It merely means that the amount of this element in the visible part of a star - the part that emits the spectrum - is too small to be detected by this method.
spectral analysis of light of stars help us
Yes.
You can conclude that it is farther than a certain distance. How much this distance is depends, of course, on how accurately the parallax angle can be measured.
The gas absorbs certain frequencies of light, producing an absorption spectrum.
Spectrometers are used for this. By looking at the spectrum of light coming from the star, scientists can tell which elements are in the star by the pattern of lines that are known to be associated with certain elements.
In accoustic measurements, spectral mean refers to the center of gravity for a certain sound wave selection.
'Astronomical spectrum' is not a specific term. I suspect you are thinking of the emission spectrum of a star, which can tell us a great deal about the composition of the star. Light and other radiations from the object are spread out into constituent wavelengths and dark lines appear across the spectrum at certain specific wavelengths which are characteristic of elements present.
The energy levels of the atom; from which when the atom is in an exited state and drops down in to a lower energy level it releases a quanta (packet) of energy which is of a certain frequency, this is then related to the colour of the light released.
spectral analysis of light of stars help us
White light is a mix of different frequencies; with certain equipment, it is possible to separate it into its components. This separated version is called a "spectrum".White light is a mix of different frequencies; with certain equipment, it is possible to separate it into its components. This separated version is called a "spectrum".White light is a mix of different frequencies; with certain equipment, it is possible to separate it into its components. This separated version is called a "spectrum".White light is a mix of different frequencies; with certain equipment, it is possible to separate it into its components. This separated version is called a "spectrum".
In theory, hydrogen has infinitely many spectral lines. The "Balmer series" has four lines in the visible spectrum; additional lines are in the ultraviolet. Other "series" have other lines - it seems that all of them are either in the ultraviolet or infrared. For more information, read the Wikipedia article on "Hydrogen spectrum". The reason there are four VISIBLE lines is basically chance - an excited hydrogen atom emits light at certain frequencies (which can be calculated, see the article for more details); our eyes see a certain range of electromagnetic waves that happens to include four of those lines.
Yes.
That's a certain breed characteristic.
Spectral lines tell us how many different energy levels an atom has, and how far apart those energy levels are spaced. This is possible because spectral lines are the result of an excess (emission lines) or deficiency (absorption lines) of observed photons emitted from certain types of matter. The lines are caused by electrons moving between energy levels within individual atoms. Since each element emits it's own unique spectrum, this means that different types of atoms must have a distinct number of electrons in very particular energy levels.
electromagnetic spectrum
The difference between continuous spectrum and the atomic emission espectrum of an element is that in emission spectrum, only certain specific frequencies of light are emitted while in a continuous spectrum, a continuous range of colors are seen in the visible light.
You may want to refine the question. Red shift is the systematic shift of spectral lines from very distant cosmic sources toward the red end of the spectrum. It seems to derive primarily from the Doppler effect, so one might say that it is Dopplered toward the red. I can think of no other specific name for it, so am not certain what you are asking.