The Cavendish Experiment, famously conducted by Henry Cavendish in 1798, wasn't just a feat of experimental brilliance; it marked a turning point in our understanding of gravity and the universe. While originally designed to determine the Earth's density, its impact extends far beyond our planet, influencing the field of stellar astronomy significantly.
The Experiment:
The experiment itself is relatively simple in principle, yet incredibly ingenious in its execution. It involved a torsion balance, a delicate apparatus consisting of a lightweight rod suspended by a thin wire. At the ends of this rod, two small lead balls were attached. By strategically placing two larger lead spheres near the smaller ones, Cavendish observed the slight twisting force, or torsion, exerted on the wire due to gravitational attraction.
Measuring the period of oscillation of the rod, Cavendish could then calculate the force of attraction between the spheres. This, combined with the known masses and distances involved, allowed him to determine the universal gravitational constant, 'G', a fundamental constant of nature that governs gravitational attraction between any two objects.
Impact on Stellar Astronomy:
The Cavendish Experiment's contribution to stellar astronomy might seem indirect, but it's fundamental. By providing the value of 'G', it allowed astronomers to:
Beyond Earth:
The Cavendish Experiment's legacy extends to other fields of physics as well. It provided the foundation for understanding gravity on a cosmic scale, paving the way for Einstein's theory of general relativity, which revolutionized our understanding of space and time.
The Cavendish Experiment is a testament to the power of experimental science. While initially designed to measure the density of our planet, its impact continues to reverberate throughout the vast cosmos, shaping our understanding of the universe and its unseen wonders.
Instructions: Choose the best answer for each question.
1. What was the primary objective of the Cavendish Experiment?
(a) To measure the speed of light (b) To determine the Earth's density (c) To prove the existence of gravity (d) To calculate the distance to the nearest star
(b) To determine the Earth's density
2. What apparatus did Cavendish use in his experiment?
(a) A telescope (b) A pendulum (c) A torsion balance (d) A barometer
(c) A torsion balance
3. What fundamental constant of nature did Cavendish determine through his experiment?
(a) The speed of light (c) (b) The gravitational constant (G) (c) Planck's constant (h) (d) Boltzmann's constant (k)
(b) The gravitational constant (G)
4. How does the Cavendish Experiment contribute to understanding stellar astronomy?
(a) By providing the value of 'G', it allows astronomers to calculate the masses of stars. (b) By providing the value of 'G', it allows astronomers to measure the distance to stars. (c) By providing the value of 'G', it allows astronomers to predict the lifespan of stars. (d) By providing the value of 'G', it allows astronomers to determine the composition of stars.
(a) By providing the value of 'G', it allows astronomers to calculate the masses of stars.
5. What is a significant implication of the Cavendish Experiment's results for modern astrophysics?
(a) It led to the discovery of the expanding universe. (b) It led to the concept of dark matter. (c) It led to the development of the Hubble Telescope. (d) It led to the discovery of new planets in our solar system.
(b) It led to the concept of dark matter.
Imagine you are a young astronomer studying a binary star system. You have observed the orbital period of the stars and their separation distance. Using the knowledge gained from the Cavendish Experiment, explain how you would calculate the masses of the two stars.
Here's how to calculate the masses of the stars in a binary system using the Cavendish Experiment's legacy:
1. **Newton's Law of Universal Gravitation:** The force of gravity between two objects is directly proportional to the product of their masses and inversely proportional to the square of the distance between them. This can be expressed as:
F = G * (m1 * m2) / r^2
Where: * F is the gravitational force * G is the universal gravitational constant (determined by Cavendish) * m1 and m2 are the masses of the two stars * r is the distance between the stars
2. **Centripetal Force:** In a binary system, the stars are in orbit around each other, experiencing a centripetal force that keeps them in their orbits. This force is equal to the gravitational force between them.
Fc = (m * v^2) / r
Where: * Fc is the centripetal force * m is the mass of one star * v is the orbital velocity of the star * r is the separation distance between the stars
3. **Equating Forces:** Since the gravitational force and the centripetal force are equal, we can equate the two equations above:
G * (m1 * m2) / r^2 = (m * v^2) / r
4. **Orbital Velocity:** We know that the orbital period (T) of a star is related to its orbital velocity (v) and the separation distance (r) by:
v = 2 * pi * r / T
5. **Solving for Mass:** By substituting the expression for orbital velocity into the equation for equal forces and rearranging, we can derive an equation to solve for the mass of one star (m1) in terms of the other star's mass (m2), the orbital period (T), and the separation distance (r):
m1 = (4 * pi^2 * r^3) / (G * T^2 * m2)
6. **Determining Both Masses:** To find the masses of both stars, we need one additional piece of information. This could be the ratio of their masses, or the observed motion of one star relative to the other.
By following these steps, using the known values for G, T, and r, and with the additional information about the stars' masses, we can calculate the individual masses of the stars in a binary system.
Comments