Non-grey hydrogen burning evolution of sub-Solar mass Population III stars

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dc.creatorHarris, G. J.
dc.creatorLynas-Gray, A. E.
dc.creatorMiller, S.
dc.creatorTennyson, J.
dc.date2006-10-05
dc.date.accessioned2026-07-07T10:23:47Z
dc.date.available2026-07-07T10:23:47Z
dc.descriptionThe primordial elements, H, He and Li are included in a low temperature equation of state and monochromatic opacity function. The equation of state and opacity function are incorporated into the stellar evolution code NG-ELMS, which makes use of a non-grey model atmosphere computed at runtime. NG-ELMS is used to compute stellar evolution models for primordial and lithium free element mixtures, for stars in the sub-Solar mass range 0.8--0.15 Msol. We find that lithium has little or no effect upon the structure and observable properties of of stars in this mass range. Furthermore lithium is completely destroyed by fusion before the main sequence in stars of mass less than ~0.7 Mol. We find that on the red giant branch and Hayashi track, the use of a non-grey model atmosphere to provide the upper boundary conditions for the stellar evolution calculation, results in significantly cooler less luminous stars, across the mass range
dc.description9 pages, 9 figures Accepted for publication in MNRAS. The definitive version is available at www.blackwell-synergy.com
dc.identifierhttps://arxiv.org/abs/astro-ph/0610165
dc.identifierhttp://arxiv.org/abs/astro-ph/0610165
dc.identifierMon.Not.Roy.Astron.Soc.374:337-343,2007
dc.identifierdoi:10.1111/j.1365-2966.2006.11160.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175960
dc.subjectAstrophysics
dc.titleNon-grey hydrogen burning evolution of sub-Solar mass Population III stars
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