Download C.s 1.6 Condition Zero

Condition Zero is a fail-safe procedure the Martian Congressional Republic Navy (MCRN) enacts during boarding procedures. It states should any of the three critical areas of the ship be lost to boarders the bridge, Combat Information Center (CIC), or engineering the ship is to be detonated (self-destructed) immediately. As these areas are considered vital to ship operation or hold critical strategic value (in the case of the CIC), should these areas fall into enemy hands the Captain (or surviving command officer) should consider the ship lost and initiate Condition zero to prevent the enemy from capturing the ship or otherwise using the ship to enemy advantage.

Return to this areas entrance and search the kitchen area for a sub machine gun. Hop onto the crates and onto the dumpster. Jump to the next set of boxes and then to the wrecked car. Climb the hood and get onto the overhang. Jump from the overhang to the air conditioning unit and find a health pack on the other side. Leap from the air conditioner to the balcony to its right. Move around to the side and shoot the guard. Drop into the hole and into the warehouse.

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We study the diffusion of classical particles in channels with varying boundaries. The problem is characterized by the Neumann boundary condition (zero normal current) in contrast to the Dirichlet boundary condition (zero function) for "quantum confinement" problems. Eliminating transverse modes, we derive an effective diffusion equation that describes particle propagation in the space of reduced dimension in the presence of a frozen drift field. The latter stems from boundary variations of the original boundary problem. Boundary variations may thus result in an appreciable change of the particle transport and, in particular, in a nonlinear response to an external field. We show also that there is a difference between the nonlinear responses of open and closed channels.

Kelvin-Voigt constitutive law, Signorini condition, zero gap function, weak formulation, existence, uniqueness, evolution equations, maximal monotone operators, semi-discrete numerical scheme, convergence, regularity, optimal order error estimates

However, as we demonstrate explicitly in this paper, there exists a possibility of such matter distributions which lead to nonzero average values of the first-order metric corrections. Namely, in the framework of the mechanical approach to cosmological problems at the late stage of the Universe evolution we give a concrete example of a rest mass density profile for which the standard formula determining the scalar perturbations results in their nonzero average values. Since exactly this formula underlies the modern N-body simulations which play an extremely important role for the structure formation analysis, the discovered weak point must be eliminated in order to be fully confident in their predictions. We suggest avoiding this challenge without exceeding the limits of the conventional CDM model, by cutting off the nonrelativistic gravitational potentials of cosmic bodies/inhomogeneities (e.g., galaxies).

In order to determine the gravitational potential corresponding to the given sphere, one can solve the Poisson equation (2.2) with the appropriate boundary conditions (R) = 0, d/dr(R) = 0 or use the standard prescription (2.8). The result is the same: inside the sphere (the region I)

meaning that the standard prescription (2.8) can lead to unreasonable nonzero average values of cosmological perturbations. One can naively suppose that the result (3.3) is true only for the considered region of the finite volume V, while averaging over the infinite volume saves the situation. This argumentation is apparently wrong since there is an infinite number of such regions in the model under consideration, and each of them makes a nonzero (negative) contribution when averaging over the infinite volume. Thus, the average value will be again nonzero (negative).

Of course, since the function describes the deviation of the metric coefficients in (2.1) from the corresponding average quantities, its own average value must be equal to zero: =0. The same statement must hold true for , rad, etc. The discovered indubitable disadvantage of the formula (2.8) should not be ignored in the modern N-body simulations (along with [11, 12]; see [16]).

therefore, =0, as it certainly should be. Thus, the use of the finite-range gravitational potential (3.4) instead of the infinite-range one (2.8) leads to reasonable zero average values of cosmological perturbations. This advantage of the proposed formula (3.4) in comparison with (2.8) may be taken into account when simulating the behavior of N-body systems.

Let us mention that in the framework of the extension of the CDM model, assuming the presence in the Universe of the additional constituent (namely, quintessence) with the linear equation of state q = qpq with the constant parameter q = - 1/3, the discussed problem of nonzero average values of cosmological perturbations in the case of the infinite-range gravitational potential is resolved in a different manner: quintessence fluctuations around a point-like nonrelativistic matter inhomogeneity cause the Yukawa form of its potential instead of the Newtonian one, and the average value of the total potential produced by all inhomogeneities is really zero [20], irrespective of the interaction range and its cutoff.

The other extension, assuming a negative spatial curvature, is also characterized by the potential of a point-like inhomogeneity, similar to the Yukawa one, so the average value of the total potential is again zero [2]. 2351a5e196