RW Cygni is a semiregular variable star in the constellation Cygnus, about a degree east of 2nd magnitude γ Cygni. Its apparent magnitude varies between 8.05 and 9.70 and its spectral type between M3 and M4.
The Gaia Data Release 2 parallax for RW Cyg is or a distance of around . RW Cygni is assumed to be a member of the Cygnus OB9 stellar association and therefore around 3,600 light-years from the Solar System.[1] Newer observations based on the parallaxes of neighbouring OB stars give RW Cygni a distance of .
RW Cygni is a luminous red supergiant with a bolometric luminosity more than . Its spectral type is given in the General Catalogue of Variable Stars as M2-4Ia-Iab, covering the range of previously published values. It has been defined as a standard star for the MK spectral classification of M3-M4Ia-Iab. In 2005, the effective temperature is directly calculated to be 3,600 K, giving a radius of . An alternate calculation gives a higher temperature of 3,920 K and a correspondingly lower radius of . A newer measurement based on its angular diameter and is Gaia Data Release 2 parallax give it a larger radius of, which would make RW Cygni one of the largest known stars. Using the more conservative figure, if it was placed at the center of Solar System, it would be extend past the orbit of Mars and into the asteroid belt.
The initial mass of RW Cygni has been estimated from its position relative to theoretical stellar evolutionary tracks to be around . Observations of its atmosphere suggest that it is losing mass at a rate of per year.[2]
RW Cygni is classified as a semiregular variable star. It is given the subtype SRc, indicating that it is a cool supergiant. Its brightness varies from extremes of magnitude +8.0 and +9.5 with a period of . No long secondary period has been detected.[3]