Proyecto IACOB: Una Nueva Era en el Estudio de Estrellas OB Galácticas

Año de inicio
2014
Año fin
2017
Unidad organizativa
Descripción

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 understand the evolution of the Cosmos. In spite of the remarkable avances in the modelling and spectroscopic analysis techniques of these stars occurred in the last two decades, our knowledge of these important (but complex) astrophysical objects has been, until very recently, limited to conclusions extracted from the analysis of single-epoch medium resolution spectroscopic observations of relatively small samples. This situation is slowly but surely changing with the compilation and analysis of large spectroscopic surveys of OB stars in the Milky Way and other external galaxies. The IACOB project is an ambitious long-term project which is contributing to the new era of investigation of massive stars by concentrating on Galactic OB stars. In particular, the project aims at building a large database of high-resolution, multi-epoch, spectra of Galactic OB stars (uisng the FIES@NOT2.5m and HERMES@MERCATOR1.2m facilities at the ORM observatory, La Palma, Spain), and the scientific exploitation of the database using state-of-the-art models and techniques. The main drivers of the project are: (1) to increase the statistics of Galactic OB stars with accurate physical parameters and abundances, (2) to investigate in detail some of the still open questions in our knowledge of the physical properties and evolution of massive stars (e.g., the actual masses of these stars, the nature of the O Vz stars, the driving mechanism of stellar winds in the weak wind regime, the uncertain stage of B supergiants in an evolutionary context, the actual rotational velocities of massive stars, the physical origin of the macroturbulent broadening, and the impact of rotation/binarity/pulsations on the evolution of massive stars), and (3) to provide an unique ground-based spectroscopic database supporting/complementing the future Gaia database.

Investigador principal
Colaboradores
Dr.
KLAUS SIMON RUBKE ZUÑIGA
Dr.
INÉS CAMACHO IÑESTA
Dr.
Jesús Maíz Apellaniz
Dr.
Ignacio Negueruela
Dr.
Norberto Castro
Dr.
Carolina Sabín-Sanjulian
Dr.
Javier Lorenzo
Dr.
Ricardo Dorda e
Dr.
María Fernanda Nieva
Dr.
Jorge García-Rojas
Dr.
Nevy Markova
Dr.
Miguel A. Urbaneja
Dr.
Rodolfo Barbá
Dr.
Julia Arias

Publicaciones y comunicaciones científicas relacionadas

  • The IACOB project. I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening

    Context. Stellar rotation is an important parameter in the evolution of massive stars. Accurate and reliable measurements of projected rotational velocities in large samples of OB stars are crucial to confront the predictions of stellar evolutionary models with observational constraints. Aims: We reassess previous determinations of projected

    Simón-Díaz, S. et al.

    Fecha de publicación:

    2
    2014
  • The B Fields in OB Stars (BOB) Survey

    The B fields in OB stars (BOB) survey is an ESO Large Programme collecting spectropolarimetric observations for a large number of early-type stars in order to study the occurrence rate, properties, and ultimately the origin of magnetic fields in massive stars. A total of 98 objects was observed over 20 nights with FORS2 and HARPSpol to July 2014

    Morel, T. et al.

    Fecha de publicación:

    9
    2014
  • B fields in OB stars (BOB). Detection of a strong magnetic field in the O9.7 V star HD 54879

    The number of magnetic stars detected among massive stars is small; nevertheless, the role played by the magnetic field in stellar evolution cannot be disregarded. Links between line profile variability, enhancements/depletions of surface chemical abundances, and magnetic fields have been identified for low-mass B-stars, but for the O-type domain

    Castro, N. et al.

    Fecha de publicación:

    9
    2015

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