The beginning development of a
star is marked by a supernova explosion, with the gases present in the nebula
being forced to scatter. As the star shrinks, radiation of the surface increases
and create pressure on the outside shell to push it away and forming a
planetary nebula or white dwarf.
B. It’s the same roughly at all latitudes
Answer:
Explanation:
= 4190 J/kg.K
= 910 J/Kg. K
= 1.50 kg
= 1.80 kg
ΔT + ΔT
= (1.50)(910)(85.0-20)+(1.80)(4190)(85.0-20)
= 578,955 J
= 579 kJ
Answer:
the final kinetic energy is 0.9eV
Explanation:
To find the kinetic energy of the electron just after the collision with hydrogen atoms you take into account that the energy of the electron in the hydrogen atoms are given by the expression:
you can assume that the shot electron excites the electron of the hydrogen atom to the first excited state, that is
-10.2eV is the energy that the shot electron losses in the excitation of the electron of the hydrogen atom. Hence, the final kinetic energy of the shot electron after it has given -10.2eV of its energy is: