<h2>
Answer:Radiation-3,Conduction-1,Convection-2</h2>
Explanation:
Radiation is the transfer of heat through electromagnetic waves.
These waves do not require any medium.This is the way we get heat from sun.Radiation is the quickest mode to transfer of heat.
Conduction is the transfer of heat through collisions of atomic particles.
This phenomenon largely occurs in solids like metals.The neighbour atoms sets the atoms into random motion thereby raising the temperature.
Convection is the transfer of heat through actual movement of medium particle.
This phenomenon occurs in gases an liquids.The medium particles actually traverse through the space transferring the heat.
Answer:
B
Explanation:
Newton’s Second Law of Motion
Newton’s Second Law of Motion states that ‘when an object is acted on by an outside force, the mass of the object equals the strength of the force times the resulting acceleration’.
This can be demonstrated dropping a rock or and tissue at the same time from a ladder. They fall at an equal rate—their acceleration is constant due to the force of gravity acting on them.
The rock's impact will be a much greater force when it hits the ground, because of its greater mass. If you drop the two objects into a dish of water, you can see how different the force of impact for each object was, based on the splash made in the water by each one.
Answer:
In the order largest to smallest
Pc = Pb, Pa
Explanation:
Power = Energy expended/time
Pa = 2/2 = 1Watt
Pb = 10/5 = 2Watt
Pc = 2E-3/1E-3 = 2Watt
Answer:
D
Explanation:
This will not change the weight and therefore not change the inertia
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.
