Docking ExercisePreparing for the return to space, NASA needs to train astronauts in spacecraft docking. Besides simulators, they want to train with actual vehicles, but we have no spacecraft touse. That and budget cuts have led to the use of a computer controlled go cart and a semitractor trailer with a 5 meter long ramp. In the trailer is a firmly mounted mini dockingring at the top of the ramp and the go cart has a matching tunnel mounted on the front sothat it will slip into the docking ring and latch. The computer on the go cart has a verysimple set of commands. Each program step specifies a time interval in seconds and eitheran acceleration in m/s2 or a velocity in m/s which is to be used for that interval. You canonly specify a velocity to maintain if you are already moving at that velocity. The cart hassensors which provide distance from the back of the trailer and velocity relative to theground and velocity relative to the trailer. The starting configuration has the cart moving at 5 m/s relative to the road and 200meters from the bottom of the ramp (205 meters from the docking ring). The truck ismoving at 15 m/s relative to the road. You are to achieve docking within 200 seconds andthe docking clamps need a 0.3 m/s impact speed to set the latches. For safety, youraccelerations should all be less than 5g’s (49 m/s2) and your velocity relative to the truckshould be less than 3 m/s when you are within 15 meters of the ramp (20 meters fromdocking).There is no unique answer for this problem, but do check to make sure that your cartdoesn’t accelerate past the docking ring. A good way to check your solution is to use aspreadsheet with 1 row per second and calculate the distance to docking at each second. This isn’t hard, but it does require attention to details and you will likely learn somethingabout how many variables you can specify without creating a conflict. Your Solution: velocity in m/s, acceleration in m/s2.

  sequence  is a continuous and distinctive band of  stars  that appears on plots of stellar  color  versus  brightness. these color-magnitude plots are known as  hertzsprung–russell diagramsafter their co-developers,  ejnar hertzsprungand  henry norris russell. stars on this band are known as  main-sequence stars  or  dwarf stars. these are the most numerous true stars in the universe, and include the earth's  sun.after condensation and ignition of a star, it generates  thermal energy  in its dense core region through  nuclear fusion  of  hydrogen  into  helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in  hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of  gravitational collapse  from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the  photosphere. the energy is carried by either  radiation  or  convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the  mass of the sun  (1.5  m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the  proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of  carbon,  nitrogen  and  oxygen  as intermediaries in the  cno cycle  that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4  m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star  evolves  away from the main sequence on the hr diagram, into a  supergiant,  red giant, or directly to a  white dwarf.

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Answer increases the risk of developing genetically influenced diseases;

F= (mass)(acceleration) = mam = 0.25 kgvi = 16 m/st = 2 svf = 0 m/s (since it was put to stop)a=(vf-vi)/ta=(0-16)/2a = 8 m/s^2 (decelerating)f = ma = (0.25 kg)(8 m/s^2)f = 2 nhope this !