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Variable star
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=====Long secondary period variables===== {{Main|Long-period variable star#Long secondary periods}} Many variable red giants and supergiants show variations over several hundred to several thousand days. The brightness may change by several magnitudes although it is often much smaller, with the more rapid primary variations are superimposed. The reasons for this type of variation are not clearly understood, being variously ascribed to pulsations, binarity, and stellar rotation.<ref name=messina>{{cite journal|bibcode=2007NewA...12..556M|title=Evidence for the pulsational origin of the Long Secondary Periods: The red supergiant star V424 Lac (HD 216946)|journal=New Astronomy|volume=12|issue=7|pages=556–561|last1=Messina|first1=Sergio|year=2007|doi=10.1016/j.newast.2007.04.002}}</ref><ref>{{cite journal|bibcode=2007ApJ...660.1486S|arxiv=astro-ph/0701463|title=Long Secondary Periods and Binarity in Red Giant Stars|journal=The Astrophysical Journal|volume=660|issue=2|pages=1486–1491|last1=Soszyński|first1=I.|year=2007|doi=10.1086/513012|s2cid=2445038}}</ref><ref>{{cite journal|bibcode=2003ApJ...584.1035O|title=On the Origin of Long Secondary Periods in Semiregular Variables|journal=The Astrophysical Journal|volume=584|issue=2|pages=1035|last1=Olivier|first1=E. A.|last2=Wood|first2=P. R.|year=2003|doi=10.1086/345715|citeseerx=10.1.1.514.3679|s2cid=40373007 }}</ref>
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