Quantum Interference Effects in Spacetime of Slowly Rotating Compact Objects in Braneworld

Mamadjanov, A.I.; Hakimov, Abdullo; Tojiev, S.R.

doi:10.1142/s0217732310032482

Cited by 11 publications

(9 citation statements)

References 24 publications

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“…(1) allows for detectable effects on our (3+1)-brane that can be used in constraining the properties of the bulk. For upper limits on the brane parameter of other braneworld models, see, e.g., [12,13]. Several large-scale tests of the RS model [5] have been proposed so far in astrophysical scenarios; they claimed bounds on ℓ at ∼ 1 − 10 µm level, which is the same order of magnitude reached in laboratory-scale experiments [14,15].…”

Section: Introductionmentioning

confidence: 94%

Model‐independent constraints on r^‐3 extra‐interactions from orbital motions

Iorio

2012

Annalen der Physik

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Constraints on long-range power-law modifications Upert ∝ r −3 of the usual Newtonian gravitational potential UN ∝ r −1 are inferred from orbital motions of well known artificial and natural bodies. They can be interpreted in terms of a characteristic length ℓ which may be identified with, e.g., the anti-de Sitter (AdS) radius of curvature ℓ in the Randall-Sundrum (RS) braneworld model, although this not a mandatory choice. Our bounds, complementary to those from tabletop laboratory experiments, do not rely upon more or less speculative and untested theoretical assumptions, contrary to other long-range RS tests proposed in astrophysical scenarios in which many of the phenomena adopted may depend on the system's composition, formation and dynamical history as well. Independently of the interpretation of ℓ, the perihelion precession of Mercury and its radiotechnical ranging from the Earth yield ℓ 10 − 50 km. Tighter bounds come from the perigee precession of the Moon, from which it can be inferred ℓ 500 − 700 m. The best constraints (ℓ 5 m) come from the Satellite-to-Satellite Tracking (SST) range of the GRACE A/B spacecrafts orbiting the Earth: proposed follow-on of such a mission, implying a sub-nm s −1 range-rate accuracy, may constrain ℓ at ∼ 10 cm level. Weaker constraints come from the double pulsar system (ℓ 80 − 100 km) and from the main sequence star S2 orbiting the compact object in Sgr A * (ℓ 6.2 − 8.8 AU). Such bounds on the length ℓ, which must not necessarily be identified with the AdS radius of curvature of the RS model, naturally translate into constraints on an, e.g., universal coupling parameter K of the r −3 interaction. GRACE yields K ≤ 1 × 10 16 m 5 s −2 .

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Section: Introductionmentioning

confidence: 94%

Model‐independent constraints on r^‐3 extra‐interactions from orbital motions

Iorio

2012

Annalen der Physik

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“…The black hole spacetimes are determined by geometry of the spherical Reissner-Nordström (RN) and axial Kerr-Newman (KN) type where the electric charge squared is substituted by the braneworld "tidal charge" parameter representing the tidal (Weyl tensor) effects of the bulk space onto the 4D black hole structure. Astrophysically relevant properties of the braneworld black holes were studied in a series of papers devoted to both motion of matter in their vicinity [8][9][10][11][12] and optical phenomena [13][14][15][16].…”

Section: Introductionmentioning

confidence: 99%

Photon and neutrino redshift in the field of braneworld compact stars

Hladik,

Stuchlik

2011

Preprint

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We study gravitational redshift of photons and neutrinos radiated by the braneworld neutron or quark stars that are considered in the framework of the simple model of the internal spacetime with uniform distribution of energy density, and the external spacetime described by the Reissner-Nordström geometry characterized by the braneworld "tidal" charge b. For negative tidal charges, the external spacetime is of the black-hole type, while for positive tidal charges, the external spacetime can be of both black-hole and naked-singularity type. We consider also extremely compact stars allowing existence of trapped null geodesics in their interior. We assume radiation of photons from the surface at radius R, neutrinos from the whole compact star interior, and their motion along radial null geodesics of the spacetime. In dependency on the compact stars parameters b and R, the photon surface redshift is related to the range of the neutrino internal redshift and the signatures of the tidal charge and possible existence of extremely compact stars are discussed. When both surface (photon) and internal (neutrino) redshift are given by observations, both compact star parameters R and b can be determined in the framework of our simple model.

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“…The black hole spacetimes are determined by geometry of the spherical Reissner-Nordström (R-N) and axial Kerr-Newman (K-N) type where the electric charge squared is substituted by the braneworld "tidal charge" parameter representing the tidal (Weyl tensor) effects of the bulk space onto the 4D black hole structure. Astrophysically relevant properties of the braneworld black holes were studied in a series of papers devoted to both motion of matter in their vicinity [42,6,1,26,29] and optical phenomena [34,33,12,11].…”

Section: Introductionmentioning

confidence: 99%

Neutrino trapping in braneworld extremely compact stars

2011

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Extremely Compact Stars (ECS) contain trapped null geodesics. When such objects enter the evolution period admitting geodetical motion of neutrinos, certain part of neutrinos produced in their interior will be trapped influencing their neutrino luminosity and thermal evolution. We study neutrino trapping in the braneworld ECS, assuming uniform distribution of neutrino emissivity and massless neutrinos. We give the efficiency of the neutrino trapping effects in the framework of the simple model of the internal spacetime with uniform distribution of energy density, and external spacetime described by the Reissner-Nordstr\"om geometry characterized by the braneworld "tidal" parameter $b$. For $b < 0$ the external spacetime is of the black-hole type, while for $b > 0$ the external spacetime can be of both black-hole and naked-singularity type. Then the ECS surface radius $R$ can be located also above the unstable (outer) photon circular orbit. Such basically new types of the spacetimes strongly alter the trapping phenomena as compared to the standard case of $b = 0$. It is shown that the neutrino trapping effects are slightly lowered by the presence of physically more plausible case of $b < 0$, as compared to the standard internal Schwarzschild spacetime, while they can be magnified by positive tidal charges if $b < 1$ and lowered for $b > 1$. However, potential astrophysical relevance of the trapping phenomena is strongly enhanced for negative tidal charges enabling a significant enlargement of the ECS surface radius to values coherent with recent observations

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Quantum Interference Effects in Spacetime of Slowly Rotating Compact Objects in Braneworld

Cited by 11 publications

References 24 publications

Model‐independent constraints on r^‐3 extra‐interactions from orbital motions

Model‐independent constraints on r^‐3 extra‐interactions from orbital motions

Photon and neutrino redshift in the field of braneworld compact stars

Neutrino trapping in braneworld extremely compact stars

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Quantum Interference Effects in Spacetime of Slowly Rotating Compact Objects in Braneworld

Cited by 11 publications

References 24 publications

Model‐independent constraints on r‐3 extra‐interactions from orbital motions

Model‐independent constraints on r‐3 extra‐interactions from orbital motions

Photon and neutrino redshift in the field of braneworld compact stars

Neutrino trapping in braneworld extremely compact stars

Contact Info

Product

Resources

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Model‐independent constraints on r^‐3 extra‐interactions from orbital motions

Model‐independent constraints on r^‐3 extra‐interactions from orbital motions