Computer Education and Instructional Technology

This study was conducted in order to examine the process that the teachers designed the website. For this purpose, www.weebly.com, which is used as a web site building tool, was selected and teachers were given tasks for web designing. In this process, eye and mouse movements of teachers were recorded and analyzed via eye tracking devices.

In this study, it was aimed to investigate the change blindness that may occur in multimedia learning environments used cueing and signaling effects. For this purpose, a multimedia animation which had some changes about computer parts was designed. Twenty-one undergraduate students participated in the experiment voluntarily. Eye and mouse movements were recorded and analysed with eye-tracking method, and participants were asked to say when they noticed the changes; their voices were simultaneously recorded. The results show that the participants were more focused on the objects being signaled, and less detected the changes in other areas. It is seen that the percentage of detecting the change occurring on the most focused object is low, except for the object using the signaling and visual cueing. The change in the object that was used the signaling and the visual cueing is the most detected change.

This series of high quality elemental abundance analyses of mostly Main Sequence normal and peculiar B, A, and F stars defines their properties and provides data for the comparison with analyses of somewhat similar stars and with theoretical predictions. Most use high dispersion and high S/N (≥ 200) spectrograms obtained with CCD detectors at the long camera of the 1.22-m Dominion Astrophysical Observatory telescope's coudé spectrograph. Here we expand the range of stars examined to include two relatively quiescent F supergiants. ν Her (F2 II) and 41 Cyg (F5 Ib-II) are analyzed as consistently as possible with previous studies. These LTE fine analyses use the ATLAS9 and the WIDTH9 programs of R. L. Kurucz. High signal-to-noise spectrograms and high quality atomic data were employed. The derived values of these photometrically constant stars are somewhat different with the abundances of ν Her being somewhat metal-poor and those of 41 Cyg being crudely solar-like. Our analyses indicate that the basic results of Luck & Wepfer (1995) who also studied ν Her and 41 Cyg are not likely to be significantly changed by new studies of all their stars.

This series of high quality elemental abundance analyses of mostly Main Sequence normal and peculiar B, A, and F stars defines their properties and provides data for the comparison with analyses of somewhat similar stars and with theoretical predictions. Most use high dispersion and high S/N (≥ 200) spectrograms obtained with CCD detectors at the long camera of the 1.22-m Dominion Astrophysical Observatory telescope's coudé spectrograph. Here we expand the range of stars examined to include two relatively quiescent F supergiants. ν Her (F2 II) and 41 Cyg (F5 Ib-II) are analyzed as consistently as possible with previous studies. These LTE fine analyses use the ATLAS9 and the WIDTH9 programs of R. L. Kurucz. High signal-to-noise spectrograms and high quality atomic data were employed. The derived values of these photometrically constant stars are somewhat different with the abundances of ν Her being somewhat metal-poor and those of 41 Cyg being crudely solar-like. Our analyses indicate that the basic results of Luck & Wepfer (1995) who also studied ν Her and 41 Cyg are not likely to be significantly changed by new studies of all their stars.

We present samples from a spectroscopic atlas of the sharp-lined, magnetic Chemically Peculiar star HR 8216 (A6pCr) based on spectrograms obtained with the long camera of the 1.22-m telescope of the Dominion Astrophysical Observatory using a Reticon detector. For the spectral region λλ3830-4770 the inverse dispersion is 2.4Åmm −1 with a 2 pixel resolution of 0.072Å. At the continuum the mean signal-to-noise ratio is 200. The wavelengths in the laboratory frame, the equivalent widths, and the identifications of the various spectral features are given. This atlas should provide useful guidance for studies of similar stars and for atomic physicists interested in improving atomic line parameters.