CPD−57°2874 is surrounded by a disc of expelled stellar material. The inner edge of the disc is 27.5 AU from the star and it is inclined at an angle of 46° to us. The particular alignment, temperature, and density of the disc combine to produce the forbidden spectral lines. The detached ring leads to speculation that the inner regions are cleared by an unseen binary companion.[5]
Photometry of CPD−57°2874 suggests that it is variable with an amplitude of perhaps 0.2 magnitude. It has not been formally classified as a variable star and the cause of the variations is unclear.[5]
^ abcdHog, E.; Kuzmin, A.; Bastian, U.; Fabricius, C.; Kuimov, K.; Lindegren, L.; Makarov, V. V.; Roeser, S. (1998). "The TYCHO Reference Catalogue". Astronomy and Astrophysics. 335: L65. Bibcode:1998A&A...335L..65H.
^ abcdefDomiciano De Souza, A.; Driebe, T.; Chesneau, O.; Hofmann, K.-H.; Kraus, S.; Miroshnichenko, A. S.; Ohnaka, K.; Petrov, R. G.; Preisbisch, T.; Stee, P.; Weigelt, G.; Lisi, F.; Malbet, F.; Richichi, A. (2007). "AMBER/VLTI and MIDI/VLTI spectro-interferometric observations of the B[e] supergiant CPD-57°2874. Size and geometry of the circumstellar envelope in the near- and mid-IR". Astronomy and Astrophysics. 464: 81. arXiv:astro-ph/0510735. Bibcode:2007A&A...464...81D. doi:10.1051/0004-6361:20054134. S2CID7829778.
^Drilling, J. S. (1991). "UBV photometry of OB+ stars in the southern Milky Way". Astrophysical Journal Supplement Series. 76: 1033. Bibcode:1991ApJS...76.1033D. doi:10.1086/191588.
^Fernandes, M. Borges (2010). "The Nature Of Stars With The B[e] Phenomenon Through Interferometric Eyes". Revista Mexicana de Astronomía y Astrofísica, Serie de Conferencias. 38: 98–99. Bibcode:2010RMxAC..38...98B.
^F. Malbet; et al. (2007). "In The Intimacy Of Stars With Amber At The VLTI". SF2A: 2. Bibcode:2007sf2a.conf...13M.
