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Research Notes of the American Astronomical Society. "The 2018 Census of Luminous Blue Variables in the Local Group". Monthly Notices of the Royal Astronomical Society. "Luminous blue variables are antisocial: Their isolation implies that they are kicked mass gainers in binary evolution".

^ Smith, Nathan Tombleson, Ryan (2015).

"Light variations of massive stars (alpha Cyg variables). "Constraining GRB progenitor models by probing Wolf-Rayet wind geometries in the Large Magellanic Cloud". Fundamental Properties and Evolutionary Status of Ofpe/WN9 Stars from HST Ultraviolet Observations".

^ a b Pasquali, Anna Langer, Norbert Schmutz, Werner Leitherer, Claus Nota, Antonella Hubeny, Ivan Moffat, Anthony F.

Publications of the Astronomical Society of the Pacific. "The Ofpe/WN9 class in the Large Magellanic Cloud". "Fundamental parameters of Wolf-Rayet stars. "Spectral classification of O and B0 supergiants in the Magellanic Clouds". "The Wolf-Rayet stars in the Large Magellanic Cloud". "A spectroscopic survey of WNL stars in the Large Magellanic Cloud: General properties and binary status". "S Doradus variables in the Galaxy and the Magellanic Clouds". CDS/ADC Collection of Electronic Catalogues. "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". "The Tycho-2 catalogue of the 2.5 million brightest stars". Others still list it only as a candidate. It has been classified as a luminous blue variable on account of the variability and spectrum, although it has never been observed in outburst. The colour also varies, with the star being bluer at minimum light.

R99 shows brightness variations of about 0.3 magnitude over a period of decades, and smaller amplitudes with the strongest periods at two and ten days. This has not been observed in other WR stars.

Significant polarisation of the spectrum continuum is also seen, suggesting an asymmetric wind. The normal temperature-stratified WR wind is accelerated to terminal velocity, causing lines of different ionisation levels of Helium to be created at different distances from the star. The wind structure of R99 may be significantly different from most WR stars and LBVs. R99 has significant differences from those other stars which preclude it being given a simple WN spectral type: the ultraviolet spectrum is strongly blanketed over a different range of wavelengths highly ionised iron lines are seen in absorption instead of emission the H i lines are unusually narrow and have no P Cygni profile a lack of any significant absorption features near H δ a number of metal lines are unusually strong or weak compared to other stars of the type there is a small unexplained infrared excess. The Ofpe/WN9 type remains even though other stars of this type have been reclassified to types between WN9 and WN11. R99 has a peculiar spectrum that has been described as OBf:pe, "unclassifiable", peculiar WN10, "similar to the unusual LBV HD 5980", "unique", and Ofpe/WN9. It is classified as a possible luminous blue variable and is one of the most luminous stars known. R99 (HD 269445) is a star in the Large Magellanic Cloud in the constellation Dorado.