Compara mètodes

	Imatge Zeeman-Doppler	Astroseismologia	Transferència radiativa	Anàlisi de corbes de rotació
Camp	Astronomia	Astronomia	Astronomia	Astronomia
Família	Process / pipeline	Process / pipeline	Process / pipeline	Process / pipeline
Any d'origen	1997	1970	1978	1970
Autor original	Jean-Francois Donati	Roger Ulrich	Dimitri Mihalas	Vera Rubin
Tipus	Observational spectroscopic method	Observational technique	Computational simulation method	Observational kinematic method
Font seminal	Donati, J. F., Semel, M., Carter, B. D., Rees, D. E., & Collier Cameron, A. (1997). Spectropolarimetric observations of active stars. Monthly Notices of the Royal Astronomical Society, 291(4), 658-682.	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.
Àlies	ZDI, Doppler Imaging, Magnetic Field Mapping	Stellar Oscillations, Stellar Seismology, Helioseismology	RT Modeling, Radiative Transport, Light Transport Simulation	Galactic Rotation Curves, Rotation Curve Method, Velocity Curve Analysis
Relacionats	3	3	3	3
Resum	Zeeman-Doppler imaging is a technique for reconstructing stellar magnetic field maps by combining Doppler broadening of spectral lines with the Zeeman splitting caused by magnetic fields. Pioneered by Jean-Francois Donati in the 1990s, this method reveals how magnetic fields are distributed on stellar surfaces and how they evolve with time.	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.