Supermassive dark stars powered by dark matter annihilation can collapse into quasi-stars whose envelopes expand and cool to match the observed properties of many JWST Little Red Dots while bypassing the restrictive conditions of nuclear-powered supermassive star formation.
year = 1964, month = aug, volume = 140, pages =
4 Pith papers cite this work. Polarity classification is still indexing.
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A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.
citing papers explorer
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JWST's Little Red Dots as collapsed Supermassive Dark Stars
Supermassive dark stars powered by dark matter annihilation can collapse into quasi-stars whose envelopes expand and cool to match the observed properties of many JWST Little Red Dots while bypassing the restrictive conditions of nuclear-powered supermassive star formation.
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Non-linear Dynamical Stability of Magnetic Polytropes
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
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Mass and Spin Growth of Very Massive Stars in Star Clusters Potentially Associated with Little Red Dots
Simulations show VMS in star clusters reach 10^3-10^4 solar masses with dimensionless spins >10 under bloated accretion conditions, potentially forming spinning IMBHs that produce GW bursts like GW190521.
- Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots