The 10th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun

Abstract

We have derived the abundance of iron relative to hydrogen in the corona of the active RS CVn binary HR 1099 (V711 Tau) using EUVE spectroscopic observations and additional X-ray constraints provided by ASCA observations. We have compared the results with simple two temperature optically thin plasma model fits to an ASCA spectrum of this star. Results from the two methods are in reasonable agreement. Existing photospheric studies also yield a similar Fe abundance of [Fe/H] ~ -0.4, suggesting at face value an absence of any coronal abundance anomaly in HR 1099 involving Fe. However, as with nearly all of the RS CVn's, existing photospheric abundances are perhaps questionable and demand further scrutiny.

PostScript File

drakej1.ps   (Color, 2085 kB)

Sections

1. Summary

2. Analysis and Results

3. Conclusions

Objects

• HR 1099

References

• Randich, S., Giampapa, M.S., & Pallavicini, R., 1994, A&A, 283, 893 (ADS)

Bibliographical Information

J.U. Drake and V. Kashyap 1998, in ASP Conf. Ser. 154, The Tenth Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, eds. R.A. Donahue & J.A. Bookbinder (San Francisco: ASP), 1014

ADS record for this paper