Spectroscopic Analysis of Massive Stars
Summary
Spectroscopic analysis of massive stars probes their physical properties, chemical compositions and dynamical behaviours by examining the absorption and emission features imprinted on their spectra. High‐resolution observations across optical and infrared wavelengths reveal information on stellar atmospheres, wind velocities, surface abundances and circumstellar environments. Key diagnostics include hydrogen and metal line profiles, molecular band heads and continuum shapes, which together constrain effective temperatures, mass‐loss rates and evolutionary stages. Modern instruments, such as echelle spectrographs on large telescopes and interferometric arrays, have enabled detailed studies of complex systems including B[e] supergiants, luminous blue variables and yellow hypergiants. By combining spectroscopy with radiative‐transfer models and hydrodynamical simulations, researchers can infer the geometry of winds and discs, the presence of shocks, and the role of rotation and binarity in shaping the observed features. Such insights are critical for improving theoretical models of massive‐star evolution, feedback to the interstellar medium and pre‐supernova configurations.
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Spectroscopic Analysis of Massive Stars publication trend
The graph below shows the total number of articles in spectroscopic analysis of massive stars across all publications each year (not limited to Nature Index journals).
Technical terms
Spectroscopy: The study of the interaction between matter and electromagnetic radiation as a function of wavelength or frequency, used to derive physical properties of stars.
Emission Line: A bright feature in a spectrum produced when atoms or molecules emit photons at specific wavelengths, indicating hot or excited gas.
CO Band Emission: Molecular emission from carbon monoxide in the near-infrared, appearing as band heads that trace cool, dense gas around stars.
Keplerian Rotation: Orbital motion of gas or particles around a central mass following Kepler’s laws, characterised by velocity inversely proportional to the square root of radius.
Circumstellar Envelope: The region of gas and dust surrounding a star, shaped by stellar winds, mass ejections and disc formation processes.
References
- Rings, Shells, and Arc Structures Around B[e] Supergiants. I. Classical Tools of Nonlinear Hydrodynamics. The Astrophysical Journal (2024).
- Dense Molecular Environments of B[e] Supergiants and Yellow Hypergiants. Galaxies (2023).
- New Insight into the FS CMa System MWC 645 from Near-Infrared and Optical Spectroscopy. Galaxies (2023).
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