c adding research resources during an investigation
<span> Using conservation of energy
Potential Energy (Before) = Kinetic Energy (After)
mgh = 0.5mv^2
divide both sides by m
gh = 0.5v^2
h = (0.5V^2)/g
h = (0.5*2.2^2)/9.81
h = 0.25m
</span>
I would say B. Because actual mass would ricochet off the sidewalk.
Answer:
N = 23.4 N
Explanation:
After reading that long sentence, let's solve the question
The contact force is the so-called normal in this case we can find it by writing the translational equilibrium equation for the y axis
N - w₁ -w₂ =
N = m₁ g + m₂ g
N = g (m₁ + m₂)
let's calculate
N = 9.8 (0.760 + 1.630)
N = 23.4 N
This is the force of the support of the two blocks on the surface.
A star’s death also depends on its mass. The most massive stars
quickly exhaust their fuel supply and explode in core-collapse
supernovae, some of the most energetic explosions in the universe. A
supernova’s radiation can easily (if only briefly) outshine the rest of
its host galaxy. The remnant stellar core will form a neutron star
or a black hole, depending on how much mass remains. If the core
contains between 1.44 and 3 solar masses, that mass will crush into a
volume just 10 to 15 miles wide before a quantum mechanical effect known
as neutron degeneracy pressure prevents total collapse. The
exact upper limit on a neutron star mass isn’t known, but around 3 solar
masses, not even neutron degeneracy pressure can combat gravity’s
inward crush, and the core collapses to form a black hole.
