SUMMARY
Stars are classified using the letters O, B, A, F, G, K, and M based on the intensity of their hydrogen Balmer lines and effective temperatures. This classification system originated in the late 1800s with Professor Draper at Harvard Observatory and was later refined by Annie Cannon. The letters represent a spectrum from hottest (O) to coolest (M), with the classification evolving to reflect the physical properties of stellar atmospheres rather than just spectral line visibility. Additional classes such as R, N, S, T, L, and C have been introduced, but the primary classification remains focused on the original letters.
PREREQUISITES
- Understanding of stellar spectra and hydrogen Balmer lines
- Familiarity with effective temperature concepts in astrophysics
- Knowledge of the historical context of astronomical classification systems
- Basic comprehension of spectral classification and its evolution
NEXT STEPS
- Research the historical development of stellar classification systems
- Explore the significance of effective temperature in stellar astrophysics
- Learn about the spectral characteristics of different star classes
- Investigate the role of Annie Cannon in refining stellar classifications
USEFUL FOR
Astronomers, astrophysics students, educators, and anyone interested in the classification of stars and the underlying principles of stellar spectra.