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In a natural thermodynamic process, the sum of the entropies of the interacting thermodynamic systems increases. In space, this law governs the fate of heat energy and its dispersion between objects and the cosmic microwave background.

An object remains at rest, or in uniform motion in a straight line, unless acted upon by a force. In the vacuum of space, spacecraft continue on their trajectories without external forces.

The total energy radiated per unit surface area of a black body across all wavelengths is proportional to the fourth power of the black body's temperature ($j^* = \sigma T^4$). This law is used to calculate the luminosity and temperature of stars.

A line segment joining a planet and the Sun sweeps out equal areas during equal intervals of time. This principle implies that planetary velocity varies depending on its distance from the Sun and is useful for mission planning in space exploration.

Every particle attracts another particle with a force that is proportional to the product of their masses and inversely proportional to the square of the distance between their centers ($F = G \frac{m_1 m_2}{r^2}$). Gravitational forces are key to understanding orbits and trajectories of bodies in space.

Galaxies are moving away from each other at speeds proportional to their distance, which can be described with $v = H_0 \times d$. This law underpins the concept of an expanding universe observable in space.

Planets orbit the Sun in ellipses with the Sun at one of the two foci. In space, this law helps in plotting spacecraft trajectories around celestial bodies.

The total momentum of an isolated system remains constant if no external forces are applied. In space, this law is evident when astronauts move in the International Space Station and their movements are counteracted by the station's opposite movement.

Objects emit radiation according to their temperature; hotter objects emit more radiation. In space, this is crucial for thermal control systems of spacecraft and understanding the heat emission of stars and planets.

Time measured along different trajectories is affected by differences in velocity and gravity, known as time dilation ($t' = \frac{t}{\sqrt{1-\frac{v^2}{c^2}}}$). Space travel at high velocities or in strong gravitational fields will experience this effect.

The transfer of heat within a material or between materials that are in direct contact. In the vacuum of space, thermal conduction is minimal except within spacecraft materials and suits.

For every action, there is an equal and opposite reaction. This principle is the basis of rocket propulsion in space as exhaust gases expelled provide the thrust to move a spacecraft.

The principle that mass and energy are equivalent and can be converted into each other ($E = mc^2$). In space, this concept is exemplified by processes like nuclear fusion in stars that produce enormous amounts of energy.

The square of the orbital period of a planet is directly proportional to the cube of the semi-major axis of its orbit ($T^2 \propto a^3$), which can be used to determine the distance of a planet from the sun or any two bodies in space.

The total energy of an isolated system remains constant over time. This principle is used in calculating the energy required for space travel and understanding the energy dynamics of celestial bodies.

These rules (current law and voltage law) govern the conservation of charge and energy in electrical circuits, essential for the power systems on spacecraft and satellites.

The magnitude of the force between two point charges is directly proportional to the magnitude of the charges and inversely proportional to the square of their separation distance ($F = k \frac{|q_1 q_2|}{r^2}$). This law is important in electrostatic calculations for spacecraft design.