Thesis (Ph.D.) - University of Birmingham, School of Physics and Space Research.
|Statement||by Simon John Jewell.|
We present evidence of global coronal wave rotation in EUV data from SOHO/EIT, STEREO/EUVI, and SDO/AIA. The sense of rotation is found to be consistent with the helicity of the source region (clockwise for positive helicity, anticlockwise for negative helicity), with the Extreme Ultraviolet Explorer Deep Survey observations of cool stars (spectral type F to M) have been used to investigate the distribution of coronal flare rates in energy and its relation to activity indicators and rotation parameters. Cumulative and differential flare rate distributions were constructed and fitted with different methods. Power laws are found to approximately describe the A/abstract. Observations at the Extreme Ultraviolet (EUV; Angstrom) of the ROSAT Wide Field Camera all-sky survey have shown that stars of spectral classes dF5 - dM6 possess bright and energetic coronae. Our stellar sample included 50 photospherically and chromospherically active stars main-sequence stars. All of them showed EUV "quiescent" emission and many exhibited :// The FIP Effect and Abundance Anomalies in Late-Type Stellar Coronae. J. J. Drake, J. M. Laming, K. G. Widing. Pages A Catalogue of Ultraviolet Observations of Chromospherically Active Binary Stars. C. La Dous, Alvaro Giménez. the Extreme Ultraviolet band of the spectrum (roughly defined as the decade in energy from Å
From the beginning of Space Astronomy, the Extreme Ultraviolet band of the spectrum (roughly defined as the decade in energy from Å) was deemed to be the `unobservable ultraviolet'. Pioneering results from an EUV telescope on the Apollo-Soyuz Mission in forcibly demonstrated › Astronomy › Astrophysics and Astroparticles. Radio and extreme-ultraviolet observations of CF Tucanae X-ray astronomy of stellar coronae (Review) The author presents radial velocities of 53 bright late-type stars with emission in the The study of the universe in Extreme Ultraviolet (EUV) wavelengths is a relatively new branch of astronomy. Lying between the X-ray and UV bands, Extreme Ultra-violet has proved to be a valuable wavelength for the study of speciﬁc groups of astronomical objects, including white dwarf stars and stellar coronae, as well as the interstellar EUVE Observations of the Seyfert Galaxy MRK C. -Y. Hwang, S. Bowyer, and M. Lampion 75 III. Coronae of Cool Stars EUVE Spectra of Coronae and Flares Carole Jordan 81 Cool Stars in the EUV: Spectral and Structural Variability Alexander Brown 89 The FIP Effect and Abundance Anomalies in Late-Type Stellar
Extremely irradiated, close-in planets to early-type stars might be prone to strong atmospheric escape. We review the literature showing that X-ray-to-optical measurements indicate that for intermediate-mass stars (IMSs) cooler than ≈K, the X-ray and extreme-ultraviolet (XUV) ﬂuxes are on average signiﬁcantly higher than those of physics, and partly with the closely related extreme ultraviolet range. Radio aspects of stellar coronae have been reviewed elsewhere (Güdel ) and will be occasionally addressed when they provide complementary information to our present subject., Typical resolutions for such observations are km s-' for STIS-EM, 15 km s-' for GHRS-GM, and 30 km s-' for FUSE. e period - the Extreme Ultraviolet Explorer (EUVE - Bowyer and Malina, ) satellite allowed access to the 80 - A spectral region for spectroscopic and photometric study of stellar coronal :// We report the detection of quiescent EUV emission from the very low mass dwarf VB 8 by the Extreme Ultraviolet Explorer (EUVE) in the Lexan/B band ( Å). of late type stellar coronas