The Molecular Line Opacity of MgH in Cool Stellar Atmospheres | Zendy

Philippe F. Weck | Zendy; A. Schweitzer | Zendy; P. C. Stancil | Zendy; P. H. Hauschildt | Zendy; K. Kirby | Zendy

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The Molecular Line Opacity of MgH in Cool Stellar Atmospheres

Author(s) -

Philippe F. Weck,

A. Schweitzer,

P. C. Stancil,

P. H. Hauschildt,

K. Kirby

Publication year - 2003

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/344722

Subject(s) - opacity , rotational–vibrational spectroscopy , physics , line (geometry) , stellar atmosphere , astrophysics , spectral line , dipole , stars , stellar classification , computational physics , astronomy , optics , quantum mechanics , mathematics , geometry

A new, complete, theoretical rotational and vibrational line list for the A-Xelectronic transition in MgH is presented. The list includes transitionenergies and oscillator strengths for all possible allowed transitions and wascomputed using the best available theoretical potential energies and dipoletransition moment function with the former adjusted to account for experimentaldata. The A-X line list, as well as new line lists for the B'-X and the X-X(pure rovibrational) transitions, were included in comprehensive stellaratmosphere models for M, L, and T dwarfs and solar-type stars. The resultingspectra, when compared to models lacking MgH, show that MgH providessignificant opacity in the visible between 4400 and 5600 Angstrom. Further,comparison of the spectra obtained with the current line list to spectraobtained using the line list constructed by Kurucz (1993) show that the Kuruczlist significantly overestimates the opacity due to MgH particularly for thebands near 5150 and 4800 Angstrom with the discrepancy increasing withdecreasing effective temperature.Comment: 10 pages, 4 figures, 3 table

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