Momentum Conservation One object m1 has a mass of 2 kg and moves with a speed of 9 m/s to the right. Another object m2 has a mass of 3 kg and moves to the left with a speed on 3 m/s. The two objects collide. After the collision, the first object m1 moves to the right with a speed of 1.5 m/s. The second object m2 moves to the right at 2 m/s. Item at position 5 5 1 point What type of collision is this? Inelastic Super-elastic Perfectly inelastic Elastic

see that this shock is completely elastic

Explanation:

In this case we have the collision of two bodies, so that the moments conserve we must define a system in such a way that the forces during the crash are internal, this system is the one formed by the two bodies

let's write the moment in two moments

initial instant. Before the crash

      p₀ = m₁ v₁_i + m₂ v₂_i

final moment. Right after the crash

        pf = m₁ v₁_f + m₂ v₂_f

to define what kind of shock we have we use the recovery constant

      po = e pf

where the term e, called the recovery constant, determines the type of shock we have, for a perfectly elastic shock it is worth 1 and for an inelastic shock it is worth 0

let's substitute the values

      2 9 - 3 3 = e (2 1,5 + 3 2)

          9 = e 9

           e = 1

therefore we see that this shock is completely elastic

One of the leading theories of hot-Jupiter formation holds that gas giants in distant orbits become hot Jupiters when the gravitational influences from nearby stars or planets drive them into closer orbits. They formed as gas giants beyond the frost line and then migrated inwards.

Explanation:

In the migration hypothesis, a hot Jupiter forms beyond the frost line, from rock, ice, and gases via the core accretion method of planetary formation. The planet then migrates inwards to the star where it eventually forms a stable orbit. The planet may have migrated inward smoothly via type II orbital migration.  

Hot-Jupiters are heated gas giant planets that are very close to their stars, just a few million miles distant and orbiting their stellar hosts in just a few days. The reason why there isn't one in our Solar System is down to its formation. All gas giants form far from their star but then some migrate inwards.

Hot-Jupiters  will just happen to transit about 10% (that is, since orbital planes) this is consistent with the rate expected from geometry of . The actual frequencies of hot Jupiters around normal stars is surprisingly hard to figure out.