X-ray and extreme-ultraviolet emission from the coronae of Capella |
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| Authors: | KJH Phillips M Mathioudakis DP Huenemoerder DR Williams ME Phillips FP Keenan |
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| Institution: | 1Space Science &Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon. OX11 0QX;2Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, BT7 1NN, Northern Ireland;3Massachusetts Institute of Technology, Center for Space Research, 70 Vassar Street, Cambridge, MA 02139, USA;4Department of Pure and Applied Physics, The Queen's University of Belfast, Belfast, BT7 1NN, Northern Ireland |
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| Abstract: | The primary objective of this work is the analysis and interpretation of coronal observations of Capella obtained in 1999 September with the High Energy Transmission Grating Spectrometer on the Chandra X-ray Observatory and the Extreme Ultraviolet Explorer ( EUVE ). He-like lines of O (O vii ) are used to derive a density of 1.7×1010 cm−3 for the coronae of the binary, consistent with the upper limits derived from Fe xxi , Ne ix and Mg xi line ratios. Previous estimates of the electron density based on Fe xxi should be considered as upper limits. We construct emission measure distributions and compare the theoretical and observed spectra to conclude that the coronal material has a temperature distribution that peaks around 4–6 MK , implying that the coronae of Capella were significantly cooler than in the previous years. In addition, we present an extended line list with over 100 features in the 5–24 Å wavelength range, and find that the X-ray spectrum is very similar to that of a solar flare observed with SMM . The observed to theoretical Fe xvii 15.012-Å line intensity reveals that opacity has no significant effect on the line flux. We derive an upper limit to the optical depth, which we combine with the electron density to derive an upper limit of 3000 km for the size of the Fe xvii emitting region. In the same context, we use the Si iv transition region lines of Capella from HST /Goddard High-Resolution Spectrometer observations to show that opacity can be significant at T =105 K , and derive a path-length of ≈75 km for the transition region. Both the coronal and transition region observations are consistent with very small emitting regions, which could be explained by small loops over the stellar surfaces. |
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| Keywords: | Sun: flares Sun: X-rays gamma-rays stars: activity stars: coronae stars: individual: Capella X-rays: stars |
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