Thank you for finally making a prediction, William. Now, can you provide the math that shows that a MECO can actually fragment, and show that the physical conditions that you assume in that model are physically viable? Please start a thread in the ATM section where you work this through, or cite a paper that does so.
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Originally Posted by William
The Paradox of Youth stars occur in a region where gas clouds cannot theoretically form due to the tidal affects of the massive compact object. It is not physically possible for the stars in question to have migrated to the location, based on the short life times of the massive stars in the clusters and the maximum distance the stars could possible have moved in their lifetimes. There is no other working hypothesis.
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It's funny, how once again, the paper you linked in the OP has an explanation for your "impossibilities"
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Originally Posted by Alexander (2005), section 7
The solutions proposed so far for the riddle of the young stars (see reviews by Genzel et al. 2003b; Ghez et al. 2005) fall into three main categories: unusual modes of star formation near the MBH; rejuvenation of old stars from the local population; and dynamic migration or capture from farther out, where stars can form. While each has some attractive features, none is quite satisfactory. The paradox of youth remains unsolved at this time.
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However, it is not clear that the required very high compression ratio (Eq. 7.1) can be achieved in such collisions.
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This scenario has yet to be studied in detail. Here again, the problem is that it is unclear whether radiation pressure can lead to the very high compression ratio that is required for fragmentation.
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The disk fragmentation model is a promising scenario for the formation of the star disks and the massive young stars on the 0.1 pc scale, but it is less clear whether it can account for the S-cluster as well.
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The weakness of this scenario for explaining the S-stars is that, lacking quantitative calculations, it is unclear whether this method can actually form such a tightly bound cluster, and it is also unclear whether collisional stripping is efficient enough and consistent with the apparent normalcy of the B-stars.
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That's a sample of the caveats for some of the "no other working hypothes[es]." Doesn't sound like any of them are "not physically possible," just that no one has yet studied this type of situation in enough detail. And, as is usually the case, the correct explanation likely involves the interplay of several of these models. I know some people who are working in this area: the problem is the number of effects that one must take into account in the models has only made them tractable (on large computing clusters) recently.
I'm waiting to see the quantitative predictions of your model of MECO fragmentation, including how the fragmentation products would look exactly like O and B stars and why they would have randomly oriented orbits.