编辑“︁WOH G64”︁（章节）

=== 光譜特徵 ===
WOH G64被發現是[[羥自由基|OH]]、[[水]]和{{chem|link=一氧化矽|SiO}} [[天文物理邁射]]發射源，這是 [[OH/IR星|OH/IR超巨星]]的典型特徵<ref name=levesque/>。它顯示了不尋常的星雲發射[[光譜]]；熱氣體富含氮，其[[徑向速度]]比恆星的正值大得多<ref name=levesque/>。恆星大氣在中紅外波長中產生強矽酸鹽[[吸收帶]]，並伴有由於高激發的[[一氧化碳]]而產生的線發射<ref>{{Cite journal |last1=Matsuura |first1=Mikako |last2=Sargent |first2=B. |last3=Swinyard |first3=Bruce |last4=Yates |first4=Jeremy |last5=Royer |first5=P. |last6=Barlow |first6=M. J. |last7=Boyer |first7=Martha |last8=Decin |first8=L. |last9=Khouri |first9=Theo |last10=Meixner |first10=Margaret |last11=van Loon |first11=Jacco Th. |last12=Woods |first12=Paul M. |date=1 November 2016 |title=The mass-loss rates of red supergiants at low metallicity: detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=462 |issue=3 |pages=2995–3005 |doi=10.1093/mnras/stw1853 |doi-access=free |issn=0035-8711|arxiv=1608.01729 }}</ref>。