Ask question

Ask question

All categories

2 years ago

15

If f3=0 and f1=12n, what does the magnitude of f? 2 have to be for there to be rotational equilibrium? answer numerically in new

tons to two significant figures.

1 answer:

lisov135 [29]2 years ago

4 0

Not to good with math im a language and history kinda guy sorry

You might be interested in

find the resultant in the x-direction , Rx and y-direction , Ry for F1 = 2.5n in the positive x-direction f2 = 1n in the negativ

Advocard [28]

The resultant in the x-direction:

Rx = F1 + F2 = 2.5 N - 1 N = 1.5 N .

The resultant in the y-direction:

Ry = F3 + F4 = 2 N - 3 N = -1 N.

5 0

2 years ago

If volume is constant and heat is added, what happens to the

bezimeni [28]

Answer:

the temperature would Increase and pressure would increase

Explanation:

This would occur because the temperature would move to the liquid through conduction and the pressure would increase because the heat would cause more and more pressure

7 0

2 years ago

Use examples to explain how the geosphere interacts with two other of Earth's spheres. Explain the interaction for each using co

Orlov [11]

The geosphere interacts with the hydrosphere when water causes rock to erode. The atmosphere provides the geosphere with heat and energy for erosion, and the geosphere reflects the sun's energy back into the atmosphere.

7 0

2 years ago

Read 2 more answers

When illustrating relative dating by

Rainbow [258]

Answer:

A The Bottom

Explanation:

Brainlist Tho??

8 0

2 years ago

Calculate the propellant mass required to launch a 2000 kg spacecraft from a 180 km circular orbit on a Hohmann transfer traject

Finger [1]

Answer:

t = 12,105.96 sec

Explanation:

Given data:

weight of spacecraft is 2000 kg

circular orbit distance to saturn = 180 km

specific impulse = 300 sec

saturn orbit around the sun R_2 = 1.43 *10^9 km

earth orbit around the sun R_1= 149.6 * 10^ 6 km

time required for the mission is given as t

$t = \frac{2\pi}{\sqrt{\mu_sun}} [\frac{1}{2}(R_1 + R_2)]^{3/2}$

where

$\mu_{sun}$ is gravitational parameter of sun = 1.32712 x 10^20 m^3 s^2. $t = \frac{2\pi}{\sqrt{ 1.32712 x 10^{20}}} [\frac{1}{2}(149.6 * 10^ 6 +1.43 *10^9 )]^{3/2}$

t = 12,105.96 sec

6 0

2 years ago