In a recent paper, Hod has proven no-go theorem for asymptotically flat static regular boson stars. In the present work, we extend discussions to the gravity with a negative cosmological constant. We consider a scalar field vanishing at infinity. In the asymptotically AdS background, we show that spherically symmetric regular boson stars cannot be constructed with self-gravitating static scalar fields, whose potential is positive semidefinite and increases with respect to its argument.
It is proved that self-gravitating static scalar fields whose self-interaction potential $V(ψ^2)$ is a monotonically increasing function of its argument cannot form spherically symmetric asymptotically flat bound matter configurations. Our compact theorem rules out, in particular, the existence of spatially regular static boson stars made of nonlinear massive scalar fields.
We present a compact theorem which reveals the fact that static spatially regular massive scalar fields with nonminimal coupling to gravity cannot form spherically symmetric asymptotically flat horizonless matter configurations. In particular, the no-go theorem rules out the existence of boson stars made of static scalar fields with generic values of the physical parameter $ξ$ which quantifies the coupling between the spacetime curvature and the massive bosonic fields.
The stability of the recently proposed static solutions for boson stars is analyzed. These solutions of Einstein-Klein-Gordon (EKG) equations arise from considering the interaction of a real scalar field with matter. We assume that the inclusion of the scalar field in addition with matter, allows to justify that stability implies that the total mass of the solution should grow when the initial condition for the density of matter at the origin is also increased. Employing numerical values for the static boson star based on a linear relation between the source and the energy density and between …
Heavy fields of Hubble scale order present during inflation contribute to the non-Gaussian signature for the three-point function of the inflaton. Taking into account that Hubble scale is around the scale of grand unified theory (GUT), this opens a possibility that the GUT scale signatures, which are very hard to be discovered at collider, might be detectable by using information from the precise observations of cosmic microwave background. We discuss a detactability of the $X, Y$ gauge boson present in any GUT in a framework of cosmological collider physics. Calculating one-loop contributions…
Cosmological Collider Physics gives us the opportunity to probe high-energy physics from observing the spacetime fluctuations generated during inflation imprinted on the cosmic microwave background. In other words, it is a method to investigate physics on energy scales that cannot be reached by terrestrial accelerators by means of precise observations of the universe. In this paper, we focus on the case where the GUT scale is close to the energy scale of inflation, and calculate three point function of inflaton by exchanging the Higgs boson in GUT at tree level. The results are found to be con…
Charged Compact Boson Stars and Shells in the Presence of a Cosmological Constant
本文研究了玻色子星和玻色子壳的理论，该理论涉及耦合到U（1）规范场和引力的大质量复标量场，在一个存在宇宙学常数$Λ$的锥形势中，我们把它当作一个取正负值的自由参数，从而使我们可以分别在de Sitter和Anti de Sitter空间中研究该理论。玻色子星被发现有两种类型，具有球状或壳状电荷密度。我们研究了这些解的性质，并确定了它们在某些特定参数值下的存在域。Kleihaus，Kunz，Laemmerzahl和List在一个理论中也得到了类似的解，这个理论涉及无质量复标量场与U（1）规范场和引力耦合，在没有宇宙学常数$Λ$的情况下，在锥形势中。
In light of no discovered new physics at the LHC, ideas which tackle the Hierarchy Problem without novelties around the TeV scale must be taken seriously. Such is a cosmological relaxation model of the Higgs mass, proposed in the pre-LHC era, which does not rely on new physics below the Planck scale. This scenario introduces a different notion of naturalness according to which the vacuum with a small expectation value of the Higgs field corresponds to an infinitely enhanced entropy point of the vacuum landscape that becomes an attractor of cosmological inflationary evolution. In this framework…
We point out that gravitational wave detectors such as LISA have the potential of probing a cosmological time evolution of the Higgs boson self-coupling constant $λ$ and thus the Higgs boson's mass $m_H= \sqrt{ 2 λ} v$. The phase transition of the Standard Model could have been a first order one if the Higgs mass was below 72 GeV at a temperature $T_\star \ge 100$ GeV. Gravitational waves could thus have been produced during the electroweak phase transition. A discovery by LISA of a stochastic background of gravitational waves with a characteristic frequency $k_\star \ge 10^{-5}$ Hz could be i…
We obtain cosmological solutions with Kasner-like asymptotics in N=2 gauged and ungauged supergravity by maximal analytic continuation of planar versions of non-extremal black hole solutions. Initially, we construct static solutions with planar symmetry by solving the time-reduced field equations. Upon lifting back to four dimensions, the resulting static regions are incomplete and bounded by a curvature singularity on one side and a Killing horizon on the other. Analytic continuation reveals the existence of dynamic patches in the past and future, with Kasner-like asymptotics. For the ungauge…
We discuss the Higgs mass and cosmological constant hierarchy puzzles with emphasis on the interplay of Poincare invariance, mass generation and renormalization group invariance. A plausible explanation involves an emergent Standard Model with the cosmological constant scale suppressed by power of the large scale of emergence. In this scenario the cosmological constant scale and neutrino masses should be of similar size.
Brane-world generalizations of the Einstein static universe
一个静态的弗里德曼膜在一个5维体（兰德尔-桑德拉姆类型的场景）可以有一个非常不同的密度，压力，曲率和宇宙学常数之间的关系比在广义相对论爱因斯坦静态宇宙的情况下。特别是，静态弗里德曼膜具有零宇宙学常数和3-曲率，但满足rho>0和rho+3 p>0，是可能的。此外，我们发现静态弗里德曼膜在满足爱因斯坦方程，但不是Schwarzschild-anti de Sitter或其专门化的散装。在具有负体积宇宙学常数的模型中，正的膜张力导致负的密度和3曲率。
We investigate Polish doughnuts with a uniform constant specific angular momentum distribution in the space-times of rotating boson stars. In such space-times thick tori can exhibit unique features not present in Kerr space-times. For instance, in the context of retrograde tori, they may possess two centers connected or not by a cusp. Rotating boson stars also feature a static ring, neither present in Kerr space-times. This static ring consists of static orbits, where particles are at rest with respect to a zero angular momentum observer at infinity. Here we show that the presence of a static …
This is the second of two works, in which we discuss the definition of an appropriate notion of mass for static metrics, in the case where the cosmological constant is positive and the model solutions are compact. In the first part, we have established a positive mass statement, characterising the de Sitter solution as the only static vacuum metric with zero mass. In this second part, we prove optimal area bounds for horizons of black hole type and of cosmological type, corresponding to Riemannian Penrose inequalities and to cosmological area bounds à la Boucher-Gibbons-Horowitz, respectively.…
Bosonic and Fermionic love number of static acoustic black hole
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；School of Physics and Optoelectronics, South China University of Technology（华南理工大学物理与光电工程学院）
