Global monopole surrounded by quintessence-like matter

Abstract

We present new static spherically-symmetric solutions of Einstein equations with the quintessencelike matter surrounding a global monopole. These new solutions of the coupling scalar-Einstein equations are more complicated, which depend on the parameter of equation of state −1 < wq < − 1 3 . A gravitating global monopole produces a gravitational field of de Sitter kind outside the core in addition to a solid angular deficit. In the wq = − 1 3 case, we have proved that the solution cannot exist since the density of quintessence-like tends to zero if wq → − 1 3 . As a new feature, these monopoles have the outer horizon depending on both Goldstone field and quintessence-like. Since current observations constrain −1.14 < wq < −0.93, new global monopoles have interesting astrophysical applications.

Massive scalar field quasinormal modes of a black hole with quintessence-like matter and a deficit solid angle

“…Recently, Li et al (2008) gave the solutions for a global monopole surrounded by the static spherically-symmetric quintessence-like matter. And when such a global monopole is swallowed by an ordinary black hole withM, a black hole with quintessence-like matter and a deficit solid angle can be formed as follows:…”

“…In the fundamental physics, QNMs are helpful to understand more deeply quantum gravity and black hole physics. This has motivated a lot of work on the calculating the QNMs of different field perturbations with massless and massive around various black holes (Vishveshwara 1970;Maldacena 1998;Leaver 1985;Nollert 1993Nollert , 1999Kunstatter 2003;Cardoso and Lemos 2001a, 2001bCardoso et al 2004;Beri et al 2004;Beri and Cardoso 2006;Konoplya 2002aKonoplya , 2002bKonoplya and Zhidenko 2006;Konoplya and Abdalla 2005;Ferrari et al 2001;Wu and Zhao 2004;Giammatteo and Moss 2005;Fiziev 2006;Giammatteo and Jing 2005;Cho 2003;Jing 2004;Ma et al 2008;Simone and Will 1992;Burko and Khanna 2004). Then, it is well known that the behavior of the massive scalar field in a black hole background is quite different from that of the massless one in many aspects: (a) it presents the so-called super-radiant instability (Bekenstein and Schiffer 1998), which does not appear in the massless field; (b) it may have infinitely longliving modes called quasi-resonances (Konoplya and Zhidenko 2005); (c) it also has a universal behavior not dependent on the spin of the field at asymptotically late times 1998).…”

“…In the previous paper (Li et al 2008), the solutions of Einstein equations with static spherically-symmetric quintessence-like matter surrounding a global monopole have been given. Furthermore, this monopole become a black hole with quintessence-like matter and a deficit solid angle when it is swallowed by an ordinary black hole.…”

Thermodynamic properties of Reissner—Nordström—de Sitter quintessence black holes

“…[17] showed the spherical spacetime solutions with parameter n. A more general form of the polynomial solutions of the spherically symmetric spacetime is given in Refs. [1] and [18], where some of the thermodynamic properties of a black hole surrounded by quintessence have been discussed. As is well known, the de Sitter solution has played a significant role in the study of the thermodynamics of black holes.…”

Quasinormal modes of Dirac field perturbation in Reissner-Nordström black hole surrounded by quintessence

“…Recently, Kiselev [19] considered Einstein's field equations for a black hole surrounded by the quintessential matter and obtained a new solution, which depend on the state parameter w q of the quintessence. From then on, several people investigate the property of the black hole surrounded by quitessence [20,21,22,23,24,25,26,27,28], and get some valuable conclusion. In this paper, we use the third-order WKB approximation to explore the quasinormal modes of massless Dirac perturbation [29,30,31,32,33] in RN(Reissner-Nordström) black hole surrounded by quintessence.…”