The binary system has an
orbital period of 129 days. The primary, component Aa, is a
Be star that is surrounded by ionized gas that is producing the
emission lines in the spectrum. This circumstellar shell is inclined by 80° to the line of sight from the Earth.[6] The system is undergoing both short term and long term variations in luminosity, with the short period variations showing a phase cycle of 1.03 days.[4] It is classified as a
Gamma Cassiopeiae variable with an amplitude of 0.16 in magnitude.[4]
The system has two visual companions. Component B is a visual magnitude 10.11 star at an
angular separation of 65.8
arc seconds along a
position angle of 46°, as of 2013. Component C with visual magnitude of 14.1 lies at an angular separation of 62.7 arc seconds along a position angle of 164°, as of 1999.[12] Both stars are likely to be unrelated and at different distances to Epsilon Capricorni.[16]
^
abAdelman, S. J.; et al. (December 2000), "On the Variability of O4-B5 Luminosity Class III-V Stars", Information Bulletin on Variable Stars, 5008 (5008): 1,
Bibcode:
2000IBVS.5008....1A.
^
abcBalona, L. A. (December 2002), "Short period spectral variability in the Be stars I: eta Centauri and epsilon Capricorni", The Journal of Astronomical Data, 8: 1,
Bibcode:
2002JAD.....8....1B.
^Kostjuk, N. D. (2004), "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)", VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002), 4027,
Bibcode:
2004yCat.4027....0K.