Answer:
0.915 Nm
Explanation:
1 revolution = 2π rad
We can use the following equation of motion to find out the acceleration acting on the disk
where ![\omega v = 2.5 rad/s is the final angular velocity of the disk, [tex]\omega_0](https://tex.z-dn.net/?f=%5Comega%20v%20%3D%202.5%20rad%2Fs%20is%20the%20final%20angular%20velocity%20of%20the%20disk%2C%20%5Btex%5D%5Comega_0)
= 0 rad/s is the initial velocity of the can when it starts from rest, 
is the angular distance traveled, 
is the angular acceleration of the disk, which we care looking for:
The moment of inertia of the solid disk is:
where m is the mass and R is the radius of the disk
The net torque applied is
Answer:
Mars and Earth are two of the planets of the solar system. Some of the ways in which Mars is different from Earth are as follows-
- The size of the earth is bigger than Mars as Earth has a radius of nearly 6400 km, whereas Mars has a radius of about 3400 km.
- The atmosphere of earth is primarily comprised of gases such as 78% of Nitrogen (N₂), 21% of Oxygen (O₂), 0.03% of Carbon dioxide (CO₂), and 0.9% of Argon (Ar), whereas the atmosphere of Mars is mainly comprised of 95% of CO₂, 3% of molecular N₂, and 2% of Ar.
- The surface gravity also marks a contrasting difference as on Mars, the gravity at the surface is only about 38%, in comparison to the gravity at the earth's surface.
Answer: D
Explanation:
When an object falls gravity is pulling down on it and is picking up speed, but as it gains speed air resistance becomes a faster. Air resistance increases with speed. And that force keeps it from accelerating eventually the object will pick up speed such that the force due to air resistance will keep it from getting any more speed at that point force due to air resistance is equal to its weight (mg) and the net force is equal to zero so it won’t accelerate any more at that point it is said to be moving in terminal velocity.
When an object has reached terminal velocity, it will have a constant velocity
My answer -
the corona,
the sun's outer layer, reaches temperatures of up to 2 million degrees
Fahrenheit (1.1 million Celsius). At this level, the sun's gravity can't
hold on to the rapidly moving particles, and it streams away from the
star.
The sun's activity shifts over the course of its 11-year cycle, with
sun spot numbers, radiation levels, and ejected material changing over
time. These alterations affect the properties of the solar wind,
including its magnetic field properties, velocity, temperature and
density. The wind also differs based on where on the sun it comes from
and how quickly that portion is rotating.
The velocity of the solar wind
is higher over coronal holes, reaching speeds of up to 500 miles (800
kilometers) per second. The temperature and density over coronal holes
are low, and the magnetic field is weak, so the field lines are open to
space. These holes occur at the poles and low latitudes, and reach their
largest when activity on the sun is at its minimum. Temperatures in the
fast wind can reach up to 1 million degrees F (800,000 C).
At the coronal streamer belt around the equator, the solar wind travels
more slowly, at around 200 miles (300 km) per second. Temperatures in
the slow wind reach up to 2.9 million F (1.6 million C).
p.s
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