Changes

==The Star==

==The Star==

Pollux is a orange-red giant with a spectral classification of K0 IIIb.  The [[star]] is 8.8 times the diameter of our [[Sun]].  However like all giants, it has a low mass - being only 1.7 times as massive as our own star.<ref>http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2000ApJ...528..885A&db_key=AST&data_type=HTML&format=&high=44a287269c18839</ref>  Pollux is 32 times as visually luminous as our Sun, with a total luminosity 46 times as great when accounting for the [[infrared]].  As a cooler class K giant, Pollux has a surface temperature of around 4770 K.<ref>http://stars.astro.illinois.edu/sow/pollux.html</ref>  The star has a [[metallicity]] (abundance of elements heavier then [[hydrogen]] and [[helium]]) between 85 and 155 percent of that of our Sun, based on the abundance of iron measured.<ref>http://www.solstation.com/stars2/pollux.htm</ref>  

Pollux is an orange-red giant with a spectral classification of K0 IIIb.  The [[star]] is 8.8 times the diameter of our [[Sun]].  However like all giants, it has a low mass - being only 1.7 times as massive as our own star.<ref>http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2000ApJ...528..885A&db_key=AST&data_type=HTML&format=&high=44a287269c18839</ref>  Pollux is 32 times as visually luminous as our Sun, with a total luminosity 46 times as great when accounting for the [[infrared]].  As a cooler class K giant, Pollux has a surface temperature of around 4770 K.<ref>http://stars.astro.illinois.edu/sow/pollux.html</ref>  The star has a [[metallicity]] (abundance of elements heavier then [[hydrogen]] and [[helium]]) between 85 and 155 percent of that of our Sun, based on the abundance of iron measured.<ref>http://www.solstation.com/stars2/pollux.htm</ref>  

The star itself has used up all its core hydrogen fuel and has shifted to fusing helium in its core to [[carbon]] and [[oxygen]].  This lose of mass will puff out from the star as a planetary nebula, consisting mostly of hydrogen and helium, with some heavier elements (such as carbon and oxygen).  Once this occurs, the resultant left over star will be a [[white dwarf]].

The star itself has used up all its core hydrogen fuel and has shifted to fusing helium in its core to [[carbon]] and [[oxygen]].  This lose of mass will puff out from the star as a planetary nebula, consisting mostly of hydrogen and helium, with some heavier elements (such as carbon and oxygen).  Once this occurs, the resultant left over star will be a [[white dwarf]].