Thespectrum of Psi9 Aurigae matches agiant star with astellar classification of B8 IIIe.[3] The 'e' suffix indicates this is aBe star that shows emission lines of hydrogen in its spectrum. This is caused by acircumstellar shell of hot gas. The emission undergoes variability on a time scale of sixteen years.[3]
^abcGhosh, K. K. (September 1989), "Search for rapid spectral variability in Psi(9) Aurigae",Publications of the Astronomical Society of the Pacific,101:839–843,Bibcode:1989PASP..101..839G,doi:10.1086/132504.
^abCrawford, D. L. (February 1963), "U, b, v, and Hβ Photometry for the Bright B8- and B9-TYPE Stars",Astrophysical Journal,137: 530,Bibcode:1963ApJ...137..530C,doi:10.1086/147526.
^Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities",Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington,Bibcode:1953GCRV..C......0W.