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RS Cancri

RS Cancri, also known as HR 3639 and HD 78712, is a star about 490 light years from the Earth in the constellation Cancer. It is a semiregular variable star, ranging in brightness from magnitude 5.4 to 7.3 over a period of about 229 days. During the time intervals when it is brighter than magnitude 6, it may be faintly visible to the naked eye of an observer far from city lights.

The variability of RS Cancri was discovered by Edward Pickering based upon 15 observations made in 1892 and 1898. S. Seliwanow derived a period of 129.5 days for the star, in 1923.^[8] In 2005, Saul Adelman and John Dennis found that the star showed two periods well determined by their data, 121.8±0.9 and 248±7 days, as well as a poorly-determined third period of about 500 days.^[9]

RS Cancri is an S-type star,^[4] on the asymptotic giant branch.^[10] Its spectrum shows technetium, implying the star has undegone the third dredge-up.^[11] RS Cancri has a stellar wind, and is losing mass at a rate of 1.7 × 10⁻⁷ solar masses per year.^[5]

RS Cancri has a circumstellar shell. It is a good target for studies of such a shell, because its rather high galactic latitude (+42 degrees) means that it is cleanly separated from the interstellar dust and gas seen along most lines of sight through the galactic plane. Dust within the shell produces far-infrared continuum emission that was resolvedbyIRAS.^[12] Both atomic and molecular gas within the shell are also measurably extended, and have been mapped.^[5]

The extensive molecular envelope surrounding RS Cancri was first detected in 1977, by Kwok-Yung (Fred) Lo and Kenneth Bechis, who used the 36 foot radio telescopeonKitt Peak to detect the J=1-0 lineofcarbon monoxide (CO).^[13] Years later, when observations of spectral lines could be made with more sensitive equipment, it was noticed that the shapes of the spectral lines suggested that RS Cancri has two distinct stellar wind components, expanding into space at different speeds.^[14] Interferometric observations have shown that the two winds consist of a ~2 km/sec wind arising from an equatorial disk within the envelope, and an ~8 km/sec bipolar wind.^[15] In subsequent decades, additional molecules such as SiO, SO, SO₂, H₂O HCN and PN have been detected.^[6]