Titlebook: Spectroscopy: The Key to the Stars; Reading the Lines in Keith Robinson Book 2007 Springer-Verlag New York 2007 Galaxy.Planet.book about sp

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TRACE

,Cool but not Smooth—The Molecular Spectra of Red Stars, cool giant often of spectral class M. The continuum in the vicinity of the Hα line was seemingly very ‘noisy’ in one or two of the spectra which I was using and I remember someone at the time commenting that perhaps all the myriad spikes and dips weren’t in fact instrumental noise but the titanium

nominal

,Glows in the Dark—Emission Lines and Nebulae,tars like Wolf- Rayet stars and symbiotic stars together with Mira variables do produce emission lines in their spectra. However, the best place to introduce our emission line studies is gaseous nebulae and planetary nebulae; their spectra consist almost exclusively of emission lines. They have also

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,Glowing Vortices—Accretion Disks,active galactic nuclei. They are also believed to form within many interacting binary stars; particularly cataclysmic variables or CVs. What’s perhaps not quite so well known is that the hot gases which make up an accretion disk can produce emission lines of hydrogen and what’s more these emission l

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,Spectral Magnetism—The Zeeman Effect,y all played with a compass too and perhaps like the young Albert Einstein were mystified as to how the needle kept pointing in the same direction no matter which way we turned the compass. Magnetic fields are produced by electric currents or flows of electric charge; the outer or optically active e

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Counteract

Our Old Friend the Doppler Effect, we shall see in the next chapter this most valuable of effects plays a big role in spectra too; first though for completeness I shall explain it here and we’ll also have a look at how important the ‘clever astronomer’s’ relativistic version of the Doppler effect really is.

终止

,Glows in the Dark—Emission Lines and Nebulae, been for many years now, great favourites with deep sky observers and so there is inevitably going to be great interest among amateur spectroscopists who want to know how these beautiful objects work.

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FLAT

When Is a Spectral Line Not a Spectral Line?,nes connected by less dark regions. A spectral line clearly isn’t just a simple infinitely narrow line; the answer to the question posed in the title of this chapter is— ‘when it is a .’. All spectral lines have a line profile; in older books it was also sometimes referred to as the line contour.