-
1
-
-
84874186273
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-
S. M. Kopeikin, G. Schäfer, C. R. Gwinn, and T. M. Eubanks, Phys. Rev. D 59, 084023 (1999).
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(1999)
Phys. Rev. D
, vol.59
, pp. 84023
-
-
Kopeikin, S.M.1
Schäfer, G.2
Gwinn, C.R.3
Eubanks, T.M.4
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3
-
-
85037209146
-
-
D. Peterson and M. Shao, in Proceedings of the ESA Symposium “HIPPARCOS, Venice 97,” edited by B. Battrick (ESA, Noordwijk, The Netherlands, 1997), p. 789
-
D. Peterson and M. Shao, in Proceedings of the ESA Symposium “HIPPARCOS, Venice 97,” edited by B. Battrick (ESA, Noordwijk, The Netherlands, 1997), p. 789.
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-
-
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4
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0000355788
-
-
the idea of the method used by Klioner and Kopeikin was put forward in Ref
-
S. A. Klioner and S. M. Kopeikin, Astron. J. 104, 897 (1992);the idea of the method used by Klioner and Kopeikin was put forward in Ref. 127.
-
(1992)
Astron. J.
, vol.104
, pp. 897
-
-
Klioner, S.A.1
Kopeikin, S.M.2
-
8
-
-
85037189298
-
-
V. A. Brumberg, Essential Relativistic Celestial Mechanics, (Adam Hilger, Bristol, 1991)
-
V. A. Brumberg, Essential Relativistic Celestial Mechanics, (Adam Hilger, Bristol, 1991).
-
-
-
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11
-
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0012916467
-
-
see also O. J. Sovers and J. L. Fanselow, Observation Model and Parameter Partials for the JPL VLBI Parameter Estimation Software “Masterfit,” JPL Report No. 83-89, 1987, Rev. 3, and Ref
-
Astron. J.R. W. Hellings92, 1446 (1986);see also O. J. Sovers and J. L. Fanselow, Observation Model and Parameter Partials for the JPL VLBI Parameter Estimation Software “Masterfit,” JPL Report No. 83-89, 1987, Rev. 3, and Ref. 123, discussion on pages 1406–7 after formula (3.23).
-
(1986)
Astron. J.
, vol.92
, pp. 1446
-
-
Hellings, R.W.1
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13
-
-
85037192528
-
-
what follows we shall often use geometrical units, e.g., see Ref
-
In what follows we shall often use geometrical units, e.g., see Ref. 5 in which (Formula presented)
-
-
-
-
14
-
-
85037237868
-
-
The difference between the parameters (Formula presented) and (Formula presented) includes terms of the post-Newtonian order of magnitude. In the weak-field limit the numerical value of (Formula presented) coincides with that of (Formula presented) which is one of the parameters of the standard parametrized post-Newtonian (PPN) formalism
-
The difference between the parameters (Formula presented) and (Formula presented) includes terms of the post-Newtonian order of magnitude. In the weak-field limit the numerical value of (Formula presented) coincides with that of (Formula presented) which is one of the parameters of the standard parametrized post-Newtonian (PPN) formalism 9. For more details see Refs. 1415, and references therein.
-
-
-
-
19
-
-
85037225858
-
-
Space-time indices (Formula presented) etc., run from 0 to 3 and are raised and lowered by means of (Formula presented) Spatial indices (Formula presented) etc., run from 1 to 3 and are raised and lowered by means of the Kronecker symbol (Formula presented) so that, actually, the upper and lower case spatial indices are not distinguished. Repeated greek and latin indices preassume summation from 0 to 3 and from 1 to 3, respectively
-
Space-time indices (Formula presented) etc., run from 0 to 3 and are raised and lowered by means of (Formula presented) Spatial indices (Formula presented) etc., run from 1 to 3 and are raised and lowered by means of the Kronecker symbol (Formula presented) so that, actually, the upper and lower case spatial indices are not distinguished. Repeated greek and latin indices preassume summation from 0 to 3 and from 1 to 3, respectively.
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-
-
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20
-
-
85037245080
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The harmonic gauge
-
The harmonic gauge 6 is fixed in the first post-Minkowskian approximation by the four differential conditions (Formula presented)where the comma denotes a partial derivative with respect to a corresponding coordinate.
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-
-
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23
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85037256230
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We take only the retarded Green function and abandoned the advanced one as we assume that the N-body system under consideration is absolutely isolated from possible external gravitational enviroment. It is equivalent to the assumption that there is no gravitational radiation impinging onto the system in the first post-Minkowskian approximation. It is interesting to emphasize that in higher post-Minkowskian approximations existence of the tail gravitational radiation effects
-
We take only the retarded Green function and abandoned the advanced one as we assume that the N-body system under consideration is absolutely isolated from possible external gravitational enviroment. It is equivalent to the assumption that there is no gravitational radiation impinging onto the system in the first post-Minkowskian approximation. It is interesting to emphasize that in higher post-Minkowskian approximations existence of the tail gravitational radiation effects 232425 brings about a small fraction of incoming radiation as being back scattered on the static part of the curvature generated by the monopole component in multipole expansion of the metric tensor. However, although the back scattered radiation is incoming, it does not come in from past null infinity (“scri minus”). Therefore, it has nothing to do with advanced Green function. Its again purely outgoing radiation at future null infinity (“scri plus”). We omit such back scatter terms in what follows for they appear only in the higher orders of the post-Minkowskian approximation scheme.
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27
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85037202122
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It is more appropriate to denote the retarded time for the ath body as (Formula presented) which would have reflected the dependence of the retarded time on the number of the body. However, it would make notations and the presentation of subsequent formulas more cumbersome. For this reason we use s instead of (Formula presented) keeping in mind that if it is not stated otherwise, coordinates, velocity, and acceleration of the ath body are taken at the corresponding retarded time (Formula presented) This remark is crucial, e.g., in the discussion regarding the definition of the center of mass of the N body system [for more details see the explanations after Eq. (151)]
-
It is more appropriate to denote the retarded time for the ath body as (Formula presented) which would have reflected the dependence of the retarded time on the number of the body. However, it would make notations and the presentation of subsequent formulas more cumbersome. For this reason we use s instead of (Formula presented) keeping in mind that if it is not stated otherwise, coordinates, velocity, and acceleration of the ath body are taken at the corresponding retarded time (Formula presented) This remark is crucial, e.g., in the discussion regarding the definition of the center of mass of the N body system [for more details see the explanations after Eq. (151)].
-
-
-
-
28
-
-
85037200398
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addition, we emphasize that the condition of weak-field approximation, that is (Formula presented), leads to general restriction on the velocity of a moving body (Formula presented) In the particular case, where the velocity (Formula presented) of the ath body is almost parallel to (Formula presented) one gets the stronger restriction (Formula presented) (Refs
-
In addition, we emphasize that the condition of weak-field approximation, that is (Formula presented), leads to general restriction on the velocity of a moving body (Formula presented) In the particular case, where the velocity (Formula presented) of the ath body is almost parallel to (Formula presented) one gets the stronger restriction (Formula presented) (Refs. 282930).
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35
-
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85037220922
-
-
It is worth noting that this statement is true only if the origin of the coordinate system is in between the source of light and observer. Under other circumstances the variable (Formula presented) may be always either positive or negative
-
It is worth noting that this statement is true only if the origin of the coordinate system is in between the source of light and observer. Under other circumstances the variable (Formula presented) may be always either positive or negative.
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36
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85037246419
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At the given stage of our study we do not fix the freedom in choosing the origin of the coordinate system by assuming, for example, that the origin coincides with the center of mass of the N-body system. Specific choices of the origin will be done later on
-
At the given stage of our study we do not fix the freedom in choosing the origin of the coordinate system by assuming, for example, that the origin coincides with the center of mass of the N-body system. Specific choices of the origin will be done later on.
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37
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85037209193
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The principal differential identity used for derivation of Eq. (19) and applied to any smooth function (Formula presented) reads (Formula presented)and allows us to change the order of operations of partial differentiation and substitution for the unperturbed light ray trajectory in the equation for light geodesics
-
The principal differential identity used for derivation of Eq. (19) and applied to any smooth function (Formula presented) reads (Formula presented)and allows us to change the order of operations of partial differentiation and substitution for the unperturbed light ray trajectory in the equation for light geodesics 1.
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38
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85037196696
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More precisely, this kind of equation is known in the literature as a “retarded-functional differential system” because of the dependence of gravitational potentials on the retarded time argument. Such an equation belongs to the framework of “predictive relativistic mechanics”
-
More precisely, this kind of equation is known in the literature as a “retarded-functional differential system” because of the dependence of gravitational potentials on the retarded time argument. Such an equation belongs to the framework of “predictive relativistic mechanics” 38394041424344.
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44
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0001081566
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L. Bel, T. Damour, N. Deruelle, J. Ibañez, and J. Martin, Gen. Relativ. Gravit. 13, 963 (1981).
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(1981)
Gen. Relativ. Gravit.
, vol.13
, pp. 963
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Bel, L.1
Damour, T.2
Deruelle, N.3
Ibañez, J.4
Martin, J.5
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45
-
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84933791236
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-
North-Holland, Amsterdam, N. Deruelle, T. Piran
-
T. Damour, in Gravitational Radiation, Les Houches 1982, edited by N. Deruelle and T. Piran (North-Holland, Amsterdam, 1983).
-
(1983)
Gravitational Radiation, Les Houches 1982
-
-
Damour, T.1
-
46
-
-
85037181012
-
-
We again emphasize that the new parameter (Formula presented) depends on the index of each body. For this reason it would be better to denote it as (Formula presented) We do not use this notation to avoid the appearance of a large number of subindices
-
We again emphasize that the new parameter (Formula presented) depends on the index of each body. For this reason it would be better to denote it as (Formula presented) We do not use this notation to avoid the appearance of a large number of subindices.
-
-
-
-
47
-
-
85037244025
-
-
Calculation of the derivative (Formula presented) at the point of light emission is obtained from the formula (30) where all quantities involved are to be taken at the retarded time (Formula presented)
-
Calculation of the derivative (Formula presented) at the point of light emission is obtained from the formula (30) where all quantities involved are to be taken at the retarded time (Formula presented)
-
-
-
-
48
-
-
85037192766
-
-
We emphasize that our formalism admits to work with world lines of arbitrary moving bodies without restricting them to straight lines only. More precisely, in the harmonic gauge (see Ref
-
We emphasize that our formalism admits to work with world lines of arbitrary moving bodies without restricting them to straight lines only. More precisely, in the harmonic gauge (see Ref. 19) the equations of motion of the bodies result from the harmonic coordinate conditions 19. In the first post-Minkowskian approximation these conditions allow motion of bodies only along straight lines with constant speeds. However, if in finding the metric tensor the nonlinear terms in the Einstein equations are taken into account, the bodies may show accelerated motion without structurally changing the linearized form of the Liénard-Wiechert solution for the metric tensor which is used for integration of equations of motion of a photon.
-
-
-
-
52
-
-
84914783674
-
-
S. W. Hawking, W. Israel
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T. Damour, in 300 Years of Gravitation, edited by S. W. Hawking and W. Israel (Cambridge University Press, Cambridge, 1987), p. 128.
-
(1987)
300 Years of Gravitation
, pp. 128
-
-
Damour, T.1
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54
-
-
85037242115
-
-
Again it would be better to denote the retarded time as (Formula presented) emphasizing its dependence on the number index of the body under consideration. We keep in mind this remark but do not use such a notation to avoid confusing mixture of indices
-
Again it would be better to denote the retarded time as (Formula presented) emphasizing its dependence on the number index of the body under consideration. We keep in mind this remark but do not use such a notation to avoid confusing mixture of indices.
-
-
-
-
56
-
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85037211496
-
-
S. A. Klioner, Preprint of the Institute of Applied Astronomy No. 6, Leningrad (in Russian).
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-
-
Klioner, S.A.1
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57
-
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85037190402
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N. Wex, Ph.D. thesis, TPI, FSU of Jena, Germany, 1995
-
N. Wex, Ph.D. thesis, TPI, FSU of Jena, Germany, 1995.
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-
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58
-
-
85037237466
-
-
The case of an observer moving with respect to the harmonic coordinate system with velocity (Formula presented) may be considered after completing the additional Lorentz transformation described by the matrix (Formula presented) with components [e.g., see Ref
-
The case of an observer moving with respect to the harmonic coordinate system with velocity (Formula presented) may be considered after completing the additional Lorentz transformation described by the matrix (Formula presented) with components [e.g., see Ref. 5, formula (2.44)] (Formula presented)(Formula presented)where (Formula presented), and (Formula presented) is the unit vector in the direction of motion of the observer.
-
-
-
-
59
-
-
85037198927
-
-
Note that in the relativistic terms of any formula of the present paper we are allowed to use the substitution (Formula presented)
-
Note that in the relativistic terms of any formula of the present paper we are allowed to use the substitution (Formula presented)
-
-
-
-
61
-
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85037219581
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-
W. Cochran, in Proceedings of the Workshop of High Resolution Data Processing, edited by M. Iye, T. Takata, and J. Wampler, SUBARU Telescope Technical Report, 1996, NAOJ, No 55, p. 30
-
W. Cochran, in Proceedings of the Workshop of High Resolution Data Processing, edited by M. Iye, T. Takata, and J. Wampler, SUBARU Telescope Technical Report, 1996, NAOJ, No 55, p. 30.
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-
-
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64
-
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85037246851
-
-
V. A. Brumberg, Relativistic Celestial Mechanics (Nauka, Moskow, 1972) (in Russian)
-
V. A. Brumberg, Relativistic Celestial Mechanics (Nauka, Moskow, 1972) (in Russian).
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-
-
-
65
-
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85037181599
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-
Synge calls the relationship (78) the Doppler effect in terms of frequency (see Ref
-
Synge calls the relationship (78) the Doppler effect in terms of frequency (see Ref. 62, p. 122). It is fully consistent with definition of the Doppler shift in terms of energy (see Ref. 62, p. 231) when one compares the energy of photon at the points of emission and observation of light. The Doppler shift in terms of energy is given by (Formula presented)where (Formula presented) (Formula presented) and (Formula presented) (Formula presented) are the four-velocities of source of light and observer and the four-momenta of photon at the points of emission and observation respectively. It is quite easy to see that both mentioned formulations of the Doppler shift effect are equivalent. Indeed, taking into account that (Formula presented) and (Formula presented), where (Formula presented) is the phase of the electromagnetic wave, we obtain (Formula presented) Thus, (Formula presented)The phase of electromagnetic wave remains constant along the light ray trajectory. For this reason, (Formula presented), and Eq. (78) holds.
-
-
-
-
66
-
-
85037216111
-
-
Taking times (Formula presented) and (Formula presented) as primary quantities instead of t and (Formula presented) brings in the retarded times s and (Formula presented) dependence on the time of the closest approach (Formula presented), that is either (Formula presented) (Formula presented) or (Formula presented) (Formula presented) It introduces partial derivatives of s and (Formula presented) with respect to (Formula presented) and modifies formula (81) as well
-
Taking times (Formula presented) and (Formula presented) as primary quantities instead of t and (Formula presented) brings in the retarded times s and (Formula presented) dependence on the time of the closest approach (Formula presented), that is either (Formula presented) (Formula presented) or (Formula presented) (Formula presented) It introduces partial derivatives of s and (Formula presented) with respect to (Formula presented) and modifies formula (81) as well.
-
-
-
-
67
-
-
85037185695
-
-
If one uses times (Formula presented) and (Formula presented) as time variables the equalities (83) assume the form (Formula presented)(Formula presented)from which and Eq. (83) it follows that (Formula presented)
-
If one uses times (Formula presented) and (Formula presented) as time variables the equalities (83) assume the form (Formula presented)(Formula presented)from which and Eq. (83) it follows that (Formula presented)
-
-
-
-
68
-
-
85037221143
-
-
This statement may not be valid in the case of Doppler tracking observations of spacecrafts in the solar system
-
This statement may not be valid in the case of Doppler tracking observations of spacecrafts in the solar system.
-
-
-
-
74
-
-
4243278868
-
-
T. Damour and J. H. Taylor, Phys. Rev. D, 45, 1840 (1992). Strictly speaking, some of the PK parameters depend, actually, on four unknown quantities—masses of pulsar and its companion and two angles of orientation of the pulsar’s angular velocity of proper rotation. However, the PK parameters presently measured in most binary pulsar systems depend on masses of the stars only.
-
(1992)
Phys. Rev. D
, vol.45
, pp. 1840
-
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Damour, T.1
Taylor, J.H.2
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76
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22444453376
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I. H. Stairs, Z. Arzoumanian, F. Camilo, A. G. Lyne, D. J. Nice, J. H. Taylor, S. E. Thorsett, and A. Wolszczan, Astrophys. J. 505, 352 (1998).
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(1998)
Astrophys. J.
, vol.505
, pp. 352
-
-
Stairs, I.H.1
Arzoumanian, Z.2
Camilo, F.3
Lyne, A.G.4
Nice, D.J.5
Taylor, J.H.6
Thorsett, S.E.7
Wolszczan, A.8
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79
-
-
85037188023
-
-
More precisely, the coordinates of the point of emission are constant in the pulsar proper reference frame. The relativistic transformation from the proper reference frame of the pulsar to the binary pulsar barycentric coordinate system
-
More precisely, the coordinates of the point of emission are constant in the pulsar proper reference frame. The relativistic transformation from the proper reference frame of the pulsar to the binary pulsar barycentric coordinate system 7980 reveals that if the pulsar moves along the elliptic orbit the barycentric vector (Formula presented) actually depends on time. However, this periodic relativistic perturbation of the vector is of order (Formula presented) where (Formula presented) is a characteristic velocity of the pulsar with respect to the barycenter of the binary system. For a typical distance (Formula presented) km this is too small to measure. Another reason for the time dependence of the barycentric vector (Formula presented) on time arises due to the effects of aberration 81, the orbital pulsar parallax 82, and the bending delay 83. These effects are also small and can be neglected in the formula for the Shapiro time delay.
-
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-
-
85
-
-
85037244185
-
-
Compare, for instance, with formula (3) in Ref
-
Compare, for instance, with formula (3) in Ref. 85.
-
-
-
-
87
-
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85037232234
-
-
Let us note once again that the post-Newtonian scheme can be applied without restriction only if the length of the light ray trajectory is small compared with the size of the gravitating system. This situation is realized in the observations of the solar system objects. We analyze this case in Sec. VII C (see also Fig. 33) in more detail
-
Let us note once again that the post-Newtonian scheme can be applied without restriction only if the length of the light ray trajectory is small compared with the size of the gravitating system. This situation is realized in the observations of the solar system objects. We analyze this case in Sec. VII C (see also Fig. 33) in more detail.
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88
-
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85037218680
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-
For comparison with other phenomenological timing models worked out by other researchers see, e.g., Ref
-
For comparison with other phenomenological timing models worked out by other researchers see, e.g., Ref. 88.
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91
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85037227846
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-
To be more precise, the post-Newtonian scheme may give inconsistent results for light propagation in those terms which are proportional to the product of mass of the light-deflecting body and square of its velocity, that is, (Formula presented) At the same time the post-Minkowskian approach of the present paper allows us to treat all such terms without ambiguity. Nevertheless, these terms are not enough for complete description of the light-ray trajectory because the first post-Minkowskian approximation does not include terms being quadratic with respect to gravitational constant G which may be comparable in self-gravitating systems with terms of order (Formula presented)
-
To be more precise, the post-Newtonian scheme may give inconsistent results for light propagation in those terms which are proportional to the product of mass of the light-deflecting body and square of its velocity, that is, (Formula presented) At the same time the post-Minkowskian approach of the present paper allows us to treat all such terms without ambiguity. Nevertheless, these terms are not enough for complete description of the light-ray trajectory because the first post-Minkowskian approximation does not include terms being quadratic with respect to gravitational constant G which may be comparable in self-gravitating systems with terms of order (Formula presented)
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-
-
-
92
-
-
85037177890
-
-
We neglect the proper motion of the pulsar in the sky which brings about the small secular change in coordinates of the vector (Formula presented) The error of the approximation is about (Formula presented), where (Formula presented) is the proper motion of the pulsar and (Formula presented) is the total span of observation. This error is much smaller than 1 (Formula presented)s being presently unmeasurable
-
We neglect the proper motion of the pulsar in the sky which brings about the small secular change in coordinates of the vector (Formula presented) The error of the approximation is about (Formula presented), where (Formula presented) is the proper motion of the pulsar and (Formula presented) is the total span of observation. This error is much smaller than 1 (Formula presented)s being presently unmeasurable.
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93
-
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0009170937
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-
J. M. Moran, J. N. Hewitt, K. L. Lo
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M. Birkinshaw, in Lecture Notes in Physics 330, Gravitational Lenses, edited by J. M. Moran, J. N. Hewitt, and K. L. Lo (Springer-Verlag, Berlin, 1989), p. 59.
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(1989)
Lecture Notes in Physics 330, Gravitational Lenses
, pp. 59
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Birkinshaw, M.1
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94
-
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85037244175
-
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The integrals in Eqs. (747576) are identically zero because of our assumption that the velocities of the gravitating bodies are constant
-
The integrals in Eqs. (747576) are identically zero because of our assumption that the velocities of the gravitating bodies are constant.
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97
-
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85037188910
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If we suppose that the dipole moment of the lens (Formula presented) is not equal to zero, then the expression for the gravitational lens potential (Formula presented) assumes the form (Formula presented)where the impact parameter (Formula presented) is the distance from the origin of the coordinate system to the point of the closest approach of light ray to the lens. The scrutiny examination of the multipole structure of the shape of the curves of constant value of (Formula presented) in cosmological gravitational lenses
-
If we suppose that the dipole moment of the lens (Formula presented) is not equal to zero, then the expression for the gravitational lens potential (Formula presented) assumes the form (Formula presented)where the impact parameter (Formula presented) is the distance from the origin of the coordinate system to the point of the closest approach of light ray to the lens. The scrutiny examination of the multipole structure of the shape of the curves of constant value of (Formula presented) in cosmological gravitational lenses 9798 may reveal the presence of dark matter in the lens and identify the position of its center of mass, velocity and density distribution which can be compared with analogous characteristics of luminous matter in the lens. In case of the transparent gravitational lens the expression for the gravitational lens potential in terms of transverse-traceless (TT) internal and external multipole moments can be found in Ref. 11. Discussion of observational effects produced by the spin of the lens is given in Ref. 99.
-
-
-
-
99
-
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17044411834
-
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A. V. Olinto, J. A. Frieman, D. N. Schramm
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M. Bartelmann, in Proceedings of the 18th Texas Symposium on Relativistic Astrophysics and Cosmology, edited by A. V. Olinto, J. A. Frieman, and D. N. Schramm (World Scientific, Singapore, 1998), p. 533.
-
(1998)
Proceedings of the 18th Texas Symposium on Relativistic Astrophysics and Cosmology
, pp. 533
-
-
Bartelmann, M.1
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101
-
-
85037215729
-
-
We emphasize that in the linear with respect to (Formula presented) approximation the gravitational shift of frequency depends only on transverse component of relative motion of lens and observer. Dependence of the gravitational shift of frequency on longitudinal motion of lens (radial velocity) appears only if one takes quadratic and higher order powers in (Formula presented)
-
We emphasize that in the linear with respect to (Formula presented) approximation the gravitational shift of frequency depends only on transverse component of relative motion of lens and observer. Dependence of the gravitational shift of frequency on longitudinal motion of lens (radial velocity) appears only if one takes quadratic and higher order powers in (Formula presented)
-
-
-
-
102
-
-
85037222875
-
-
It is worthwhile to point out that in the expression (Formula presented) for the impact parameter the term (Formula presented) must be treated as (Formula presented) where (Formula presented) are coordinates of the source of light. The unique interpretation of meaning of the impact parameter (Formula presented) in the last term of Eq. (168) as well as in the expression (153) for the gravitational lens potential (Formula presented) is achieved immediately after solving relativistic equations of light geodesic in which the unperturbed trajectory of light ray is used everywhere. This eliminates ambiguity in the definition of (Formula presented)
-
It is worthwhile to point out that in the expression (Formula presented) for the impact parameter the term (Formula presented) must be treated as (Formula presented) where (Formula presented) are coordinates of the source of light. The unique interpretation of meaning of the impact parameter (Formula presented) in the last term of Eq. (168) as well as in the expression (153) for the gravitational lens potential (Formula presented) is achieved immediately after solving relativistic equations of light geodesic in which the unperturbed trajectory of light ray is used everywhere. This eliminates ambiguity in the definition of (Formula presented)
-
-
-
-
103
-
-
85037202777
-
-
Remember that (Formula presented) and (Formula presented) as a consequence of Eq. (88)
-
Remember that (Formula presented) and (Formula presented) as a consequence of Eq. (88).
-
-
-
-
105
-
-
85037232159
-
-
Critics of the results of Ref
-
Critics of the results of Ref. 103 by Gurvits and Mitrofanov 105 is not rigorously justified. A discrepancy by a factor of 2 between amplitudes of the perturbation of the background cosmic radiation in Refs. 103 and 105 has an algebraic origin rather than a physical one.
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-
-
107
-
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0009174811
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N. Aghanim, S. Prunet, O. Forni, and F. R. Bouchet, Astron. Astrophys. 334, 409 (1998).
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85037214397
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More details about how to integrate the equations of light propagation accounting for (static) high-order multipoles can be found in Refs
-
More details about how to integrate the equations of light propagation accounting for (static) high-order multipoles can be found in Refs. 411.
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85037220974
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If one tries to perform a global integration of Eq. (179) using the Taylor time series expansion of the bodies’ coordinates, the correct logarithmic behavior of the integral takes place only if the first two terms in the expansion are taken into account which is physically equivalent to the case of bodies moving uniformly along straight lines. The logarithm diverges if limits of integration in Eq. (179) go to (Formula presented) and (Formula presented), respectively. Account for the third term in the expansion (accelerated motion of the bodies) supresses the logarithmic behavior of the integral for large intervals of integration comparable with the characteristic Keplerian period of the system, and brings about incorrect prediction for the Shapiro time delay and the total angle of deflection of light. As bodies in self-gravitating systems always move with acceleration, one evidently has a mathematical inconsistency in the Taylor time series expansion for finding a numerical value of the integral (179) in the case where the photon goes beyond the limits of the near zone of the system
-
If one tries to perform a global integration of Eq. (179) using the Taylor time series expansion of the bodies’ coordinates, the correct logarithmic behavior of the integral takes place only if the first two terms in the expansion are taken into account which is physically equivalent to the case of bodies moving uniformly along straight lines. The logarithm diverges if limits of integration in Eq. (179) go to (Formula presented) and (Formula presented), respectively. Account for the third term in the expansion (accelerated motion of the bodies) supresses the logarithmic behavior of the integral for large intervals of integration comparable with the characteristic Keplerian period of the system, and brings about incorrect prediction for the Shapiro time delay and the total angle of deflection of light. As bodies in self-gravitating systems always move with acceleration, one evidently has a mathematical inconsistency in the Taylor time series expansion for finding a numerical value of the integral (179) in the case where the photon goes beyond the limits of the near zone of the system.
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125
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85037238279
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L. Petrov, Absolute methods for determination of reference system from VLBI observations, in Proceedings of the 13-th Working Meeting on European VLBI for Geodesy and Astrometry, edited by W. Schlüter and H. Hase (BKG, Wettzell, 1999), pp. 138–143
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L. Petrov, Absolute methods for determination of reference system from VLBI observations, in Proceedings of the 13-th Working Meeting on European VLBI for Geodesy and Astrometry, edited by W. Schlüter and H. Hase (BKG, Wettzell, 1999), pp. 138–143.
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127
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85037242647
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IERS Conventions, IERS Technical Note 21, Obs. de Paris, edited by D. D. McCarthy, 1996
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IERS Conventions, IERS Technical Note 21, Obs. de Paris, edited by D. D. McCarthy, 1996.
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129
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85037255753
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For VLBI observations of spacecrafts in the solar system the term under discussion can be important and deserves a more careful study
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For VLBI observations of spacecrafts in the solar system the term under discussion can be important and deserves a more careful study.
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133
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85037244315
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European Space Agency Information Note No 41-97, Paris, December, 1997, url http://www.esa.int/Info/97/info41.html
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European Space Agency Information Note No 41-97, Paris, December, 1997, url http://www.esa.int/Info/97/info41.html
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85037235777
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That is, the metric tensor obeys the special four differential conditions in Ref
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That is, the metric tensor obeys the special four differential conditions in Ref. 19 which single out the class of the harmonic coordinates from the infinite number of arbitrary coordinate systems on the space-time manifold.
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144
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85037216120
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A complete analysis of differences between two relativistic formulations of light deflection, the post-Newtonian and post-Minkowskian, will be given elsewhere
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A complete analysis of differences between two relativistic formulations of light deflection, the post-Newtonian and post-Minkowskian, will be given elsewhere.
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146
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0002155461
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N. Ashby, in Gravitation and Relativity: At the turn of the Millennium, Proceedings of the GR-15 Conference, IUCAA, Pune, India, 1997, edited by N. Dadhich and J. Narlikar (InterUniversity Centre for Astronomy and Astrophysics, Pune, 1998), p. 231.
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149
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85037215796
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We again emphasize that among three variables t, (Formula presented), and (Formula presented) only two can be considered as independent because of relationship (Formula presented) derived in Eq. (16). The same is valid for the set (Formula presented) (Formula presented), and (Formula presented)
-
We again emphasize that among three variables t, (Formula presented), and (Formula presented) only two can be considered as independent because of relationship (Formula presented) derived in Eq. (16). The same is valid for the set (Formula presented) (Formula presented), and (Formula presented)
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150
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85037251660
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See formula (24) for calculation of partial derivative of retarded time s with respect to (Formula presented)
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See formula (24) for calculation of partial derivative of retarded time s with respect to (Formula presented)
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151
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85037245358
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Hence, the upper limit of the integral is not differentiated with respect to (Formula presented) as it was in Eq. (249)
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Hence, the upper limit of the integral is not differentiated with respect to (Formula presented) as it was in Eq. (249).
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