Blue dwarf (red-dwarf stage)

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A blue dwarf is a predicted class of star that develops from a red dwarf after it has exhausted much of its hydrogen fuel supply. Because red dwarfs fuse their hydrogen slowly and are fully convective (allowing their entire hydrogen supply to be fused, instead of merely that in the core), they are predicted to have lifespans of trillions of years; the Universe is currently not old enough for any blue dwarfs to have formed yet. Their future existence is predicted based on theoretical models. [1]

Contents

Hypothetical scenario

Stars increase in luminosity as they age, and a more luminous star must radiate energy more quickly to maintain equilibrium. For stars more massive than red dwarfs, the resulting internal pressure increases their size, causing them to become red giants with larger surface areas. However, it is predicted that red dwarfs with less than 0.25  solar masses, rather than expanding, will increase radiative rate through an increase in surface temperature, hence emitting more blue and less red light. This is because the surface layers of red dwarfs do not become significantly more opaque with increasing temperature, so higher-energy photons from the interior of the star can escape, rather than being absorbed and re-radiated at lower temperatures as occurs in larger stars. [1]

Despite their name, blue dwarfs would not necessarily increase in temperature enough to become blue stars. Simulations have been conducted on the future evolution of red dwarfs with stellar mass between 0.06 M☉ and 0.25 M☉. [1] [2] [3] Of the masses simulated, the bluest of the blue dwarf stars at the end of the simulation had begun as a 0.14 M☉ red dwarf, and ended with surface temperature approximately 8,600 K (8,330 °C; 15,020 °F), making it a type A blue-white star.

End of stellar life

Blue dwarfs are believed to eventually completely exhaust their store of hydrogen fuel, and their interior pressures are insufficient to fuse any other fuel. Once fusion ends, they are no longer main-sequence "dwarf" stars and become so-called white dwarfs – which, despite the name, are not main-sequence "dwarfs" and are not stars, but rather stellar remnants. [1]

Once the former "blue"-dwarf stars have become degenerate, non-stellar white dwarfs, they cool, losing the remnant heat left over from their final hydrogen-fusing stage. The cooling process also requires enormous periods of time – much longer than the age of the universe at present – similar to the immense time previously required for them to change from their original red dwarf stage to their final blue dwarf stage. The stellar remnant white dwarf will eventually cool to become a black dwarf. (The universe is not old enough for any stellar remnants to have cooled to "black", so black dwarfs are also a well-founded, but still hypothetical object.)

It is also theoretically possible for these dwarfs at any stage of their lives to merge and become larger stars, such as helium stars. [4] Such stars should ultimately also become white dwarfs, which like the others, will cool down to black dwarfs.

See also

Related Research Articles

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References

  1. 1 2 3 4 Adams, F.C.; Bodenheimer, P.; Laughlin, G. (2005). "M dwarfs: Planet formation and long term evolution". Astronomische Nachrichten. 326 (10): 913–919. Bibcode:2005AN....326..913A. doi: 10.1002/asna.200510440 .
  2. ↑ Laughlin, G.; Bodenheimer, P.; Adams, F.C. (10 June 1997). "The end of the Main Sequence". The Astrophysical Journal. 482 (1): 420–432. Bibcode:1997ApJ...482..420L. doi: 10.1086/304125 . S2CID   121940819.
  3. ↑ Adams, F.C.; Laughlin, G.; Graves, G.J.M. (2004). Red dwarfs and the end of the Main Sequence. Revista Mexicana de Astronomía y Astrofísica. Vol. 22. pp. 46–49. CiteSeerX   10.1.1.692.5492 .
  4. ↑ Adams, Fred C.; Laughlin, Gregory (1997). "A dying universe: The long-term fate and evolution of astrophysical objects". Reviews of Modern Physics. 69 (2): 337–372. arXiv: astro-ph/9701131 . Bibcode:1997RvMP...69..337A. doi:10.1103/RevModPhys.69.337. S2CID   12173790.
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