``low state'' evidently recurs with a period consistent with the ``Damineli Cycle'' of 5.5 years; 2) the X-ray emission exhibits ``flares'' which occur quasi-periodically; 3) the overall X-ray brightness in the current ``cycle'' is brighter than at the same phase in the last cycle; 4) the hard, variable ``core'' source is apparently resolvable at lower energies but unresolvable at energies above ~4 keV. The X-ray data appear consistent with a model of X-ray generation via colliding winds in a massive binary system coupled with dust scattering, though the ``flaring'' activity probably requires that the wind from at least one of the stars is azimuthally structured. It is difficult to account for all the X-ray properties by activity in a single star. .

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