User:ZaperaWiki44/sandbox/Quasi-star: Difference between revisions

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Quasi-stars formed in metal-enriched regions may be

The most direct prediction of this work is shown in Fig. 4, where we estimate the detectability of QSs in a JWST field of view. At low metallicities, QSs at redshifts of a few may resemble featureless blackbodies, with colours reminiscent of brown dwarfs. Direct redshift measurements may not be feasible, in which case QSs would have to be identified via their massive hosts. Their low numbers – a consequence of their short lifetimes – will make it even more challenging to find them with a telescope having a relatively small field of view. It is possible that some QSs could have formed in metal-enriched regions and even at relatively low redshifts (z≳ 2). These might be relatively easy to detect but extremely rare. Other, secondary characteristics of QSs might conceivably aid in their detection, e.g. if accretion on to the BH deep in the core leads to the formation of a jet that pierces the stellar surface.--><ref name=volonteri>{{cite journal|doi=10.1111/j.1365-2966.2010.17359.x}}</ref>