61 Cygni

61 Cygni is relatively dim, so it does not appear on ancient star maps, nor is it given a name in western or Chinese systems. The name "61 Cygni" is part of the Flamsteed designation assigned to stars. According to this designation scheme, devised by John Flamsteed to catalog his observations, stars of a particular constellation are numbered in the order of their right ascension, not in Greek letters as the Bayer designation does. The star does not appear under that name in Flamsteed's Historia Coelestis Britannica, although it has been stated by him that 61 Cygni actually corresponds to what he referred to as 85 Cygni in the 1712 edition. It has also been called "Bessel's Star" or "Piazzi's Flying Star". == Observation history ==

Early observations The first well recorded observation of the star system using optical instruments was made by James Bradley on 25 September 1753, when he noticed that it was a double star. William Herschel began systematic observations of 61 Cygni as part of a wider study of binary stars. His observations led to the conclusion that binary stars were separated enough that they would show different movements in parallax over the year, and hoped to use this as a way to measure the distance to the stars. In 1792, Giuseppe Piazzi noticed the high proper motion when he compared his own observations of 61 Cygni with those of Bradley, made 40 years earlier. This led to considerable interest in 61 Cygni by contemporary astronomers, and its continual observation since that date. Piazzi noted that this motion meant that it was probably one of the closest stars, and suggested it would be a prime candidate for an attempt to determine its distance through parallax measurements, along with two other possibilities, Delta Eridani and Mu Cassiopeiae. with a value of 369.0 ±19.1 mas to A and 260.5 ±18.8 to B, and estimated the center point to be at 313.6 ±13.6. This corresponds to a distance of about 600,000 astronomical units, or about 10.4 light-years. This was the first direct and reliable measurement of the distance to a star other than the Sun. His measurement was published only shortly before similar parallax measurements of Vega by Friedrich Georg Wilhelm von Struve and Alpha Centauri by Thomas Henderson that same year. Bessel continued to make additional measurements at Königsberg, publishing a total of four complete observational runs, the last in 1868. The best of these placed the center point at 360.2 ±12.1 mas, made during observations in 1849. Only a few years after Bessel's measurement, in 1842 Friedrich Wilhelm Argelander noted that Groombridge 1830 had an even larger proper motion, and 61 Cygni became the second highest known. It was later moved further down the list by Kapteyn's Star and Barnard's Star. 61 Cygni has the sixth highest proper motion of all stellar systems listed in the latest Gaia catalogues, but retains the title of highest proper motion among stars visible to the naked eye. von Struve first argued for its status as a binary in 1830, but the matter remained open. The binary nature of this system was clear by 1934, and orbital elements were published. In 1911, Benjamin Boss published data indicating that the 61 Cygni system was a member of a comoving group of stars. This group containing 61 Cygni was later expanded to include 26 potential members. Possible members include Beta Columbae, Pi Mensae, 14 Tauri and 68 Virginis. The space velocities of this group of stars range from 105 to 114 km/s relative to the Sun. Observations taken by planet search programs show that both components have strong linear trends in the radial velocity measurements. == Amateur observation ==

An observer using 7×50 binoculars can find 61 Cygni two binocular fields southeast of the bright star Deneb. The angular separation of the two stars is slightly greater than the angular size of Saturn (16–20″). So, under ideal viewing conditions, the binary system can be resolved by a telescope with a 7 mm aperture. This is well within the capability for aperture of typical binoculars, though to resolve the binary these need a steady mount and some 10x magnification. With a separation of 28 arc-seconds between the component stars, 10× magnification would give an apparent separation of 280 arc-seconds, above the generally regarded eye resolution limit of 4 arc-minutes or 240 arc-seconds. == Properties ==

Although it appears to be a single star to the naked eye, 61 Cygni is a widely-separated binary star system, composed of two K class (orange) main sequence stars, the brighter 61 Cygni A and fainter 61 Cygni B, which have apparent magnitudes of 5.2 and 6.1, respectively. Both appear to be old-disk stars, with an estimated age that is older than the Sun. At a distance of just over 11 light-years, it is the 15th-nearest-known star system to the Earth (not including the Sun). 61 Cygni A is the fourth-nearest star that is visible to the naked eye for mid-latitude northern observers, after Sirius, Epsilon Eridani, and Procyon A. 61 Cygni A's long-term stability led to it being selected as an "anchor star" in the Morgan–Keenan (MK) classification system in 1943, serving as the K5 V "anchor point" since that time. Keenan & McNeil 1989). 61 Cygni A is a typical BY Draconis variable star designated as V1803 Cyg while 61 Cygni B is a flare type variable star named HD 201092 with their magnitudes varying 5.21 V and 6.03, respectively. The two stars orbit their common barycenter in a period of 659 years, with a mean separation of about 84 AU—84 times the separation between the Earth and the Sun. The relatively large orbital eccentricity of 0.48 means that the two stars are separated by about 44 AU at periapsis and 124 AU at apoapsis. The leisurely orbit of the pair has made it difficult to pin down their respective masses, and the accuracy of these values remain somewhat controversial. In the future this issue may be resolved through the use of asteroseismology. 61 Cygni B displays a more chaotic pattern of variability than A, with significant short-term flares. There is an 11.7-year periodicity to the overall activity cycle of B. As a result of differential rotation, the period of rotation varies by latitude from 32 to 47 days, with an average period of 38 days. However, a 2008 evolutionary model using the CESAM2k code from the Côte d'Azur Observatory gives an age estimate of for the pair. == Claims of a planetary system ==

On different occasions, it has been claimed that 61 Cygni might have unseen low-mass companions, planets or a brown dwarf. Kaj Strand of the Sproul Observatory, under the direction of Peter van de Kamp, made the first such claim in 1942 using observations to detect tiny but systematic variations in the orbital motions of 61 Cygni A and B. These perturbations suggested that a third body of about 16 Jupiter masses must be orbiting 61 Cygni A. Reports of this third body served as inspiration for Hal Clement's 1953 science fiction novel Mission of Gravity. In 1957, van de Kamp narrowed his uncertainties, claiming that the object had a mass of eight times that of Jupiter, a calculated orbital period of 4.8 years, and a semi-major axis of 2.4 AU, where 1 AU is the average distance from the Earth to the Sun. In 1977, Soviet astronomers at the Pulkovo Observatory near Saint Petersburg suggested that the system included three planets: two giant planets with six and twelve Jupiter masses around 61 Cyg A, and one giant planet with seven Jupiter masses around 61 Cygni B. In 1978, Wulff-Dieter Heintz of the Sproul Observatory proved that these claims were spurious, as they were unable to detect any evidence of such motion down to six percent of the Sun's mass—equivalent to about 60 times the mass of Jupiter. In 2018, analysis of the DR2 data gathered by the Gaia space telescope revealed significant proper motion anomalies in the orbits of the binary stars around each other; the stars were not quite orbiting around their centre of mass with 61 Cygni B also orbiting too slowly for its assumed mass. These anomalies taken together are indicative of the possible presence of a perturbing third object in orbit around 61 Cygni B. However, subsequent works found the astrometric data of the two stars to be consistent with a binary system with no third body. Refining planetary boundaries Since no certain planetary object has been detected around either star so far, McDonald Observatory team has set limits to the presence of one or more planets around 61 Cygni A and 61 Cygni B with masses between 0.07 and 2.1 Jupiter masses and average separations spanning between 0.05 and 5.2 AU. Because of the proximity of this system to the Sun, it is a frequent target of interest for astronomers. Both stars were selected by NASA as "Tier 1" targets for the proposed optical Space Interferometry Mission. This mission is potentially capable of detecting planets with as little as 3 times the mass of the Earth at an orbital distance of 2 AU from the star. Measurements of this system appeared to have detected an excess of far infrared radiation, beyond what is emitted by the stars. Such an excess is sometimes associated with a disk of dust, but in this case it lies sufficiently close to one or both of the stars that it has not been resolved with a telescope. A 2011 study using the Keck Interferometer Nuller failed to detect any exozodiacal dust around 61 Cygni A. Object for biosignature research The two stars are among five (all nearby star) paradigms listed among those K-type stars of a type in a 'sweet spot' between Sun-analog stars and M stars for the likelihood of evolved life, per analysis of Giada Arney from NASA's Goddard Space Flight Center. == See also ==