Activity in Red-Dwarf Stars: Proceedings of the 71st by M. Rodonò (auth.), Patrick B. Byrne, Marcello Rodonò (eds.)

By M. Rodonò (auth.), Patrick B. Byrne, Marcello Rodonò (eds.)

IAU Colloquium No. seventy one had its rapid origins in a small collecting of individuals . within the optical and UV examine of flare stars which happened throughout the 1979 Montreal common meeting. We well-known primary swap used to be happening within the research of those gadgets. Space-borne tools (especially lUE and Einstein) and a brand new genera­ tion of ground-based apparatus have been having a profound impression at the diversity of investigations it used to be attainable to make. To extract greatest make the most of those new chances it'd be precious as by no means sooner than to have sturdy verbal exchange with colleagues in different disciplines, for instance,. with atomic and sun physicists. equally, reports of phenomena linked to the outer atmospheres of the late-type stars may well now desire to offer major insights into yes features of sun task. So, in view of the wide variety of backgrounds of these partaking, the assembly had an strangely excessive percentage of invited reports whereas many of the contributed papers have been offered as posters. it really is enjoyable that during the quick time because the assembly a great deal of correspondence has been bought from members remarking at the luck of this structure. as soon as the choice have been taken in precept to carry the assembly, a truly enormous volume of labor fell at the organizing committees, viz. the medical and native Organizing Committees. The clinical Organizing Committee was once chaired by way of D.J. Mullan and consisted of A.D.

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Additional resources for Activity in Red-Dwarf Stars: Proceedings of the 71st Colloquium of the International Astronomical Union Held in Catania, Italy, August 10–13, 1982

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CO and CaOH show strong non-linear effects (Fig . 3). The ternperature dependences are valid f or all population t ypes arnong dM stars and f1are stars, so the effects of rnetallicity on the ternperature re l ations rnust be srnall. 4 H20 03 02 .. o. 0 c) 0 . 3500 .. __ 3000 4000 3500 3000 r~ :,;:. I CaH ? ~ .. ",. . . ·--~~--1 Telt OS . 0 3500 3000 Telf Fig. 2. Empirical r el a t ionshi ps between eff ec tive ternperature and the strengths of rnol ecul ar feat ures in red dwarf s tars. The photornetri c data used as ordinates are frorn a)Persson et al.

Ahler et al. 1981; Baliunas et al. 1983; Marcy 1983). Third, detailed modeling of stellar chromospheric, traosition region, and coronal emission based on simple extensioos of solar •loop models seem to give a fairly good aecount of the observations {cf. articles by Dupree, Giampapa, Goluh, aod Linsky in these Proceedings, and by Linsky 1983 aod Vaiaoa 1983). Fourth, the range of variability in stellar activity-related emission - ranging from short, flare-like traosients to rotational modulation and long·term, eycle-like variations - eomport with expectations based on solar Observations (cf.

2. Rotation from a cross-correlation technique A method has been developed by Benz and Mayor (1981) which utilize a crosscorrelation analysis between the spectrum of the star and a reference mask in the spectrograph. This observing technique has long been known as a very efficient way of obtaining accurate radial velocities (Griffin 1967). The position of the correlation dip yields the radial velocity of the star, and the width of the dip reflects the width of the absorption lines in the spectrum.

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