Atoms in the atmosphere of the star is responsible for the dark lines in its spectrum.
Not necessarily. The absence of specific spectral lines could be due to factors like the star's temperature, composition, or magnetic fields affecting the spectral lines. It could also be that the element is present in trace amounts that are not detectable in the spectrum.
Red shift would cause helium's Fraunhofer lines to shift towards the red end of the spectrum. This occurs because as the light from the helium source is redshifted, the wavelengths of the spectral lines observed would also increase, causing them to appear at longer wavelengths.
Its not. You can't see ultraviolet. (it lies just above the visible spectrum.)
The visible light spectrum is the part of the spectrum that can be separated into rainbow-like colors. This range of wavelengths extends from about 400 nanometers (violet) to 700 nanometers (red).
By looking at the lines in a star's spectrum of light, astronomers can tell what kinds of elements the star is made of. This happens because when a beam of light hits an atom or molecule, that atom absorbs a characteristic wavelength (color) of visible light. Scientists have made a huge list of different elements and the different patterns of lines observed in theirj corresponding "spectra" (fancy word for light spectrums), and by using such lists can deduce precisely what each star is made of.
Dark dust clouds primarily absorb and scatter visible light, hence appearing dark to us. They do not radiate strongly in the ultraviolet part of the electromagnetic spectrum.
The part of the electromagnetic spectrum that we can see is visible light. Visible light consists of the colors of the rainbow, ranging from violet at shorter wavelengths to red at longer wavelengths. This portion of the spectrum is detected by our eyes and is responsible for our sense of sight.
The emission spectrum of barium nitrate typically includes several bands of light in the visible region, with some lines in the blue-green part of the spectrum being the most prominent. The specific wavelengths and intensities of these lines can vary depending on the experimental conditions.
It is putting the light from the Sun or a star through a spectrograph, in other words a specially designed piece of equipment with a prism, to split it up into its different colours, red to violet. A spectrosope uses collimated light so that each 'colour' or wavelength arrives in its own measureable position on the spectrum. When that is done, a set of dark lines can be seen in the spectrum, each line corresponding to an element or compound in the source that provided the light. The sodium lines in the yellow part of the spectrum are a good example, and in the Sun's spectrum there are two dark lines close together in the yellow region, indicating that sodium is absorbing light in the outer layers of the Sun. This technique is used to analyse stars in great detail to discover their chemical makeup.
Not necessarily. The absence of specific spectral lines could be due to factors like the star's temperature, composition, or magnetic fields affecting the spectral lines. It could also be that the element is present in trace amounts that are not detectable in the spectrum.
Stroma is the site for dark reaction.It does not light.
The electromagnetic waves given off by high voltage power lines are beyond the visible part of the spectrum.
Radiant light energy refers to the energy carried by electromagnetic waves that are visible to the human eye. This energy is part of the electromagnetic spectrum and is responsible for the sensation of sight. It includes all the colors of light that we can perceive.
Heat from the sun is primarily felt as infrared radiation, which falls within the electromagnetic spectrum just below visible light. Infrared radiation is responsible for warming our skin and the Earth's surface.
It is unique to a specific atom. The emission spectrum of sodium, for example, has two characteristic lines close together in the yellow part of the spectrum, which cannot be found in any other atom. Each line in a spectrum relates to a change in electron state or level.
We call that the visible or optical spectrum.
The visible spectrum