Poster Open Access

Understanding stars close to the gap

Wei-Chun Jao; Todd Henry; Elliott Horch; Eliot Vrijmoet; Gemini Speckle Team

Theoretical models show the main sequence gap is a result of the mixing of 3He during the merger of envelope and core convection zones. Unlike stars the either side of the gap, stars in a narrow mass range will go through instability phases, where their dynamos could switch between the αΩ dynamo like the Sun and Ω2 dynamo like late M dwarfs. At the same time, they show radial pulsation and their fluxes fluctuate, which resemble the pulsations observed in evolved stars like red giants and asymptotic giant branch stars. Consequently, they are a unique type of dwarf like no other on the main sequence. In this work, we would like to know 1) will the unstable interior structures result in observable characteristics such as flaring and spots, and 2) what is the mass range for these stars observationally? Here we present our preliminary results: 1) stars in the gap have higher percentage rate of activities than their adjacent regions, and 2) high resolution speckle results yield promising close binaries to  yield dynamical masses in the future.

Files (1.9 MB)
Name Size
poster.pdf
md5:58f2f96b31de5759e3c4d2f9243c354e
1.9 MB Download
91
91
views
downloads
All versions This version
Views 9191
Downloads 9191
Data volume 172.5 MB172.5 MB
Unique views 7171
Unique downloads 8383

Share

Cite as