General relativistic boson stars

By F. Schunck, E. W. Mielke. 2003

620 citations recorded by the source corpus.

There is accumulating evidence that (fundamental) scalar fields may exist in nature. The gravitational collapse of such a boson cloud would lead to a boson star (BS) as a new type of a compact object. As with white dwarfs and neutron stars, a limiting mass exists similarly, below which a BS is stable against complete gravitational collapse to a black hole. According to the form of the self-interaction of the basic constituents and spacetime symmetry, we can distinguish mini-, axidilaton, soliton, charged, oscillating and rotating BSs. Their compactness prevents a Newtonian approximation; however, modifications of general relativity, as in the case of Jordan?Brans?Dicke theory as a low-energy limit of strings, would provide them with gravitational memory. In general, a BS is a compact, completely regular configuration with structured layers due to the anisotropy of scalar matter, an exponentially decreasing 'halo', a critical mass inversely proportional to the constituent mass, an effective radius and a large particle number. Due to the Heisenberg principle, a completely stable branch exists, and as a coherent state, it allows for rotating solutions with quantized angular momentum. In this review, we concentrate on the fascinating possibilities of detecting the various subtypes of (excited) BSs: possible signals include gravitational redshift and (micro-)lensing, emission of gravitational waves, or, in the case of a giant BS, its dark matter contribution to the rotation curves of galactic halos.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/02a740e5a488e5deca833149d1bc3d089ca36535

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Citations in the corpus

Superradiance (2015, background): “re [528]: Boson stars made up of fundamental self-interacting scalar elds that are prevented from gravitational collapse through the Heinsenberg uncertainty principle (for reviews on the subject see [536,537,538]). Bosons stars can be as compact as a NS and as massive as the BH candidate at the cent”
Anisotropic solutions by gravitational decoupling (2017, methodology): “Indeed, this simple and systematic method could be conveniently exploited in a large number of relevant cases, such as the Einstein-Maxwell [21] and Einstein-Klein-Gordon system [22, 23, 24, 25], for higher derivative gravity [26, 27, 28], f(R)-theories of gravity [29, 30, 31, 32, 33, 34, 35], Hořav”
Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “These compact objects can be classified according to the scalar potential in the Klein-Gordon Lagrangian [533, 530, 535].”
The imitation game: Proca stars that can mimic the Schwarzschild shadow (2021, background): “timate, for all the computed BSs solutions, the virial identity and mass relations are obeyed within a factor of 10 9. 4 Scalar BSs Many scalar BS models have been considered over the years - see e:g:[9]. Here, we shall divide our analysis into two dierent cases, depending on the choice of the self-”
Numerical methods for finding stationary gravitational solutions (2015, background): “[268] F.”
Imaging a boson star at the Galactic center (2015, background): “A lot of work has been devoted to these objects and to their stability and we redirect to reviews containing the relevant references (Jetzer 1992; Schunck & Mielke 2003; Liebling & Palenzuela 2012).”
Kerr black holes with Proca hair (2016, background): “KBHsSH, moreover, are asymptotically flat, regular on and outside the event horizon, reduce to (specific) Kerr solutions in the limit of vanishing hair, and to gravitating solitons known as boson stars [43,44] in the limit of vanishing horizon.”