Imagine you are a scientist observing a chemical reaction in a highly controlled, closed chamber. You are monitoring the reaction A⇌B. The pressure of reactant A is artificially maintained at exactly 1 bar throughout the entire experiment—think of it as being connected to a massive reservoir of gas A. Your only job is to watch the pressure of product B evolve over time as you manipulate the temperature.
This is exactly the scenario presented in this beautiful JEE Advanced problem. It elegantly combines graphical interpretation with the core principles of chemical thermodynamics. Let's break down the journey step-by-step.
Decoding the Graph
Extracting the Equilibrium Pressures
The graph provided is the heart of the problem. It plots the partial pressure of B against time. Notice how the curve features two distinct, perfectly horizontal flat lines. In the world of chemical kinetics and thermodynamics, a flat line on a concentration or pressure vs. time graph screams one word: Equilibrium.
Before time t′, the system is held at a temperature of 1000 K. The graph shows that the pressure of B is perfectly stable at 10 bar. This is our first crucial data point: at 1000 K, the equilibrium partial pressure of B is PB=10 bar.
Suddenly, at time t′, the temperature is doubled to 2000 K. The system experiences a thermal shock! The pressure spikes dramatically (a consequence of the sudden heating and rapid kinetic shift), but eventually, the system finds a new balance. It settles into a new horizontal line at 100 bar. This gives us our second data point: at 2000 K, the new equilibrium partial pressure of B is PB=100 bar.
The Equilibrium Constant
The Bridge to Thermodynamics
To connect these physical observations to thermodynamic properties, we need the equilibrium constant, Kp. For our simple reaction A⇌B, the equilibrium constant is defined as the ratio of the partial pressures of the products to the reactants:
The problem explicitly states a massive constraint: PA is maintained at 1 bar throughout the experiment. This makes our calculation incredibly straightforward. The equilibrium constant Kp is numerically equal to the partial pressure of B!
Let's calculate
Kp for both temperatures:
At
1000 K:
K1000=110=10
At
2000 K:
K2000=1100=100
The Master Equation
Gibbs Free Energy
Now we bring in the heavy machinery of thermodynamics. The standard Gibbs free energy change, ΔG∘, is fundamentally linked to the equilibrium constant by the master equation:
This equation tells us how the intrinsic thermodynamic drive of the reaction (ΔG∘) dictates the final equilibrium position (Kp) at a given temperature (T).
We need to find the ratio of the standard Gibbs energy at 1000 K to that at 2000 K. Let's set up the fraction:
Ratio=ΔG2000∘ΔG1000∘=−R(2000)ln(K2000)−R(1000)ln(K1000)
The Final Ratio
Mathematical Elegance
First, let's clear the clutter. The negative signs and the universal gas constant R cancel out immediately from the numerator and denominator.
Ratio=2000ln(100)1000ln(10)
Here is where a solid grasp of logarithm properties saves the day. Do not leave ln(100) as it is. Recognize that 100 is simply 102. Using the power rule of logarithms, ln(xn)=nln(x), we can rewrite the denominator:
Substitute this beautiful simplification back into our ratio:
Ratio=2000×2ln(10)1000ln(10)
Look at that elegance! The ln(10) terms cancel out completely. We are left with pure, simple arithmetic:
The final answer is 0.25.
Beyond the Problem
Le Chatelier's Whisper
Before we close the book on this problem, let's think like an examiner. What hidden story does this data tell?
Notice that as we increased the temperature from 1000 K to 2000 K, our equilibrium constant Kp increased from 10 to 100. The reaction shifted forward to produce more B at the higher temperature. According to Le Chatelier's Principle, a system will shift to absorb added heat if the reaction is endothermic. Therefore, because heating the system drove the reaction forward, we can definitively conclude that the forward reaction A→B is an endothermic process (ΔH>0).
Always look for these deeper physical insights—they are what separate good students from great physicists and chemists!