Temperature Influence on Divergence Angles of Quartz Crystal Wollaston Prism

Zhao, Shuang; Fu-quan, WU; Zhang, Dongsheng; Zhao, Xin; Jin-Xi, Wang; Xue, Mei; Wei-gang, Zhong

doi:10.1088/0256-307x/25/7/038

Cited by 2 publications

(3 citation statements)

References 7 publications

(1 reference statement)

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“…The fluid can be considered such that the state parameter ω is ratio of fluid pressure p to its density ρ, that is ω = p/ρ. The different models for dark energy have been proposed among: quintessence [5,6], phantom dark energy [7,8], quintom [9,10], K-essence [11] and others. The difference of these models for dark energy is the value of parameter ω q .…”

Section: Introductionmentioning

confidence: 99%

Distinguishing a rotating Kiselev black hole from a naked singularity using the spin precession of a test gyroscope

2018

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We study the critical values of the quintessential and spin parameters, to distinguish a rotating Kiselev black hole (RKBH) from a naked singularity. For any value of the dimensionless quintessential parameter ω q ∈ (−1, −1/3), when increasing the value of quintessential parameter α, the size of the event horizon increases, whereas the size of the outer horizon decreases. We then study the spin precession of a test gyroscope attached to a stationary observer in this spacetime. Using the spin precessions we differentiate black holes from naked singularities. If the precession frequency becomes large, as approaching to the central object in the quintessential field along any direction, then the spacetime is a black hole. A spacetime will contain a naked singularity if the precession frequency remains finite everywhere except at the singularity itself. Finally, we study the Lense-Thirring precession frequency for rotating Kiseleb black hole and the geodetic precession for Kiselev black hole.2 of general relativity and to measure the precession rate due to the LT and geodetic effects relative to the Copernican system or the fixed star HR8703, known as IM Pegasi, of a test gyro due to the rotation of the Earth, Gravity Probe B has been launched [29].The geodetic precession in the Schwarzschild black hole and the KBH have been studied in [31][32][33]. The LT-precession in the strong gravitational field of the Kerr and Kerr-Taub-NUT black holes has been discussed in [34].During the gravitational collapse of massive stars, the existence of naked singularities is the topic of great interest for researchers in the field of gravitational theory and relativistic astrophysics. The key question is that how one can differentiate whether the ultimate product in the life cycle of the compact object under the self-gravity collapse is naked singularity or black hole? Mathematically, a black hole is solution of the Einstein field equations (EFE). A stationary vacuum Kerr solution of EFE is characterized by two parameters, namely the mass M and angular momentum J of the central object. If the spin parameter a (angular momentum per unit mass) satisfies the condition M ≥ a, Kerr solution represent black hole and the Kerr singularity is contained in the event horizon. However, if M < a the event horizon disappears, represents the naked singularity. Recently, Chakraborty et al [35,36] gave the criteria based on the spin precession frequency of a test gyroscope attached to both static and stationary observers, to differentiate black holes from naked singularities. Using these criteria the Kerr black hole and naked singularities are discussed.The novelty of the present paper is to differentiate rotating black holes in a quintessential matter (rotating KBH) from a naked singularity. A stationary rotating Kiselev solution of Einstein field equation is characterized by four parameter, black hole mass M, spin parameter a, dimensionless quintessential parameter ω q and quintessential parameter representing the intensity of the quintessence ener...

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Section: Introductionmentioning

confidence: 99%

Distinguishing a rotating Kiselev black hole from a naked singularity using the spin precession of a test gyroscope

2018

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“…We now study the Dirac Eqs. (9)(10)(11)(12) in the background of metric (3). To solve the Dirac equations, we will consider the corresponding Compton wave of the Dirac particle as in the form of…”

Section: Dirac Equation In Bbhsqmentioning

confidence: 99%

“…In addition, the scalar fields are also hypothetical forms of dark energy where a broad types of scalar field models have been suggested such as quintessence [8][9][10][11][12][13][14][15], phantom models [16][17][18][19][20], K-essence [21,22], quintom [23,24], and so on. Ultimately, the difference between these models is due to the magnitude of w q and for quintessence −1 ≤ w q ≤ − 1 3 .…”

Section: Introductionmentioning

confidence: 99%

Solution of Dirac equation and greybody radiation around a regular Bardeen black hole surrounded by quintessence

2020

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The exact solutions of the Dirac equation that describe a massive, non-charged particle with spin− 1 2 in the curved spacetime geometry of regular Bardeen black hole surrounded by quintessence (BBHSQ) are investigated. We first derive the Dirac equation in the BBHSQ background using a null tetrad in the Newman-Penrose formalism. Afterward, we separate the Dirac equation into ordinary differential equations for the radial and angular parts. The angular equations are solved exactly in terms of standard spherical harmonics. The radial part equations are transformed into a Schrödinger like differential wave equations with effective potentials. The effect of the quintessence on the regular Bardeen black hole is studied by understanding the physical behavior of the effective potentials. In addition, the potentials are plotted with changing the quintessence parameters, magnetic monopole charge parameter and the frequency of the particle in the physically acceptable regions. Finally, we study the greybody radiation of spin−0 particles from the BBHSQ.2

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Temperature Influence on Divergence Angles of Quartz Crystal Wollaston Prism

Cited by 2 publications

References 7 publications

Distinguishing a rotating Kiselev black hole from a naked singularity using the spin precession of a test gyroscope

Distinguishing a rotating Kiselev black hole from a naked singularity using the spin precession of a test gyroscope

Solution of Dirac equation and greybody radiation around a regular Bardeen black hole surrounded by quintessence

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