arXiv subjects

Hideyoshi Arakida

Publications and source records attributed to Hideyoshi Arakida.

13 recordsLinked to original sources

arXiv2021

The optical geometry definition of the total deflection angle of a light ray in curved spacetime

Assuming a static and spherically symmetric spacetime, we propose a novel concept of the total deflection angle of a light ray. The concept is defined by the difference between the sum of internal angles of two triangles; one of the triangles lies on curved spacetime distorted by a gravitating body and the other on its background. The triangle required to define the total deflection angle can be realized by setting three laser-beam baselines as in planned space missions such as LATOR, ASTROD-GW, and LISA. Accordingly, the new total deflection angle is, in principle, measurable by gauging the internal angles of the triangles. The new definition of the total deflection angle can provide a geometrically and intuitively clear interpretation. Two formulas are proposed to calculate the total deflection angle on the basis of the Gauss--Bonnet theorem. It is shown that in the case of the Schwarzschild spacetime, the expression for the total deflection angle $α_{\rm Sch}$ reduces to Epstein--Shapiro's formula when the source of a light ray and the observer are located in an asymptotically flat region. Additionally, in the case of the Schwarzschild--de Sitter spacetime, the expression for the total deflection angle $α_{\rm SdS}$ comprises the Schwarzschild-like parts and coupling terms of the central mass $m$ and the cosmological constant $Λ$ in the form of ${\cal O}(Λm)$ instead of ${\cal O}(Λ/m)$. Furthermore, $α_{\rm SdS}$ does not include the terms characterized only by the cosmological constant $Λ$.

gr-qc↗

arXiv2021

General Relativistic Aberration Equation and Measurable Angle of Light Ray in Kerr Spacetime

We will mainly discuss the measurable angle (local angle) of the light ray $ψ_P$ at the position of the observer $P$ instead of the total deflection angle (global angle) $α$ in Kerr spacetime. We will investigate not only the effect of the gravito-magnetic field or frame dragging but also the contribution of the motion of the observer with a coordinate radial velocity $v^r$ and a coordinate transverse velocity $bv^ϕ$ ($b$ is the impact parameter and $v^ϕ$ is a coordinate angular velocity) which are converted from the components of the 4-velocity of the observer $u^r$ and $u^ϕ$, respectively. Because the motion of observer causes an aberration, we will employ the general relativistic aberration equation to obtain the measurable angle $ψ$. The measurable angle $ψ$ given in this paper can be applied not only to the case of the observer located in an asymptotically flat region but also to the case of the observer placed within the curved and finite-distance region. Moreover, when the observer is in radial motion, the total deflection angle $α_{\rm radial}$ can be expressed by $α_{\rm radial} = (1 + v^r)α_{\rm static}$ which is consistent with the overall scaling factor $1 - v$ with respect to the total deflection angle $α{\rm static}$ in the static case. instead of $1 - 2v$ where $v$ is the velocity of the lens object. On the other hand, when the observer is in transverse motion, the total deflection angle is given by the form $α_{\rm transverse} = (1 + bv^ϕ/2)α_{\rm static}$ if we define the transverse velocity as having the form $bv^ϕ$.

gr-qc↗

arXiv2018

General Relativistic Aberration Equation and Measurable Angle of Light Ray in Kerr--de Sitter Spacetime

As an extension of our previous paper, instead of the total deflection angle $α$, we will mainly focus on discussing the measurable angle of the light ray $ψ$ at the position of the observer in Kerr--de Sitter spacetime which includes the cosmological constant $Λ$. We will investigate the contributions of the radial and transverse motions of the observer which are connected with the radial velocity $v^r$ and transverse velocity $bv^ϕ$ ($b$ is the impact parameter) as well as the spin parameter $a$ of the central object which induces the gravitomagnetic field or frame dragging and the cosmological constant $Λ$. The general relativistic aberration equation is employed to take into account the influence of the motion of the observer on the measurable angle $ψ$. The measurable angle $ψ$ derived in this paper can be applied to the observer placed within the curved and finite-distance region in the spacetime. The equation of the light trajectory will be obtained in such a way that the background is de Sitter spacetime instead of Minkowski spacetime. If we assume that the lens object is the typical galaxy, the static terms ${\cal O}(Λbm, Λba)$ are basically comparable with the second order deflection term ${\cal O}(m^2)$, and they are almost one order smaller that of the Kerr deflection $-4ma/b^2$. The velocity-dependent terms ${\cal O}(Λbm v^r, Λbav^r)$ for radial motion and ${\cal O}(Λb^2mv^ϕ, Λb^2av^ϕ)$ for transverse motion are at most two orders of magnitude smaller than the second order deflection ${\cal O}(m^2)$. We also find that even when the radial and transverse velocities have the same sign, their asymptotic behavior as $ϕ$ approaches $0$ is differs, and each diverges to the opposite infinity.

gr-qc↗

arXiv2018

Light Deflection and Gauss-Bonnet Theorem: Definition of Total Deflection Angle and its Applications

In this paper, we re-examine the light deflection in the Schwarzschild and the Schwarzschild-de Sitter spacetime. First, supposing a static and spherically symmetric spacetime, we propose the definition of the total deflection angle $α$ of the light ray by constructing a quadrilateral $Σ^4$ on the optical reference geometry ${\cal M}^{\rm opt}$ determined by the optical metric $\bar{g}_{ij}$. On the basis of the definition of the total deflection angle $α$ and the Gauss-Bonnet theorem, we derive two formulas to calculate the total deflection angle $α$; (i) the angular formula that uses four angles determined on the optical reference geometry ${\cal M}^{\rm opt}$ or the curved $(r, ϕ)$ subspace ${\cal M}^{\rm sub}$ being a slice of constant time $t$ and (ii) the integral formula on the optical reference geometry ${\cal M}^{\rm opt}$ which is the areal integral of the Gaussian curvature $K$ in the area of a quadrilateral $Σ^4$ and the line integral of the geodesic curvature $κ_g$ along the curve $C_Γ$. As the curve $C_Γ$, we introduce the unperturbed reference line that is the null geodesic $Γ$ on the background spacetime such as the Minkowski or the de Sitter spacetime, and is obtained by projecting $Γ$ vertically onto the curved $(r, ϕ)$ subspace ${\cal M}^{\rm sub}$. We demonstrate that the two formulas give the same total deflection angle $α$ for the Schwarzschild and the Schwarzschild--de Sitter spacetime. In particular, in the Schwarzschild case, the result coincides with Epstein--Shapiro's formula when the source $S$ and the receiver $R$ of the light ray are located at infinity. In addition, in the Schwarzschild--de Sitter case, there appear order ${\cal O}(Λm)$ terms in addition to the Schwarzschild-like part, while order ${\cal O}(Λ)$ terms disappear.

gr-qc↗

arXiv2012

Note on the perihelion/periastron advance due to cosmological constant

We will comment on the perihelion/periastron advance of celestial bodies due to the cosmological constant $Λ$. It is well known that the cosmological constant $Λ$ causes the perihelion/periastron shift; however, there seems to still exist a discrepancy among the various derived precession formulae. We will point out that the expression $Δω_Λ = (πc^2 Λa^3/(GM))\sqrt{1 - e^2}$ is the general formula for any orbital eccentricity $e$ and the expression $Δω_Λ = (πc^2 Λa^3/(GM))(1 - e^2)^3$ comes from the nearly circular ($e \ll 1$) approximation.

gr-qc↗

arXiv2012

Effect of inhomogeneity of the Universe on a gravitationally bound local system: A no-go result for explaining the secular increase in the astronomical unit

We will investigate the influence of the inhomogeneity of the universe, especially that of the Lema{î}tre-Tolman-Bondi (LTB) model, on a gravitationally bound local system such as the solar system. We concentrate on the dynamical perturbation to the planetary motion and derive the leading order effect generated from the LTB model. It will be shown that there appear not only a well-known cosmological effect arisen from the homogeneous and isotropic model, such as the Robertson-Walker (RW) model, but also the additional terms due to the radial inhomogeneity of the LTB model. We will also apply the obtained results to the problem of secular increase in the astronomical unit, reported by Krasinsky and Brumberg (2004), and imply that the inhomogeneity of the universe cannot have a significant effect for explaining the observed $d{\rm AU}/dt = 15 \pm 4 ~{\rm [m/century]}$.

gr-qc↗

arXiv2012

Effect of the cosmological constant on the bending of light and the cosmological lens equation

We revisit the effect of cosmological constant $Λ$ on the light deflection and its role in the cosmological lens equation. First, we re-examine the motion of photon in the Schwarzschild spacetime, and explicitly describe the trajectory of photon and deflection angle $α$ up to the second-order in $G$. Then the discussion is extended to the contribution of the cosmological constant $Λ$ in the Schwarzschild-de Sitter or Kottler spacetime. Contrary to the previous arguments, we emphasize the following points: (a) the cosmological constant $Λ$ does appear in the orbital equation of light, (b) nevertheless the bending angle of light $α$ does not change its form even if $Λ\neq 0$ since the contribution of $Λ$ is thoroughly absorbed into the definition of the impact parameter, and (c) the effect of $Λ$ is completely involved in the angular diameter distance $D_A$.

gr-qc↗

arXiv2011

Application of Time Transfer Function to McVittie Spacetime: Gravitational Time Delay and Secular Increase in Astronomical Unit

We attempt to calculate the gravitational time delay in a time-dependent gravitational field, especially in McVittie spacetime, which can be considered as the spacetime around a gravitating body such as the Sun, embedded in the FLRW (Friedmann-Lemaître-Robertson-Walker) cosmological background metric. To this end, we adopt the time transfer function method proposed by Le Poncin-Lafitte {\it et al.} (Class. Quant. Grav. 21:4463, 2004) and Teyssandier and Le Poncin-Lafitte (Class. Quant. Grav. 25:145020, 2008), which is originally related to Synge's world function $Ω(x_A, x_B)$ and enables to circumvent the integration of the null geodesic equation. We re-examine the global cosmological effect on light propagation in the solar system. The round-trip time of a light ray/signal is given by the functions of not only the spacial coordinates but also the emission time or reception time of light ray/signal, which characterize the time-dependency of solutions. We also apply the obtained results to the secular increase in the astronomical unit, reported by Krasinsky and Brumberg (Celest. Mech. Dyn. Astron. 90:267, 2004), and we show that the leading order terms of the time-dependent component due to cosmological expansion is 9 orders of magnitude smaller than the observed value of $d{\rm AU}/dt$, i.e., $15 \pm 4$ ~[m/century]. Therefore, it is not possible to explain the secular increase in the astronomical unit in terms of cosmological expansion.

gr-qc↗

arXiv2010

Diffusive Propagation of High Energy Cosmic Rays in Galaxy: Effect of Hall Drift

We phenomenologically developed a propagation model of high energy galactic cosmic rays. We derived the analytical solutions by adopting the semi-empirical diffusion equation, proposed by Berezinskii {\it et al.}(1990) and the diffusion tensor proposed by Ptuskin {\it et al.}(1993). This model takes into account both the symmetric diffusion and the antisymmetric diffusion due to the particle Hall drift. Our solutions are an extension of the model developed by Ptuskin {\it et al.} (1993) to a two-dimensional two-layer (galactic disk and halo) model, and they coincide completely with the solution derived by Berezinskii {\it et al.} (1990) in the absence of antisymmetric diffusion due to Hall drift. We showed that this relatively simple toy model can be used to explain the variation in the exponent of the cosmic ray energy spectrum, $γ$, around the knee $E \approx 10^{15}$ eV.

astro-ph.HE↗

arXiv2009

Influence of Dark Matter on Light Propagation in Solar System

We investigated the influence of dark matter on light propagation in the solar system. We assumed the spherical symmetry of spacetime and derived the approximate solution of the Einstein equation, which consists of the gravitational attractions caused by the central celestial body, i.e. the Sun, and the dark matter surrounding it. We expressed the dark matter density in the solar system in the following simple power-law form, $\varrho(t, r) = ρ(t)(\ell/r)^k$, where $t$ is the coordinate time; $r$, the radius from the central body; $\ell$, the normalizing factor; $k$, the exponent characterizing $r$-dependence of dark matter density; and $ρ(t)$, the arbitrary function of time $t$. On the basis of the derived approximate solution, we focused on light propagation and obtained the additional corrections of the gravitational time delay and the relative frequency shift caused by the dark matter. As an application of our results, we considered the secular increase in the astronomical unit reported by Krasinsky and Brumberg (2004) and found that it was difficult to provide an explanation for the observed $d{\rm AU}/dt = 15 \pm 4 ~[{\rm m/century}]$.

astro-ph↗

arXiv2009

Secular increase of the Astronomical Unit: a possible explanation in terms of the total angular momentum conservation law

We give an idea and the order-of-magnitude estimations to explain the recently reported secular increase of the Astronomical Unit (AU) by Krasinsky and Brumberg (2004). The idea proposed is analogous to the tidal acceleration in the Earth-Moon system, which is based on the conservation of the total angular momentum and we apply this scenario to the Sun-planets system. Assuming the existence of some tidal interactions that transfer the rotational angular momentum of the Sun and using reported value of the positive secular trend in the astronomical unit, $\frac{d}{dt}{AU} = 15 \pm 4 {(m/cy)}$, the suggested change in the period of rotation of the Sun is about $21 {ms/cy}$ in the case that the orbits of the eight planets have the same "expansion rate." This value is sufficiently small, and at present it seems there are no observational data which exclude this possibility. Effects of the change in the Sun's moment of inertia is also investigated. It is pointed out that the change in the moment of inertia due to the radiative mass loss by the Sun may be responsible for the secular increase of AU, if the orbital "expansion" is happening only in the inner planets system. Although the existence of some tidal interactions is assumed between the Sun and planets, concrete mechanisms of the angular momentum transfer are not discussed in this paper, which remain to be done as future investigations.

astro-ph.EP↗

arXiv2008

Time Delay in Robertson-McVittie Spacetime and its Application to Increase of Astronomical Unit

We investigated the light propagation by means of the Robertson-McVittie solution which is considered to be the spacetime around the gravitating body embedded in the FLRW (Friedmann-Lema{î}tre-Robertson-Walker) background metric. We concentrated on the time delay and derived the correction terms with respect to the Shapiro's formula. To relate with the actual observation and its reduction process, we also took account of the time transformations; coordinate time to proper one, and conversely, proper time to coordinate one. We applied these results to the problem of increase of astronomical unit reported by Krasinsky and Brumberg (2004). However, we found the influence of the cosmological expansion on the light propagation does not give an explanation of observed value, $d{\rm AU}/dt = 15 \pm 4$ [m/century] in the framework of Robertson-McVittie metric.

gr-qc↗

arXiv2008

Quasi-Hilda Comet 147P/Kushida-Muramatsu: Another long temporary satellite capture by Jupiter

The quasi-Hilda comets (QHCs), being in unstable 3:2 Jovian mean motion resonance, are considered a major cause of temporary satellite capture (TSC) by Jupiter. Though the QHCs may be escaped Hilda asteroids, their origin and nature have not yet been studied in sufficient detail. Of particular interest are long TSCs/orbiters. Orbiters -- in which at least one full revolution about the planet is completed -- are rare astronomical events; only four have been known to occur in the last several decades. Every case has been associated with a QHC: 82P/Gehrels 3; 111P/Helin-Roman-Crockett; P/1996 R2 (Lagerkvist); and the possibly QHC-derived D/1993 F2 (Shoemaker-Levy 9, SL9). We focus on long TSC/orbiter events involving QHCs and Jupiter. Thus we survey the known QHCs, searching for further long TSCs/orbiters over the past century. First, we confirmed the long TSC/orbiter events of 82P, 111P, and 1996 R2 in order to test our method against previous work, applying a general N-body Newtonian code. We then used the same procedure to survey the remaining known QHCs and search for long TSC/orbiter events. We newly identified another long TSC/orbiter: 147P/Kushida-Muramatsu from 1949 May 14 (+97days/-106 days)--1961 July 15. Our result is verified by integrations of 243 cloned orbits which take account of the present orbital uncertainty of this comet. This is the third long TSC and the fifth orbiter to be found, thus long TSC/orbiter events involving Jupiter have occurred once per decade. Two full revolutions about Jupiter were completed and the capture duration was 12.17 (+0.29/-0.27) years; both these numbers rank 147P as third among long TSC/orbiter events, behind SL9 and 111P. This study also confirms the importance of the QHC region as a dynamical route into and out of Jovian TSC, via the Hill's sphere.

astro-ph↗