Attitudes of Secondary Students Toward Online and Face-to-Face Learning in Mathematics: A Quantitative Causal-Comparative Study

The purpose of this quantitative, causal-comparative study is to investigate the current differences between online and face-to-face student attitudes toward mathematics and computer-based learning at the high school level. Because instruction and technology use have been influenced by the Covid-19 pandemic, it is important to assess student attitudes toward mathematics and computer-based learning in both traditional face-to-face and online settings. This study was conducted with 70 face-to-face students and 67 online high school students in a single school district in North Carolina. The Galbraith-Haines Mathematics-Computer Attitude Scales were used as the data collection instrument measuring student confidence toward mathematics, mathematics motivation, computer confidence, and computer-mathematics interaction. A secure Google form was used for data collection in the spring of 2023. A one-way MANOVA was used to determine if there was a difference in attitudes between the online and face-to-face participants in the dependent variables. The result of the MANOVA was significant, where F(4, 127) = 10.448, p \u3c .001, Pillai’s Trace = .248, and partial η^2 = 0.248, suggesting there are significant differences on the dependent variables by setting type for high school mathematics students in online and face-to-face settings. Results indicated a higher confidence in mathematics held by face-to-face students, higher mathematics motivation held by online students, and higher computer-mathematics interaction held by online students. No significant difference was found between online and face-to-face students in the area of computer confidence. Recommendations for further studies include a larger sample size, a comparison of technology uses, and a qualitative study

Generalized Warped Disk Equations

The manner in which warps in accretion disks evolve depends on the magnitude of the viscosity. ... See full text for complete abstract

Mass loss and supernova progenitors

We first discuss the mass range of type IIP SN progenitors and how the upper and lower limits impose interesting constraints on stellar evolution. Then we discuss the possible implications of two SNe, 2002ap and 2006jc, for Wolf-Rayet star mass-loss rates and long Gamma-ray bursts.Comment: 7 pages, 3 figures, to appear in the Conference Proceedings of "Unsolved Problems in Stellar Astrophysics

The coupling between pulsation and mass loss in massive stars

To what extent can pulsational instabilities resolve the mass-loss problem of massive stars? How important is pulsation in structuring and modulating the winds of these stars? What role does pulsation play in redistributing angular momentum in massive stars? Although I cannot offer answers to these questions, I hope at the very least to explain how they come to be asked.Comment: 12 pages, 1 figure, to appear in proceedings of "Unsolved Problems in Stellar Physics" conference (Cambridge, UK, July 2007

A Search for Pulsation in Very Low-mass Stars and Brown Dwarfs

Brown dwarfs and very low-mass stars constitute a crucial link between the intertwined processes of star formation and planet formation. To date, however, observational methods to uncover their formation mechanism or determine important properties such as mass and age have been lacking. Pulsation powered by deuterium burning in brown dwarfs and very low-mass stars is a newly suggested phenomenon that offers unprecedented opportunities to probe the interiors and evolution of these objects. We report on a photometric campaign to search for low-amplitude pulsations among young star-cluster members using a number of telescopes

Forecasting Seismic Signatures of Stellar Magnetic Activity

For the Sun, a tight correlation between various activity measures and oscillation frequencies is well documented. For other stars, we have abundant data on magnetic activity and its changes but not yet on its seismic signature. A prediction of the activity induced frequency changes in stars based on scaling the solar relations is presented. This seismic signature of the activity should be measurable in the data expected within few years.Comment: 8 pages, 3 figures, to appear in proceedings of "Unsolved Problems in Stellar Physics" conference (Cambridge, UK, July 2007