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On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars

Mendigutía, I. ; Oudmaijer, R. D. ; Rigliaco, E. ; Fairlamb, J. R. ; Calvet, N. ; Muzerolle, J. ; Cunningham, N. ; Lumsden, S. L.

In: Monthly Notices of the Royal Astronomical Society, 2015, vol. 452, no. 3, p. 2837-2844

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    Titre
    • On the origin of the correlations between the accretion luminosity and emission line luminosities in pre-main-sequence stars
    Auteur
    • Mendigutía, I.. School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
    • Oudmaijer, R. D.. School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
    • Rigliaco, E.. Swiss Federal Institute of Technology, Department of Physics-Institute for Astronomy, Wolfgang-Pauli-Strasse 27, CH-8093 Zurich, Switzerland
    • Fairlamb, J. R.. School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
    • Calvet, N.. Department of Astronomy, University of Michigan, 830 Dennison Building, 500 Church Street, Ann Arbor, MI 48109, USA
    • Muzerolle, J.. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
    • Cunningham, N.. School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
    • Lumsden, S. L.. School of Physics and Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2015, vol. 452, no. 3, p. 2837-2844. Oxford University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:289360
    Summary
    Correlations between the accretion luminosity and emission line luminosities (Lacc and Lline) of pre-main-sequence (PMS) stars have been published for many different spectral lines, which are used to estimate accretion rates. Despite the origin of those correlations is unknown, this could be attributed to direct or indirect physical relations between the emission line formation and the accretion mechanism. This work shows that all (near-UV/optical/near-IR) Lacc-Lline correlations are the result of the fact that the accretion luminosity and the stellar luminosity (L*) are correlated, and are not necessarily related with the physical origin of the line. Synthetic and observational data are used to illustrate how the Lacc-Lline correlations depend on the Lacc-L* relationship. We conclude that because PMS stars show the Lacc-L* correlation immediately implies that Lacc also correlates with the luminosity of all emission lines, for which the Lacc-Lline correlations alone do not prove any physical connection with accretion but can only be used with practical purposes to roughly estimate accretion rates. When looking for correlations with possible physical meaning, we suggest that Lacc/L* and Lline/L* should be used instead of Lacc and Lline. Finally, the finding that Lacc has a steeper dependence on L* for T Tauri stars than for intermediate-mass Herbig Ae/Be stars is also discussed. That is explained from the magnetospheric accretion scenario and the different photospheric properties in the near-UV