By Jim Mesko, Joe Sewell, Don Greer

Constructed out of the DB-7 sequence of sunshine bombers. A-20s, Havocs & DB-7s observed motion in nearly each significant theatre of operation in the course of WWII. Used as a mild bomber, flooring strafer & nightfighter. Over a hundred images, forty aspect drawings, three pages of scale drawings, thirteen colour work, 50 pages.

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**Extra resources for A-20 Havoc in action No 144**

**Example text**

Later, they acquired time dependence, and therefore the full time derivative implied in Eqs. 16) became different from the partial one implied in Eq. 11). 20). This restriction, too, parallels a similar one present in field theories. Below we shall encounter a situation where this restriction becomes crucial. 5 If we agree that is a function of both the time and the parameters Cn , but not of their derivatives,6 then the right-hand side of Eq. 22) will implicitly contain the first time derivatives of Cn .

Celestial Mechanics and Dynamical Astronomy (submitted). 22. Colombo, G. (1966). Cassini’s second and third laws. , 71, pp. 891–896. 23. Efroimsky, M. (2005b). Long-term evolution of orbits about a precessing oblate planet. 2. The case of variable precession. Celestial Mechanics & Dynamical Astronomy (submitted). 24. Efroimsky, M. (2005c). The theory of canonical perturbations applied to attitude dynamics and to the Earth rotation. astro-ph/0506427. 3 Solving Two-Point Boundary Value Problems Using Generating Functions: Theory and Applications to Astrodynamics Vincent M.

From Eq. 31). This condition coincides with the Lagrange constraint = 0 when the perturbation depends only upon positions (not upon velocities or momenta). 31) deviates from that of Lagrange, and the orbital elements rendered by Eq. 33) are no longer osculating (so that the corresponding instantaneous conics are no longer tangent to the physical trajectory). Of an even greater importance will be the following observation. If we have a velocitydependent perturbing force, we can always find the appropriate Lagrangian variation and, therefrom, the corresponding variation of the Hamiltonian.