Answer:
a) 0.15 μC b) 9.4*10¹¹ electrons.
Explanation:
As the total charge must be conserved, the total charge on the spheres, after being brought to contact each other, and then separated, must be equal to the total charge present in the spheres prior to be put in contact:
Q = +8.2μC +9.0 μC +(-7.8 μC) + (-8.8 μC) = +0.6 μC
As the spheres are assumed perfect conductors, as they are identical, once in contact each other, the excess charge spreads evenly on each sphere, so the final charge, on each of them, is just the fourth part of the total charge:
Qs = Qt/4 = 0.6 μC / 4 = 0.15 μC.
b) As the charge has a positive sign, this means that each sphere has a defect of electrons.
In order to know how many electrons are absent in each sphere, we can divide the total charge by the charge of one electron, which is the elementary charge e, as follows:
There are a lot.
Some of them are
Gamma radiation
X-ray radiation
Ultraviolet radiation
Visible radiation
Infrared radiation
Microwave radiation
I believe it is called the Greenhouse effect.
Answer:
The magnitude of the acceleration is equal to 19.6m/s² and the acceleration is directed upwards though the magnitude of the charge has doubled. This is because the electric force is directed upwards and from newton's second law of motion the charge will have acceleration in the same direction as the electric force on the charge.
Explanation:
The detailed solution can be found in the attachment below.
Thank you for reading and I hope this is helpful to you.
Answer:
5 years
Explanation:
The centripetal acceleration of a planet is equal to the acceleration due to gravity.
ac = g
Centripetal acceleration is:
ac = v² / r
where v is velocity and r is radius of travel.
Acceleration due to gravity is:
g = GM / r²
where G is gravitational constant, M is the mass of the sun, and r is the radius of travel.
Therefore:
v² / r = GM / r²
v² = GM / r
v = √(GM / r)
Distance is speed times time, so:
d = v t
2πr = √(GM / r) t
t = 2πr √(r / (GM))
t = 2π √(r³) / √(GM)
We know that when r = 1 AU, t = 1 year.
1 = 2π √(1³) / √(GM)
1 = 2π / √(GM)
2π = √(GM)
Substituting:
t = 2π √(r³) / (2π)
t = √(r³)
When r = 3AU:
t = √(3³)
t = 5.2
Planet B takes approximately 5 years to orbit the sun.