Our Sun will eventually turn into a red giant and, finally, a white dwarf. Use the Hertzsprung-Russell diagram to describe how the Sun's luminosity and temperature will change as it goes through these stages.

Most stars are rather simple things. They come in a variety of sizes and temperatures, but the great majority can be characterized by just two parameters: their mass and their age. (Chemical composition also has some effect, but not enough to change the overall picture of what we will be discussing here. All stars are about three-quarters hydrogen and one-quarter helium when they are born.)

(newtons first law)

conservation of momentum law states :

momentum before collision = momentum after collision

momentum p (kg-m/s)= mass * velocity

say moving car=1 000 kg, velocity = 10 m/s then p = 1 000*10= 10 000 kg-m/s

say still car = 2 000 kg, velocity = 0 m/s then p = 2 000* 0 = 0 kg-m/s

total momentum prior to collision = 10 000 + 0 = 10 000 kg-m/s

momentum after collision = 10 000 kg-m/s

mass now = 1 000 kg+2 000 kg = 3 000 kg

10 000 = 3 000 kg* velocity m/s

10 000/3 000 = velocity

3.33 m/s = velocity after collision

an impulse is a force applied over time , momentum is exclusive of external forces and a perfect collision is implied