Answer:
Rate = -1/2 Δ[SO<sub>2</sub>]/Δt
so its gonna be (in more simple terms) rate= -1/2Δ(SO2)/Δt
Explanation:
Hey there!:
density = 3.51 g/cm³
Volume = 0.0270 cm³
Therefore:
D = m / V
3.51 = m / 0.0270
m = 3.51 * 0.0270
m = 0.09477 g
All of the energy from the Sun that reaches the Earth arrives as solar radiation, part of a large collection of energy called the electromagnetic radiation spectrum. Solar radiation includes visible light, ultraviolet light, infrared, radio waves, X-rays, and gamma rays. Radiation is one way to transfer heat.
Answer: At equilibrium, the partial pressure of
is 0.0330 atm.
Explanation:
The partial pressure of
is equal to the partial pressure of
. Hence, let us assume that x quantity of
is decomposed and gives x quantity of
and x quantity of
.
Therefore, at equilibrium the species along with their partial pressures are as follows.
At equilibrium: 0.123-x x x
Now, expression for
of this reaction is as follows.
![K_{p} = \frac{[PCl_{3}][Cl_{2}]}{[PCl_{5}]}\\0.0121 = \frac{x \times x}{(0.123 - x)}\\x = 0.0330](https://tex.z-dn.net/?f=K_%7Bp%7D%20%3D%20%5Cfrac%7B%5BPCl_%7B3%7D%5D%5BCl_%7B2%7D%5D%7D%7B%5BPCl_%7B5%7D%5D%7D%5C%5C0.0121%20%3D%20%5Cfrac%7Bx%20%5Ctimes%20x%7D%7B%280.123%20-%20x%29%7D%5C%5Cx%20%3D%200.0330)
Thus, we can conclude that at equilibrium, the partial pressure of
is 0.0330 atm.