X-ray coronae and stellar magnetospheres

摘要

Chandra's spectroscopic resolving power allows us to measure velocity shifts down to ～30 km/s in line profiles. Observations covering >2 Prot are needed to disentangle flaring and quiescent coronal emission. The rotational modulation in X-ray lightcurves and spectra enable us to estimate the size and location of non-flaring X-ray emitting regions stellar coronae. We probe the coronal structure in systems covering a range of parameters (e.g., spectral type and rotation rate), and summarise results from new studies.