Search for $p \bar{p} \rightarrow WZ \rightarrow l\nu_l b \bar{b}$ signal with the CDF experiment at Tevatron

Pani, P.

doi:10.2172/984600

Cited by 6 publications

(7 citation statements)

References 6 publications

(9 reference statements)

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“…In recent years superradiant instabilities of astrophysical BHs have been used -together with precision measurements of BH mass and spin (see e.g. [30]) -to constrain stringy axions and ultralight scalars [24,31] (these constraints being complementary to those coming from cosmological observations [32,33]), to derive bounds on light vector fields [20] and on the mass of the graviton [22], as well as to put intrinsic bounds on magnetic fields near BHs [34] and on the fraction of primordial BHs in dark matter [35]. However, all these predictions are based on a linearized analysis, neglecting backreaction and other competitive effects -such as GW emission and gas accretion -which can have an impact on the development of the process (see Fig.…”

Section: Introductionmentioning

confidence: 99%

Black holes as particle detectors: evolution of superradiant instabilities

Brito

Cardoso

Pani

2015

Class. Quantum Grav.

278

398

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Superradiant instabilities of spinning black holes can be used to impose strong constraints on ultralight bosons, thus turning black holes into effective particle detectors. However, very little is known about the development of the instability and whether its nonlinear time evolution accords to the linear intuition. For the first time, we attack this problem by studying the impact of gravitational-wave emission and gas accretion on the evolution of the instability. Our quasi-adiabatic, fully-relativistic analysis shows that: (i) gravitational-wave emission does not have a significant effect on the evolution of the black hole, (ii) accretion plays an important role and (iii) although the mass of the scalar cloud developed through superradiance can be a sizeable fraction of the black-hole mass, its energy-density is very low and backreaction is negligible. Thus, massive black holes are well described by the Kerr geometry even if they develop bosonic clouds through superradiance. Using Monte Carlo methods and very conservative assumptions, we provide strong support to the validity of the linearized analysis and to the bounds of previous studies.

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Section: Introductionmentioning

confidence: 99%

Black holes as particle detectors: evolution of superradiant instabilities

Brito

Cardoso

Pani

2015

Class. Quantum Grav.

278

398

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“…Other types of EOS-independent relations were also well studies in the literature (see e.g. [42][43][44][45][46][47][48][49][50][51][52][53]).…”

Section: Introductionmentioning

confidence: 99%

Rapidly rotating neutron stars with a massive scalar field—structure and universal relations

Doneva

Yazadjiev

2016

J. Cosmol. Astropart. Phys.

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We construct rapidly rotating neutron star models in scalar-tensor theories with a massive scalar field. The fact that the scalar field has nonzero mass leads to very interesting results since the allowed range of values of the coupling parameters is significantly broadened. These deviations from pure general relativity can be very large for values of the parameters that are in agreement with the observations. The rapid rotation can magnify the differences several times compared to the static case. The universal relations between the normalized moment of inertia and quadrupole moment are also investigated both for the slowly and rapidly rotating cases. The results show that these relations are still EOS independent up to a large extend and the deviations from pure general relativity can be large. This places the massive scalar-tensor theories amongst the few alternative theories of gravity that can be tested via the universal I-Love-Q relations.

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“…We should note that also a variety of other (nearly) EOS independent relations exists in the literature connecting different neutron star properties, their oscillations spectrum, etc. (see for example [16][17][18][19][20][21][22][23][24][25][26]).…”

Section: Introductionmentioning

confidence: 99%

I-Q relations for rapidly rotating neutron stars inf(R)gravity

Doneva¹,

Yazadjiev²,

Kokkotas³

2015

Phys. Rev. D

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In the present paper we study the behavior of the normalized I-Q relation for neutron stars in a particular class of f (R) theories of gravity, namely the R 2 gravity that is one of the most natural and simplest extensions of general relativity in the strong field regime. We study both the slowly and rapidly rotating cases. The results show that the I-Q relation remain nearly equation of state independent for fixed values of the normalized rotational parameter, but the deviations from universality can be a little bit larger compared to the general relativistic case. What is the most interesting in our studies, is that the differences with the pure Einstein's theory can be large reaching above 20%. This is qualitative different from the majority of alternative theories of gravity, where the normalized I-Q relations are almost indistinguishable from the general relativistic case, and can lead to observational constraints on the f (R) theories in the future.

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Search for $p \bar{p} \rightarrow WZ \rightarrow l\nu_l b \bar{b}$ signal with the CDF experiment at Tevatron

Cited by 6 publications

References 6 publications

Black holes as particle detectors: evolution of superradiant instabilities

Black holes as particle detectors: evolution of superradiant instabilities

Rapidly rotating neutron stars with a massive scalar field—structure and universal relations

I-Q relations for rapidly rotating neutron stars inf(R)gravity

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