CHANDRA-LETGS X-ray observations of Capella. Temperature, density and abundance diagnostics

Details CHANDRA-LETGS X-ray observations of Capella. Temperature, density and abundance diagnostics CHANDRA-LETGS X-ray observations of Capella. Temperature, density and abundance diagnostics

Mar 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...368..888m&link_type=abstract

Astronomy and Astrophysics, v.368, p.888-900 (2001)

Astronomy and Astrophysics

Astrophysics

55

Stars: Individual: Capella, Stars: Coronae, Stars: Late-Type, Stars: Activity, X-Rays: Stars, Atomic Processes

Scientific paper

We report an analysis of the X-ray spectrum of Capella from 6 to 175 Å obtained with the Low Energy Transmission Grating Spectrometer (LETGS) on board of the X-ray space observatory CHANDRA. Many emission line features appear that can be resolved much better as compared to former instruments (EUVE and ASCA). Coronal electron densities (ne) and temperatures (T) of brightly emitting regions are constrained by an analysis of ratios of density- and temperature-sensitive lines of helium-like ions and highly ionized iron atoms. Lines emitted by e.g., O VII & VIII, Mg X-XII, Si XII-XIV, Fe IX, X & XV-XXIII are used to derive T. Line ratios in the helium-like triplets of C V, N VI, O VII, Mg XI, and Si XIII yield T in the range 0.5-10 MK, and ne in the range 109-1013 cm-3. The Fe IX/X ratio yields T =~ 0.9 MK, while lines from Fe XVIII to XXII give T ~ 6-10 MK. Flux ratios of Fe XX-XXII lines indicate for the electron densities an upper limit in the range ne <~ (2-5) 1012 cm-3. From line ratios of Fe XVII and Fe XVIII we derive constraints on the optical depth tau of ~ 1-1.5. An emission measure distribution is derived from Fe line intensities. Results for element abundances (relative to Fe) from a 4-T model are: O and Ne/Fe about solar, N, Mg and Si/Fe ~ 2x solar. The results for T and ne are described in terms of quasi-static coronal loop models and it is shown that the X-ray emission originates from compact structures much smaller than the stellar radii.

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