V1429 Aquilae

V1429 Aql has a peculiar spectrum dominated by emission lines of hydrogen and many ionised metals, with Fe being particularly strong and numerous. There are also comparatively weak forbidden lines, primarily [Fe], but also [N]. Some absorption lines are present, but are either very weak or hidden by the emission. Many lines have variable profiles, particularly the hydrogen and helium series which vary during the orbit from emission to P Cygni profiles. The absorption lines are considered to be formed in the photosphere of the primary star, although some Fe absorption appears to be from gas between the stars. No lines of the secondary can be detected. The emission lines are formed in circumstellar material between and around the two stars Overall, the spectral type is given as B3 Ibe. In infrared spectra, the Pfund series of lines are strongly in emission, a very unusual feature characteristic of supergiant Be stars and LBVs. V1429 Aql is given a B2:e spectral type from analysis in the infrared. ==System==

V1429 Aquilae is a single-lined spectroscopic binary. The existence of a companion is inferred from the highly periodic variations in the radial velocity of its spectral lines and by equally periodic variations in brightness and spectral line profiles. It is unclear whether there are partial eclipses of the larger star or just of gas surrounding the stars. The orbital period is well-defined at 60.7 days and it is moderately eccentric (0.244). The primary star fills its roche lobe for at least part of the orbit. The other characteristics of the orbit are disputed. The orbital velocity of the secondary is unknown, and the possible inclinations do not sufficiently restrict the possible models of the system. Assumptions based on broadly similar data produce wildly different results for the masses of the stars, from to for the primary. A third star is visible in infrared images just over one arc second away. It is statistically likely to be in a wide orbit around the spectroscopic pair, about 5,700 AU away. The system contains material being transferred from the primary to the secondary star as well as material surrounding both stars. A dense clump of gas near the centre of mass of the system, and co-rotating with the stars, produces the bulk of the emission lines. A more diffuse region of gas surrounds both stars and produces some absorption components in the spectrum. The entire system is surrounded by a shell of material about 0.8 parsecs across, assuming that MWC 314 is 3,000 parsecs away. This appears in infrared images as a circular ring 25 arc-seconds from the central star. There is a much larger bipolar nebula detected by its Hα radiation. It is 13 parsecs from end to end. ==Variability==

The variability of V1429 Aquilae's brightness was first reported by Anatoly S. Miroshnichenko in 1996, based on photometry undertaken from 1990 through 1995. It was given its variable star designation in 1997. V1429 Aquilae shows brightness variations of about 0.3 magnitudes and a detectable period of 4.16 days. No longterm variations in brightness have been detected over several decades of observations. The profiles of many spectral lines also vary with the same period, produced partly by radial velocity variations. The absorption and emission lines show different radial velocity amplitudes, but with the same period. Most of these variations can be accounted for by the orbit of the two stars and material being transferred from the primary to the secondary, with the gas being involved in partial eclipses, and possibly also partial eclipses of the stars themselves. The two stars are also distorted into ellipsoidal shapes by their gravity and vary in brightness as they rotate. In addition to the orbital variations, two pulsation modes have been observed with amplitudes of a few thousandths of a magnitude and periods of 0.77 and 1.42 days. ==Physical properties==

Estimates of the distance of V1429 Aquilae made by indirect methods range between 2.4 == References ==