Search results
Results from the WOW.Com Content Network
Representative lifetimes of stars as a function of their masses The change in size with time of a Sun-like star Artist's depiction of the life cycle of a Sun-like star, starting as a main-sequence star at lower left then expanding through the subgiant and giant phases, until its outer envelope is expelled to form a planetary nebula at upper right Chart of stellar evolution A mass-radius plot ...
Often when a star is a member of a pair of close-orbiting binary stars, the tidal attraction of the gasses near the center of mass is sufficient to pull gas from one star onto its partner. This effect is especially prominent when the partner is a white dwarf, neutron star, or black hole. Mass loss in binary systems has particularly interesting ...
Simulated collision of two neutron stars. A stellar collision is the coming together of two stars [1] caused by stellar dynamics within a star cluster, or by the orbital decay of a binary star due to stellar mass loss or gravitational radiation, or by other mechanisms not yet well understood.
Astronomers recently spotted a black hole swallowing up a star like celestial spaghetti — and no, that's not science fiction. Star dies by "spaghettification" as it's consumed by black hole Skip ...
Any main-sequence star with an initial mass of greater than 8 M ☉ (eight times the mass of the Sun) has the potential to become a neutron star. As the star evolves away from the main sequence, stellar nucleosynthesis produces an iron-rich core. When all nuclear fuel in the core has been exhausted, the core must be supported by degeneracy ...
Diagram of stellar evolution, showing the various stages of stars with different masses. A black dwarf is a theoretical stellar remnant, specifically a white dwarf that has cooled sufficiently to no longer emit significant heat or light.
Swallowing up planets might be the reason that some stars appear more reddish than others, according to new research published on the preprint server arXiv.
The compression caused by the collapse raises the temperature until thermonuclear fusion occurs at the center of the star, at which point the collapse gradually comes to a halt as the outward thermal pressure balances the gravitational forces. The star then exists in a state of dynamic equilibrium. During the star's evolution a star might ...