Inferring coronal structure using X-ray spectra: A Chandra study of AB Dor

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dc.creatorHussain, G. A. J.
dc.creatorBrickhouse, N. S.
dc.creatorDupree, A. K.
dc.creatorJardine, M.
dc.creatorvan Ballegooijen, A.
dc.creatorCameron, A. Collier
dc.creatorDonati, J. F.
dc.creatorFavata, F.
dc.date2004-10-07
dc.date.accessioned2026-07-07T02:14:57Z
dc.date.available2026-07-07T02:14:57Z
dc.descriptionThe Chandra X-ray observatory monitored the single cool star, AB Doradus, continuously for a period lasting 88ksec (1.98 Prot) in 2002 December with the LETG/HRC-S. The X-ray lightcurve shows significant rotational modulation. It can be represented as having a flat level of emission superimposed with bright flaring regions that appear at the same phases in both rotation cycles. Phase-binned OVIII line profiles show centroid shifts that also repeat in consecutive rotation cycles. These Doppler shifts trace a roughly sinusoidal pattern with a a semi-amplitude of 30 +/-10km/s. By taking both the lightcurve and spectral diagnostics into account along with constraints on the rotational broadening of line profiles (provided by archival Chandra HETG FeXVII line profiles) we can construct a simple model of the X-ray corona. The corona can be described as having two components, one component is homogeneously distributed, extending less than 1.75R*; and the other consists of at least two compact emitting regions near the stellar surface. These compact regions account for 16% of the X-ray emission and are likely to be located less than 0.4R* above the stellar surface.
dc.description4 pages, 4 figures. Submitted for publication in the Proceedings of the 13th Cool Stars, Stellar Systems and the Sun workshop, ESA-SP, Eds. Favata, F., et al., 2004 (in press)
dc.identifierhttps://arxiv.org/abs/astro-ph/0410213
dc.identifierhttp://arxiv.org/abs/astro-ph/0410213
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8337
dc.subjectAstrophysics
dc.titleInferring coronal structure using X-ray spectra: A Chandra study of AB Dor
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