Bohr's Atomic Model and Spectra

The video explores the evolution of atomic models, starting with the Rutherford and Thompson models, which left unresolved issues regarding electron stability. It introduces the concept of electrons orbiting the nucleus, akin to planets around the sun, and discusses the implications of classical electromagnetic theory. The video delves into spectral lines, highlighting Balmer's work on hydrogen, and explains Bohr's quantized momentum theory, which introduced quantum numbers and energy levels. Bohr's model provided insights into atomic spectra and had significant applications in astronomy, though it left some questions unanswered, such as the stability of electron orbits.

What was the main issue with the Rutherford model of the atom?

• It didn't include neutrons.

• It couldn't explain why electrons don't fall into the nucleus.

• It didn't account for the mass of the atom.

• It couldn't explain the stability of the nucleus.

How was the problem of electron collapse initially addressed?

• By suggesting electrons repel the nucleus.

• By assuming electrons are stationary.

• By proposing electrons orbit the nucleus.

• By introducing neutrons.

What does classical electromagnetic theory predict about accelerating charges?

• They gain energy.

• They remain stable.

• They become stationary.

• They radiate energy.

Who developed mathematical relationships for hydrogen spectral lines?

• Albert Einstein

• Ernest Rutherford

• Niels Bohr

• Johann Balmer

What did Niels Bohr introduce to explain atomic structure?

• Electromagnetic waves

• Classical mechanics

• Quantized momentum theory

• A new element

What happens when an electron absorbs a photon with matching energy?

• The electron jumps to a higher energy level.

• The electron jumps to a lower energy level.

• The electron emits light.

• The electron remains in the same shell.

What did Bohr's model help explain in terms of hydrogen spectra?

• The Doppler effect

• The Rutherford model

• The Balmer series

• The photoelectric effect

How can we determine the composition of a star?

• By measuring its temperature

• By analyzing its absorption lines

• By observing its brightness

• By calculating its mass

What astronomical phenomenon can be measured using spectral lines?

• Star brightness

• Star size

• Star temperature

• Star radial velocities

What was a significant limitation of Bohr's model?

• It couldn't explain why electrons don't radiate energy.

• It didn't include protons.

• It couldn't explain the mass of the atom.

• It didn't account for electron spin.