THE ROTATION EFFECTS TO THE EVOLUTION OF THE B-EMISSION STARS: CASE STUDY HR 8520, HR 8402, AND HR 5941

• Main Author: RATNA WULANDARI - Nim: 10314014 , TRI
• Format: Final Project
• Language: Indonesia
• Online Access: https://digilib.itb.ac.id/gdl/view/31372
• Institution: Institut Teknologi Bandung

<p align="justify">B-emission (Be) stars are B-type stars, which rotate with high velocities (100-300 km/s or more), whose spectra show, or have shown, emission lines at Hydrogen Balmer (e.g. H&#945; and H&#946;), and sometimes at neutral Helium and ionized metals. Observations show that, within a certain period, these lines experience phase changes, from Be (single peak, double peak, and Be-shell) to B-normal profiles or vice versa. These emission lines are formed in the envelope surrounding the stars. There is an estimate that this formation is affected by the evolution of the stars. Stellar evolution describes the lives of the stars, from the beginning to the end of their lives, usually presented in the Hertzsprung-Russel diagram (H-R diagram). In this final project, we study the effects of rotation velocity to the evolution of intermediate Be-stars. The stars are HR 8520, HR 8402, and HR 5941. They are single stars, having different masses, rotation velocities, and spectrum profiles. For modelling the evolution, we use MESA-Web (Modules for Experiments in Stellar Astrophysics), a web-based interface of the stellar evolution code. Models show that the evolution of studied stars are affected by rotation. <p align="justify"> <br />