Talk:Am star

From Wikipedia, the free encyclopedia
Jump to: navigation, search
WikiProject Astronomy / Astronomical objects  (Rated Start-class, Mid-importance)
WikiProject icon Am star is within the scope of WikiProject Astronomy, which collaborates on articles related to Astronomy on Wikipedia.
Start-Class article Start  This article has been rated as Start-Class on the project's quality scale.
 Mid  This article has been rated as Mid-importance on the project's importance scale.
Taskforce icon
This article is supported by WikiProject Astronomical objects, which collaborates on articles related to astronomical objects.


Just a note before authoring it into the article:

Am stars are sometimes classfied acc2 the scheme kSP1hSP2mSP3 and similar, f.ex. HD 159560 is of type kA3hA7mF2 = Am(A3/A7/F2). These k h m have eluded me for a couple of years, but the links explain that k a.k.a. K is really CaII K-line, h a.k.a. H is really Hydrogen Balmer lines, and m a.k.a. M is really "metallic lines". Since Am stars are slow rotators, their "surfaces" have a uniform temperature in comparison to f.ex. the fast rotator standard star Vega, who have a non-uniform surface temperature. The said paper calls Vega abnormal, and the Am stars normal, which is kind of easy to understand. The so called peculiar spectra of Am stars have a tripartite spectrum version to classify them, although this kind of spectrum would also be applicable to any A to early F star. ... said: Rursus (bork²) 09:16, 13 January 2009 (UTC)

  • page 171 tells us that Vega α Lyr and α Dra are underabundant in MgII.
... said: Rursus (bork²) 09:35, 13 January 2009 (UTC)