April 9, 2015

Migrating hot jupiter as a model for non-coalescing black holes, and for always disjoint manifolds?

Filed under: Letters from Ionia — Tags: , , — zankaon @ 3:20 pm

Might hot jupiter`s inward migration to current assumed stable orbit serve as a model for the possibility of coalescing black holes?

Assuming a past 2-body interaction of gas giants, resulting in an additional vectorial component for subsequent inward spiraling hot jupiter; why would such inward spiraling cease?

Might it result from spin orbital dynamics, respectively for star and planet? Or is it when angular velocity becomes sufficient that one can consider as if one has (fictitious) centrifugal force off setting such inward migration? So not related to mass nor curvature. How would such model differ from inward spiraling black holes, and simulations thereof?

Since orbital velocity of earth is ~30 km/s, what would the orbital  velocity of a hot jupiter be? For conservation of angular momentum, with decrease in moment of inertia, would angular velocity be quite high? Would inward migration of hot jupiter be gradual; hence favoring settling into a stable orbit for billions of years? Might distant orbits, like for Proxima centuari, also only be possible if there is gradual settling into such extremely far out orbits?

Would  orbital velocity of hot jupiter be much increased, consistent with reduced moment of inertia, and angular momentum conservation? If not, would this be be evidence for, and consistent with, an ejected third body, and it`s contribution to changes in observed angular momentum components?

Might one consider such inward spiraling as approximation of equiangular spiral? Then use rectification of spiral to get distance along such inward spiral path; that is the distance from original orbital distance (of cold jupiter) to rectilinear axis passing through it`s star. If one then assumes the orbital velocity remained reasonable, with any change of a gradual nature, then the duration for such hot jupiter to arrive could seemingly be estimated – less than 500 million years?

Would such hot jupiter scenario seem more likely than coalescence of mass, in principle (angular momentum problem?) as well as for simulations? Likewise then for consideration of merging of other massive objects, such as for NS-NS stars or BH-NS merging for GRB origin, or for hot Jupiter and star considered merger?

That is, does nature have a problem with such massive merger models; perhaps related to angular momentum and centrifugal motion? Is this in turn related to larger theme that manifolds act as though they want to be left alone; perhaps they can not change. That is, disjoint, then aways disjoint; and if intersecting, then always intersecting; also resistance to deformation?

So might a hot jupiter migratory model, and assumed current stable orbit, serve as an example of what might happen for black holes attempting to coalesce, as well as also representative of manifold behavior in general?   TMM

Rectification of equiangular spiral.


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