Answer:
True.
Explanation:
Velocity can be defined as the rate of change in displacement (distance) with time. Velocity is a vector quantity and as such it has both magnitude and direction.
Mathematically, velocity is given by the equation;
Simply stated, a vector quantity has both magnitude and direction.
Thus, a vector quantity is: A deer running 15 meters per second due west.
Answer: Arrow B
Explanation:
Arrow B best best represents the path the ball follows after the string breaks.
This is because the described situation is related to <u>uniform circular motion</u>, in which the tangential velocity is the linear velocity vector that is <u>always tangent to the trajectory</u> and is the distance traveled by the ball in its circular motion in a period of time.
Hence, if this circular motion suddenly stops, the ball will fly in a direction that is tangent to that circle.
Answer:
- your body moving forwards when sudden brakes/force is applied e.g. sudden braking in a car
- feeling a backwards force when something moves quickly from rest e.g a bus
- when you stir a cup of tea, it continues to swirl for a short period of time even though you have stopped
- when shaking a tree, it's leaves or fruit fall down
- satellites which move due to the inertia of motion
hope this helped :)
When a car maintains a velocity of exactly 65 mph, it's acceleration is zero.
<h3>What is acceleration?</h3>
The acceleration is time rate of change of velocity.
When the velocity is not changing with respect to time, it is said to be an object moving with constant velocity.
At constant velocity, there is no acceleration.
Thus, when a car maintains a velocity of exactly 65 mph, it's acceleration is zero.
Learn more about acceleration.
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The planetary temperature energy balance is obtained by radiating back the absorbed radiation energy from outer-space, by the planet and thus acquiring thermal equilibrium.
What is the process of attaining thermal equilibrium by Earth?
The Stefan-Boltzmann law states that the more the temperature a planet has, the more it will radiate out to reach thermal equilibrium.
We know that outer space contains large masses of radiative energy freely distributed in its vast expanse. A small fraction of this energy is absorbed by the Earth through the atmosphere, surface land, clouds etc.
Now, radiative balance is achieved when a planet's surface continuously warms up until it reaches its peak at which point the same amount of absorbed energy can then be radiated back to space. The relative amount of energy radiated back by a planet is dependent upon the size of the planet.
A colder planet relatively absorbs lower amount of radiation energy from space. In some time, as the planet heats up enough, the energy is radiated back to the space attaining thermal equilibrium.
Learn more about Stefan-Boltzmann law here:
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