### Table 1 Gravitational Lensing Models

"... In PAGE 8: ...Table1 : Gravitational Lensing Models Figure 4: Image con gurations by an elliptical lens. The source planes are on the left and the corresponding images are on the right.... In PAGE 33: ...omplete ring images are excluded in the statistics due to their rareness. Then, eq.(108) becomes L W = 4 (1 ? K)2 1 ? 1 6 R2 0 2 0 + ; (109) where K = 2 ED2 d ( E)=m( E). Numerical computations using the three spherical models in Table1 show that the term (1=6)(R0= 0)2 becomes important only if the radius of the circular galaxy is larger than 8 kpc and gt; 30, while most of the known giant arcs have 10. Therefore, neglecting the source extension cannot cause too serious problems in the evaluation of P(zs; ).... ..."

### Table 5. Constancy of the Gravitational Constant

1984

"... In PAGE 45: ... The variation in the moment of inertia a ects the spin rate of the pulsar, while the variation in the mass can a ect the orbital period in a manner that can add to or subtract from the direct e ect of a variation in G, given by _ Pb=Pb = ?1 2 _ G=G. Thus, the bounds quoted in Table5 for the binary pulsar PSR 1913+16 and the pulsar PSR 0655+64 are theory-dependent and must be treated as merely suggestive. 3.... In PAGE 52: ... This e ect was previously considered unimportant when _ Pb was known only to 10 percent accuracy. Damour and Taylor carried out a careful estimate of this e ect using data on the location and proper motion of the pulsar, combined with the best information available on galactic rotation, and found _ P GAL b apos; ?(1:7 0:5) 10?14 : (50) Subtracting this from the observed _ Pb ( Table5 ) gives the residual _ P OBS b = ?(2:408 0:010[OBS] 0:005[GAL]) 10?12 ; (51) which agrees with the prediction, within the errors. In other words, _ P GR b _ P OBS b = 1:0023 0:0041[OBS] 0:0021[GAL] : (52) The parameters r and s are not separately measurable with interesting accuracy for PSR 1913+16 because the orbit apos;s 47 inclination does not lead to a substantial Shapiro delay.... ..."

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### Table 1: Notations for the cable. ~g : gravitational acceleration

1993

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### Table 2. Properties of Gravitationally Smoothed 13-Atom Morse Clusters.

"... In PAGE 3: ... Morse Clusters The potential for Morse clusters, subject to gravitational interac- tions, becomes VH20849rH20850 H11005 H20888i H20888 jH11022i H20873e2H9251H208491H11002rijH20850 H11002 2eH9251H208491H11002rijH20850 H11002 H5107 rij H20874 (4) where, following Hoare and McInnes,24 we set H9251 H11005 3. The results of our calculations on Morse clusters are summa- rized in Table2 . Note that the softer Morse potential makes the global optimization problem almost trivial by comparison with Lennard-Jones clusters, even without the application of any grav- itational mutual attraction.... ..."

### Table 4.7: Performance of the VSC under influence of gravitational acceleration.

### Table 4.7: Performance of the VSC under influence of gravitational acceleration.

1996

"... In PAGE 12: ...cceleration. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 79 Table4 . IS: Energy spent to drive the 3-link nlanipulator with two passive joints along the Cartesian points in set A.... ..."

### TABLE 1. The Three Gravitational Interactions are Related to Different Types of Matter.

### Table 1. The perturbed results

1997

"... In PAGE 12: ...esults .u11.i/; u12.i// which are given in Table1 and plotted in Fig. 6.... ..."

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