Balmer lines
... The emission from stars is quite similar to the emission from black bodies. Generally, dense opaque objects behave approximately like black bodies. The energy emitted per square metre from the surface of a black body is E = T4 A sphere with a radius of r has a surface area of 4 r2, so a spherical bl ...
... The emission from stars is quite similar to the emission from black bodies. Generally, dense opaque objects behave approximately like black bodies. The energy emitted per square metre from the surface of a black body is E = T4 A sphere with a radius of r has a surface area of 4 r2, so a spherical bl ...
Light, spectra, Doppler shifts
... the substance. As long as the temperature is above absolute zero (-273 deg C = 0 degrees Kelvin), the substance also gives off light. In fact, it gives off light at all wavelengths. This is called continuous radiation, also known as black body radiation. What color such a substance appears to be dep ...
... the substance. As long as the temperature is above absolute zero (-273 deg C = 0 degrees Kelvin), the substance also gives off light. In fact, it gives off light at all wavelengths. This is called continuous radiation, also known as black body radiation. What color such a substance appears to be dep ...
Neon Sodium Mercury Helium Argon
... • Hotter objects emit more total radiation per unit area. • Hotter objects emit photons with a higher average energy. • Thermal Radiation (BB) is an example of “continuum emission”. ...
... • Hotter objects emit more total radiation per unit area. • Hotter objects emit photons with a higher average energy. • Thermal Radiation (BB) is an example of “continuum emission”. ...
The Relationship Between a Star`s Color, Temperature, and
... by a hot object and its temperature. • By “main” color, I mean the peak wavelength, called λmax , at the top of the Planck Curve. ...
... by a hot object and its temperature. • By “main” color, I mean the peak wavelength, called λmax , at the top of the Planck Curve. ...
Black body
A black body (also blackbody) is an idealized physical body that absorbs all incident electromagnetic radiation, regardless of frequency or angle of incidence. A white body is one with a ""rough surface [that] reflects all incident rays completely and uniformly in all directions.""A black body in thermal equilibrium (that is, at a constant temperature) emits electromagnetic radiation called black-body radiation. The radiation is emitted according to Planck's law, meaning that it has a spectrum that is determined by the temperature alone (see figure at right), not by the body's shape or composition.A black body in thermal equilibrium has two notable properties:It is an ideal emitter: at every frequency, it emits as much energy as – or more energy than – any other body at the same temperature.It is a diffuse emitter: the energy is radiated isotropically, independent of direction.An approximate realization of a black surface is a hole in the wall of a large enclosure (see below). Any light entering the hole is reflected indefinitely or absorbed inside and is unlikely to re-emerge, making the hole a nearly perfect absorber. The radiation confined in such an enclosure may or may not be in thermal equilibrium, depending upon the nature of the walls and the other contents of the enclosure.Real materials emit energy at a fraction—called the emissivity—of black-body energy levels. By definition, a black body in thermal equilibrium has an emissivity of ε = 1.0. A source with lower emissivity independent of frequency often is referred to as a gray body.Construction of black bodies with emissivity as close to one as possible remains a topic of current interest.In astronomy, the radiation from stars and planets is sometimes characterized in terms of an effective temperature, the temperature of a black body that would emit the same total flux of electromagnetic energy.