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A gravastar is an object hypothesized in astrophysics by Pawel O. Mazur and Emil Mottola as an alternative to the black hole theory. It has usual black hole metric outside of the horizon, but de Sitter metric inside. On the horizon there is a thin shell of matter. The term "gravastar" is a portmanteau of the words "gravitational vacuum star".[1]


In the original formulation by Mazur and Mottola, gravastars contain a central region featuring a p=-ρ false vacuum or "dark energy", a thin shell of p=ρ perfect fluid, and a true vacuum p=ρ=0 exterior. The dark energy like behavior of the inner region prevents collapse to a singularity and the presence of the thin shell prevents the formation of an event horizon, avoiding the infinite blue shift. The inner region has thermodynamically no entropy and may be thought of as a gravitational Bose–Einstein condensate. Severe red-shifting of photons as they climb out of the gravity well would make the fluid shell also seem very cold, almost absolute zero.

In addition to the original thin shell formulation, gravastars with continuous pressure have been proposed. These objects must contain anisotropic stress.[2]

Externally, a gravastar appears similar to a black hole: it is visible by the high-energy radiation it emits while consuming matter, and by the Hawking radiation it creates[citation needed]. Astronomers observe the sky for X-rays emitted by infalling matter to detect black holes. A gravastar would produce an identical signature. It is also possible, if the thin shell is transparent to radiation, that gravastars may be distinguished from ordinary black holes by different gravitational lensing properties as null geodesics may pass through.[3]

Mazur and Mottola suggest that the violent creation of a gravastar might be an explanation for the origin of our universe and many other universes, because all the matter from a collapsing star would implode "through" the central hole and explode into a new dimension and expand forever, which would be consistent with the current theories regarding the Big Bang.[4] This "new dimension" exerts an outward pressure on the Bose–Einstein condensate layer and prevents it from collapsing further.

Gravastars also could provide a mechanism for describing how dark energy accelerates the expansion of the universe. One possible hypothesis uses Hawking radiation as a means to exchange energy between the "parent" universe and the "child" universe, and so cause the rate of expansion to accelerate, but this area is under much speculation.[citation needed]

Gravastar formation may provide an alternate explanation for sudden and intense gamma-ray bursts throughout space.[citation needed]

LIGO's observations of gravitational waves from colliding objects have been found either to not be consistent with the gravastar concept,[5][6][7] or to leave the question unanswered.[8][9]

In comparison with black holes[edit]

By taking quantum physics into account, the gravastar hypothesis attempts to resolve contradictions caused by conventional black hole theories.[10]

Event horizons[edit]

In a gravastar, the event horizon is not present. The layer of positive pressure fluid would lie just outside the 'event horizon', being prevented from complete collapse by the inner false vacuum.[1] Due to the absence of an event horizon the time coordinate of the exterior vacuum geometry is everywhere valid.

Dynamic stability of gravastars[edit]

In 2007, theoretical work indicated that under certain conditions gravastars as well as other alternative black hole models are not stable when they rotate.[11] Theoretical work has also shown that certain rotating gravastars are stable assuming certain angular velocities, shell thicknesses, and compactnesses. It is also possible that some gravastars which are mathematically unstable may be physically stable over cosmological timescales.[12] Theoretical support for the feasibility of gravastars does not exclude the existence of black holes as shown in other theoretical studies.[13]

See also[edit]


  1. ^ a b . This solution of Einstein equations is stable and has no singularities. "Los Alamos researcher says 'black holes' aren't holes at all". Los Alamos National Laboratory. Archived from the original on 13 December 2006. Retrieved 10 April 2014.
  2. ^ Cattoen, Celine; Faber, Tristan; Visser, Matt (2005-09-25). "Gravastars must have anisotropic pressures". Classical and Quantum Gravity. 22 (20): 4189–4202. arXiv:gr-qc/0505137. Bibcode:2005CQGra..22.4189C. doi:10.1088/0264-9381/22/20/002.
  3. ^ Sakai, Nobuyuki; Saida, Hiromi; Tamaki, Takashi (2014-11-17). "Gravastar shadows". Phys. Rev. D. 90. arXiv:1408.6929. Bibcode:2014PhRvD..90j4013S. doi:10.1103/physrevd.90.104013.
  4. ^ "Is space-time actually a superfluid?". New Scientist. Archived from the original on 2006-06-09. Retrieved 2017-11-04. It’s the big bang," says Mazur. "Effectively, we are inside a gravastar.
  5. ^ Chirenti, Cecilia; Rezzolla, Luciano (2016-10-11). "Did GW150914 produce a rotating gravastar?". Physical Review D. 94 (8): 084016. arXiv:1602.08759. Bibcode:2016PhRvD..94h4016C. doi:10.1103/PhysRevD.94.084016. we conclude it is not possible to model the measured ringdown of GW150914 as due to a rotating gravastar.
  6. ^ "Did LIGO detect black holes or gravastars?". ScienceDaily. October 19, 2016. Retrieved 2017-11-04.
  7. ^ "LIGO's black hole detection survives the gravastar test - ExtremeTech". ExtremeTech. 2016-10-26. Retrieved 2017-11-04.
  8. ^ "Was gravitational wave signal from a gravastar, not black holes?". New Scientist. 2016-05-04. Retrieved 2017-11-04. Our signal is consistent with both the formation of a black hole and a horizonless object – we just can’t tell
  9. ^ Cardoso, Vitor; Franzin, Edgardo; Pani, Paolo (2016-04-27). "Is the gravitational-wave ringdown a probe of the event horizon?". Physical Review Letters. 116 (17): 171101. arXiv:1602.07309. Bibcode:2016PhRvL.116q1101C. doi:10.1103/PhysRevLett.116.171101. ISSN 0031-9007. PMID 27176511.
  10. ^ Stenger, Richard (22 January 2002). "Is black hole theory full of hot air?". Retrieved 10 April 2014.
  11. ^ Vitor Cardoso; Paolo Pani; Mariano Cadoni; Marco Cavaglia (2007). "Ergoregion instability of ultra-compact astrophysical objects". Physical Review D. 77 (12). arXiv:0709.0532. Bibcode:2008PhRvD..77l4044C. doi:10.1103/PhysRevD.77.124044.
  12. ^ Chirenti, Cecilia; Rezzolla, Luciano (October 2008). "Ergoregion instability in rotating gravastars" (PDF). Physical Review D. 78 (8). arXiv:0808.4080. Bibcode:2008PhRvD..78h4011C. doi:10.1103/PhysRevD.78.084011. Archived from the original (PDF) on 4 March 2016. Retrieved 10 April 2014.
  13. ^ Rocha; Miguelote; Chan; da Silva; Santos; Anzhong Wang (2008). "Bounded excursion stable gravastars and black holes". arXiv:0803.4200 [gr-qc].

Further reading[edit]

External links[edit]