Physics of Ionized Nebulae

Description

The research that is being carried out by the group can be condensed into two main lines:

1) Study of the structure, dynamics, physical conditions and chemical evolution of Galactic and extragalactic ionized nebulae through detailed analysis and modelization of their spectra. Investigation of chemical composition gradients along the disk of our Galaxy and in nearby galaxies.

2) Determine the physical-chemical conditions of galactic planetary nebulae with bipolar geometry and nebulae around symbiotic stars. The aim is to understand the origin of bipolarity and to test theoretical models that attempt to explain nebular morphology and kinematics, with special emphasis on models with central binary stars. We will also study the implications of the evolution of binary systems in other astrophysical scenarios, such as the formation of jets, cataclysmic variables, and nova and supernova-type explosions.

  1. Using EMIR/GTC spectra in the near infrared range, tellurium and bromine emission lines have been detected for the first time in two planetary nebulae. These heavy element detections in one of their places where they are formed, give us information about the abundance patterns of heavy elements owing to the r-process and the s-process.

Publications related

  • Small-spatial-scale variations of nebular properties and the abundance discrepancy in three Galactic HII regions

    We present the results of long-slit spectroscopy in several slit positions that cover different morphological structures of the central parts of three bright Galactic HII regions: M8, M17 and NGC 7635. We study the spatial distributions of a large number of nebular parameters, such as the extinction coefficient, line fluxes, physical conditions and

    Mesa-Delgado, A. et al.

    Advertised on:

    7
    2010
  • M1-78: a nitrogen-rich Galactic compact H II region beyond the Perseus arm

    Context: There is considerable controversy surrounding the nature of M1-78, a compact nebula located beyond the Perseus arm. It was first classified as a planetary nebula and is nowadays generally considered to be a compact H II region. Aims: To investigate the nature of M1-78 further, we present a detailed spectroscopic study of M1-78 in the

    Martín-Hernández, N. L. et al.

    Advertised on:

    4
    2008
  • Fluorescent Excitation of Balmer Lines in Gaseous Nebulae: Case D

    Nonionizing stellar continua are a potential source of photons for continuum pumping in the hydrogen Lyman transitions. In the environments where these transitions are optically thick, de-excitation occurs through higher series lines. As a result, the emitted flux in the affected lines has a fluorescent contribution in addition to the usual

    Luridiana, V. et al.

    Advertised on:

    2
    2009

Talks related

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