Answer:
The items here are describing either a condition in a later interacton or a protogalactic cloud. The results matching with spiral and elliptical galaxy are:
For spiral galaxy are options 6,3,2 and 5.
and for elliptical galaxy are options 4 and 1.
Explanation:
Here it is given that astrnomers suspect that types of galaxy can be affected both by the conditions which occurs due to protogalactic cloud and then from it forms the initial conditions and then by the later interactions with the other galaxies.
so, both types of galaxies are matched with their respective items given:
A. Spiral galaxy:
2. A galaxy collision results tostripping of gas.
3. The protogalactic cloud rotates in a very slow motion.
5. The density of protogalactic cloud is very high.
6. when the protogalactic cloud shrinks cloud forms very rapidly.
B. Elliptical galaxy:
1. The protogalactic cloud has high angular momentum.
4. Most of the protogalactic gases settles down into a disk.
Using the formula: ΔY = V₀y * t + (1/2) * ay * t²
Solve for time and get: 1.968s
Then use: v = d/t in the x-direction and get: d = 3.936
Answer:
μ=0.151
Explanation:
Given that
m= 3.5 Kg
d= 0.96 m
F= 22 N
v= 1.36 m/s
Lets take coefficient of kinetic friction = μ
Friction force Fr=μ m g
Lets take acceleration of block is a m/s²
F- Fr = m a
22 - μ x 3.5 x 10 = 3.5 a ( take g =10 m/s²)
a= 6.28 - 35μ m/s²
The final speed of the block is v
v= 1.36 m/s
We know that
v²= u²+ 2 a d
u= 0 m/s given that
1.36² = 2 x a x 0.96
a= 0.963 m/s²
a= 6.28 - 35μ m/s²
6.28 - 35μ = 0.963
μ=0.151
Hi there!
We can use the following equation to relate angular velocity to linear velocity.
v = linear velocity (m/s)
ω = angular velocity (3.46 rad/sec)
r = distance from axis of rotation (.12 m)
Plug in the given values.
