مقایسهٔ روش‌ها

	اختروسیزمولوژی (Asteroseismology)	انتقال تابشی	تحلیل منحنی چرخش
حوزه	نجوم	نجوم	نجوم
خانواده	Process / pipeline	Process / pipeline	Process / pipeline
سال پیدایش	1970	1978	1970
پدیدآور	Roger Ulrich	Dimitri Mihalas	Vera Rubin
نوع	Observational technique	Computational simulation method	Observational kinematic method
منبع بنیادین	Ulrich, R. K. (1970). The five-minute oscillations on the solar surface. Astrophysical Journal, 162, 993-999.	Mihalas, D. (1978). Stellar Atmospheres (2nd ed.). San Francisco: W.H. Freeman. ISBN: 0716703742	Vera C. Rubin & W. Kent Ford Jr. (1970). Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions. Astrophysical Journal, 159, 379-403.
نام‌های دیگر	Stellar Oscillations, Stellar Seismology, Helioseismology	RT Modeling, Radiative Transport, Light Transport Simulation	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis
مرتبط	3	3	3
خلاصه	Asteroseismology is the study of stellar oscillations—tiny brightness and radial velocity variations caused by sound waves resonating inside stars. Proposed by Roger Ulrich in 1970 and established as a major field by the Kepler and TESS space telescopes, asteroseismology provides unprecedented precision in determining stellar masses, ages, and internal structure.	Radiative transfer is the mathematical treatment of how light propagates through matter, including absorption, emission, and scattering. Central to astrophysics and stellar atmosphere modeling, radiative transfer calculations translate physical conditions (density, temperature, composition) into observable spectra and colors, bridging theory and observation.	Galaxy rotation curve analysis is the technique of measuring how orbital velocities change with distance from the center of a galaxy. Pioneered by Vera Rubin and W. Kent Ford Jr. in 1970, rotation curves revealed one of astronomy's great mysteries: galaxies rotate too fast to be held together by their visible stars alone, providing direct evidence for dark matter.