WY Velorum

Early publications in 1928 and 1939 classified the star as a possible R Coronae Borealis variable. Later authors were split on whether it was a symbiotic star or a VV Cephei-type star. The two differ in that the former consists of a red giant and a white dwarf or neutron star, while the latter is usually composed of a K- or M-type RSG and a massive early B-type star. The latter was confirmed to be the case in a 1988 paper, and the companion was identified as a giant star with the spectral type B2. This study also presented the absolute magnitudes of the two stars, −4.8 for the primary and −1.7 for the secondary, albeit this has been calculated using a distance of 1400 pc, smaller than modern estimates. With an updated value of 1900 pc, its KS band absolute magnitude is gauged at −11.3. No radial velocity variations have been detected, so the binary likely has a small orbital inclination. ==Spectrum==

The star has a peculiar spectrum, as indicated by the "pe" suffix in the spectral type (the "p" stands for peculiar, and the "e" stands for emission lines). It displays various strong emission lines, namely of hydrogen, nitrogen, oxygen, silicon, sulfur, iron, nickel, copper, and possibly chromium, many of them forbidden lines. Among them, the strong [Fe II] (forbidden line of singly ionized iron) emission is particularly unusual. Its spectral peculiarities are so unique that astronomer William P. Bidelman could identify the star by merely looking at the spectrum. However, in the ultraviolet region, as observed by the International Ultraviolet Explorer, it only shows the emission lines for Mg II (Mg+). In this regard, it is similar to the symbiotic star CH Cygni, except that CH Cygni also has neutral oxygen lines. Excess infrared emission signifies the existence of circumstellar dust at a temperature of . The spectrum does not appear to be reddened. ==Historical observations==

s for WY Velorum. The upper plot, of ASAS-SN data, shows the variability on the timescale of months. The lower plot, of AAVSO data, shows the variability on the timescale of years. The purple dots show the yearly averages. The star's variability was first discovered by Annie Jump Cannon. Between 1890 and 1901, the brightness gradually increased from magnitude 9.8 to 9.2, but it slowly dimmed since 1902 to reach magnitude 10.1 by May 1922. Additional research on the light curves published in 1947 by Cecilia Payne-Gaposchkin indicate that the fading that began in 1902 halted around 1916, after which the star remained almost constant until 1933, when it began to brighten again. No discernible changes occurred in the spectrum of the star between 1944 and 1948, but in 1952, the H-α line shifted from a single line to a double line, and previously unseen faint H-β features appeared. In 1956, it was reported that the calcium H and K lines swung from absorption to emission during two consecutive nights. By 1969, the RSG had likely become fainter than it was in the 1940s. ==References==