Answer:
Explanation:
The amount of heat released from water is equal to the sum of latent and sensible heats. Let suppose that water is initially at a temperature of 
. Then:
Finally, the amount of heat released from water is now computed by replacing variables:
![\Delta H_{tot} = (1\,mol)\cdot \left[\left(75.3\,\frac{kJ}{mol\cdot K} \right)\cdot (25^{\circ}C-0^{\circ}C)+ 6.025\,\frac{kJ}{mol} + \left(37.7\,\frac{kJ}{mol\cdot K} \right)\cdot (0 + 10^{\circ}C)\right]](https://tex.z-dn.net/?f=%5CDelta%20H_%7Btot%7D%20%3D%20%281%5C%2Cmol%29%5Ccdot%20%5Cleft%5B%5Cleft%2875.3%5C%2C%5Cfrac%7BkJ%7D%7Bmol%5Ccdot%20K%7D%20%5Cright%29%5Ccdot%20%2825%5E%7B%5Ccirc%7DC-0%5E%7B%5Ccirc%7DC%29%2B%206.025%5C%2C%5Cfrac%7BkJ%7D%7Bmol%7D%20%2B%20%5Cleft%2837.7%5C%2C%5Cfrac%7BkJ%7D%7Bmol%5Ccdot%20K%7D%20%5Cright%29%5Ccdot%20%280%20%2B%2010%5E%7B%5Ccirc%7DC%29%5Cright%5D)
Answer:
The electric field will be decreased by 29%
Explanation:
The distance between point P from the distance z = 2.0 R
Inner radius = R/2
Outer raidus = R
Thus;
The electrical field due to disk is:
)
Similarly;
However; the relative difference is:
![\dfrac{\hat {k_a} - \hat {k_b}}{\hat {k_a} }= \dfrac{E_a -E_a + \dfrac{\sigma}{2 \varepsilon_o \Big[1 - \dfrac{2.0 \ R}{\sqrt{(2.0 \ R)^2 + (\dfrac{R}{2})^2}} \Big] } } { \dfrac{\sigma}{2 \varepsilon_o \Big [ 1 - \dfrac{2.0 \ R}{\sqrt{ (2.0 \ R)^2 + (R)^2}} \Big] }}](https://tex.z-dn.net/?f=%5Cdfrac%7B%5Chat%20%7Bk_a%7D%20-%20%5Chat%20%7Bk_b%7D%7D%7B%5Chat%20%7Bk_a%7D%20%7D%3D%20%5Cdfrac%7BE_a%20-E_a%20%2B%20%5Cdfrac%7B%5Csigma%7D%7B2%20%5Cvarepsilon_o%20%20%5CBig%5B1%20-%20%5Cdfrac%7B2.0%20%5C%20R%7D%7B%5Csqrt%7B%282.0%20%5C%20R%29%5E2%20%2B%20%28%5Cdfrac%7BR%7D%7B2%7D%29%5E2%7D%7D%20%5CBig%5D%20%7D%20%7D%20%7B%20%5Cdfrac%7B%5Csigma%7D%7B2%20%5Cvarepsilon_o%20%5CBig%20%5B%201%20-%20%5Cdfrac%7B2.0%20%5C%20R%7D%7B%5Csqrt%7B%20%282.0%20%5C%20R%29%5E2%20%2B%20%28R%29%5E2%7D%7D%20%5CBig%5D%20%7D%7D)
Answer:
Convective zone, chromosphere, corona
Explanation:
A star like the Sun is divided into different layers according to pressure, density, temperature, and the mechanics of energy transport (in the case of the convective zone and radiative zone) for each of those layers.
In stars, there is an equilibrium between two forces, the force of gravity in the inward direction due to their own mass and the radiation pressure in the upward direction as a consequence of the nuclear reaction in their core, that is known as hydrostatic equilibrium.
That leads to different layers according with the properties described above.
Near the core, in the Sun, there is a radiative zone since radiation is the best mechanism of energy transport in this area. Then, in the next layer, it can be found that convection becomes a more efficient way of energy transport that radiation due to the fact that the inner part of the convection zone is at a greater temperature than the outer one.
Finally, there is the atmosphere of the Sun (chromosphere, photosphere, and corona).
Key terms:
Convection: Transport of energy due to different in density and temperature of a material (liquid, gas).
Answer:
30×6=n
Explanation:
30 students in her class× 6 = number of students in the entire 4th grade.
