Spatially Varying Stellar Opacity Model

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dc.contributor.authorNyambuya, G. G.
dc.date.accessioned2017-09-21T14:29:11Z
dc.date.accessioned2023-06-26T13:02:03Z
dc.date.available2017-09-21T14:29:11Z
dc.date.available2023-06-26T13:02:03Z
dc.date.issued2017-04
dc.descriptionJournal Articleen_US
dc.description.abstractUsing Larson (1982)’s empirical law as a solid foundational basis for our central thesis – for a plausible solution to the radiation problem of massive star formation, we argue in favour of a spatially varying dust-and-gas opacity. This spatially varying dust- and-gas opacity allows us to present – what appears to us, as – a perdurable solution to the long-standing riddle of massive star formation and the radiation barrier problem. In the proposed solution, massive stars form in the gravitationally bound dense dust-and-gas centres of massive molecular clouds via monolithic core accretion where the radiation problem is non-existent. Influenced by the radial mass profile, the opacity increases systematically from the stellar right up to the molecular cloud (core) surface. The opacity at the stellar surface is unbelievably ultra-low (∼ 10−12 kg−1m2) so much that, the radiation field should not be an impediment to accretion of any form – be it via direct radial in-fall of matter onto the nascent star or accretion through the disk. Ultimately, this model favours massive star formation via a scaled-up version of low mass star formation.en_US
dc.identifier.citationNyambuya G. G. 2017. Spatially Varying Stellar Opacity Model : A Plausible Solution to the Radiation Problem of Massive Star Formation. Research in Astronomy and Astrophysicsen_US
dc.identifier.urihttp://196.220.97.103:4000/handle/123456789/810
dc.language.isoenen_US
dc.publisherIOP Scienceen_US
dc.subjectaccretionen_US
dc.subjectmassiveen_US
dc.subjectstaren_US
dc.subjectformationen_US
dc.subjectradiationen_US
dc.subjectproblemen_US
dc.titleSpatially Varying Stellar Opacity Modelen_US
dc.title.alternativeA Plausible Solution to the Radiation Problem of Massive Star Formationen_US
dc.typeArticleen_US
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