To solve this problem it is only necessary to apply the kinematic equations of angular motion description, for this purpose we know by definition that,
![\theta = \frac{1}{2}\alpha t^2 +\omega_0 t + \theta_0](https://tex.z-dn.net/?f=%5Ctheta%20%3D%20%5Cfrac%7B1%7D%7B2%7D%5Calpha%20t%5E2%20%2B%5Comega_0%20t%20%2B%20%5Ctheta_0)
Where,
Angular Displacement
Angular Acceleration
Angular velocity
Initial angular displacement
For this case we have neither angular velocity nor initial angular displacement, then
![\theta = \frac{1}{2}\alpha t^2](https://tex.z-dn.net/?f=%5Ctheta%20%3D%20%5Cfrac%7B1%7D%7B2%7D%5Calpha%20t%5E2)
Re-arrange for ![\alpha,](https://tex.z-dn.net/?f=%5Calpha%2C)
![\alpha = \frac{2\theta}{t^2}](https://tex.z-dn.net/?f=%5Calpha%20%3D%20%5Cfrac%7B2%5Ctheta%7D%7Bt%5E2%7D)
Replacing our values,
![\alpha = \frac{2(40rev*\frac{2\pi rad}{1rev})}{60^2}](https://tex.z-dn.net/?f=%5Calpha%20%3D%20%5Cfrac%7B2%2840rev%2A%5Cfrac%7B2%5Cpi%20rad%7D%7B1rev%7D%29%7D%7B60%5E2%7D)
![\alpha = 0.139rad/s](https://tex.z-dn.net/?f=%5Calpha%20%3D%200.139rad%2Fs)
Therefore the ANgular acceleration of the mass is ![0.139rad/s^2](https://tex.z-dn.net/?f=0.139rad%2Fs%5E2)
Put the object or material on a scale to figure out<span> its mass. 3. Divide the mass by the volume to </span>figure out the density<span> (p = m / v). You may also need to know </span>how to calculate<span> the volume of a </span>solid s<span>o use the formula</span>
Between the stars' absolute magnitudes<span> or </span>luminosities<span> versus their </span>stellar classifications<span> or </span>effective temperatures<span>. </span>
An electron that is far away from the nucleus have higher energy than an electron near the nucleus. Nucleus are positively charged and those electrons near it get attracted; those electrons gain kinetic energy hence reducing their internal energy. The electrons far from nucleus have low kinetic energy hence more internal energy.