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The influence of rotation on optical emission profiles of O stars
- Source :
- Monthly Notices of the Royal Astronomical Society. 426:1043-1049
- Publication Year :
- 2012
- Publisher :
- Oxford University Press (OUP), 2012.
-
Abstract
- We study the formation of photospheric emission lines in O stars and show that the rectangular profiles, sometimes double peaked, that are observed for some stars are a direct consequence of rotation, and it is unnecessary to invoke an enhanced density structure in the equatorial regions. Emission lines, such as N IV 4058 and the N III 4634-4640-4642 multiplet, exhibit non-standard "limb darkening" laws. The lines can be in absorption for rays striking the center of the star and in emission for rays near the limb. Weak features in the flux spectrum do not necessarily indicate an intrinsically weak feature -- instead the feature can be weak because of cancellation between absorption in "core" rays and emission from rays near the limb. Rotation also modifies line profiles of wind diagnostics such as He II 4686 and Halpha and should not be neglected when inferring the actual stratification, level and nature of wind structures.
- Subjects :
- Physics
010308 nuclear & particles physics
Astrophysics::High Energy Astrophysical Phenomena
Flux
Astronomy and Astrophysics
Astrophysics::Cosmology and Extragalactic Astrophysics
Astrophysics
Rotation
01 natural sciences
Core (optical fiber)
Stars
13. Climate action
Space and Planetary Science
Limb darkening
0103 physical sciences
Astrophysics::Solar and Stellar Astrophysics
Astrophysics::Earth and Planetary Astrophysics
Emission spectrum
010303 astronomy & astrophysics
Astrophysics::Galaxy Astrophysics
Line (formation)
O-type star
Subjects
Details
- ISSN :
- 00358711 and 46344640
- Volume :
- 426
- Database :
- OpenAIRE
- Journal :
- Monthly Notices of the Royal Astronomical Society
- Accession number :
- edsair.doi...........fe9c223bb684482bafc839d1b5d953ba