## Astronomy Chapter 6 Flashcards

6,000 K If the temperature of star B is twice the temperature of star A, what can we say about the energy emitted by the surface of star B compared to the energy emitted by star A? Each square meter emits sixteen times as much energy per second. Which subatomic particle has a negative charge? electron.

## Astronomy Exam 2 Flashcards

Which electron energy level transition corresponds to a hydrogen atom absorbing a visible light photon that has a wavelength of 656 nanometers? The electron makes the transition from energy level 2 to energy level 3. which subatomic particle has a negative charge? electron.

## Homework #6 Solutions Astronomy 10, Section 2 due: Monday

To solve this problem, we use Wienʼs Law of Blackbody Radiation, namely that the product of the peak wavelength and the temperature is a constant. λ × T = 3 × max 106 3 106 λ = 3 × 106 = × = 150 nm max T 20,000 3) Infrared observations of a star show that it is most intense at a wavelength of 2000 nm.

## Blackbody radiation

Black-body radiation is the thermal electromagnetic radiation within, or surrounding, a body in thermodynamic equilibrium with its environment, emitted by a black body (an idealized opaque, non-reflective body).

## The Electromagnetic Spectrum

Electromagnetic radiation with wavelengths between roughly 400 and 700 nm is called visible light because these are the waves that human vision can perceive. This is also the band of the electromagnetic spectrum that most readily reaches Earth’s surface.

## Chapter 3 The Mechanisms of Electromagnetic Emissions

But the peak amount of energy is radiated at shorter wavelengths for higher temperatures. This relationship is known as Wien’s Law. A beam of electromagnetic radiation can be regarded as a stream of tiny packets of energy called photons. Planck’s Law states that the energy carried by a photon is directly proportional to its frequency.

## Stefan

The Stefan–Boltzmann law, also known as Stefan’s law, describes the intensity of the thermal radiation emitted by matter in terms of that matter’s temperature. It is named for Josef Stefan, who empirically derived the relationship, and Ludwig Boltzmann who derived the law theoretically.

## Blackbody Radiation

Here, L is the luminosity (energy per unit time) and R is the radius of the sphere. The second of the two properties listed above is referred to as Wien’s Law. To determine the peak wavelength of the spectrum of a blackbody, the equation is: λ m a x = (0.29 c m K) / T This equation is not rendering properly due to an incompatible browser. See.

## Radiation

The Sun radiates like a perfect black body with an emissivity of exactly 1. (a) Calculate the surface temperature of the Sun, given that it is a sphere with a 7.00 × 10 8-m radius that radiates 3.80 × 10 26 W into 3-K space. (b) How much power does the Sun radiate per square meter of its surface?

## Astro Chapters 6

The amount of electromagnetic energy radiated from every square meter of the surface of a black body each second is which of the following? proportional to temperature to the fourth power Which electron energy level transition corresponds to a hydrogen atom absorbing a visible light photon that has a wavelength of 656 nanometers?