Observational Consequences of Turbulent Pressure in the Envelopes of Massive Stars

Grassitelli, L.; Fossati, L.; Simón-Diáz, S.; Langer, N.; Castro, N.; Sanyal, D.
Referencia bibliográfica

The Astrophysical Journal Letters, Volume 808, Issue 1, article id. L31, 6 pp. (2015).

Fecha de publicación:
7
2015
Número de autores
6
Número de autores del IAC
1
Número de citas
45
Número de citas referidas
39
Descripción
The major mass fraction of the envelope of hot luminous stars is radiatively stable. However, the partial ionization of hydrogen, helium, and iron gives rise to extended sub-surface convection zones in all of them. In this work, we investigate the effect of the pressure induced by the turbulent motion in these zones based on the mixing-length theory, and we search for observable consequences. We find that the turbulent pressure fraction can amount up to ∼ 5% in OB supergiants and up to ∼ 30% in cooler supergiants. The resulting structural changes are, however, not significantly affecting the evolutionary tracks compared to previous calculations. Instead, a comparison of macroturbulent velocities derived from high-quality spectra of OB stars with the turbulent pressure fraction obtained in corresponding stellar models reveals a strong correlation between these two quantities. We discuss a possible physical connection and conclude that turbulent pressure fluctuations may drive high-order oscillations, which—as conjectured earlier—manifest themselves as macroturbulence in the photospheres of hot luminous stars.
Proyectos relacionados
Imagen Proyecto IACOB
Proyecto IACOB: Una Nueva Era en el Estudio de Estrellas OB Galácticas

Massive stars has been many times claimed as Cosmic Engines and Gifts of Nature for the study of the Universe, from the Solar neighbourhood to the large-z Universe. The complete understanding of the physical properties and evolution of massive stars (and their interplay with the ISM) is crucial for many fields of Astrophysics and, ultimately, to

Sergio
Simón Díaz