61 Cygni // is a binary star system in the constellation Cygnus, consisting of a pair of K-type dwarf stars that orbit each other in a period of about 659 years. Of apparent magnitude 5.20 and 6.05, respectively, they can be seen with binoculars in city skies or with the naked eye in rural areas without light pollution.
Epoch J2000.0 Equinox J2000.0
|61 Cygni A|
|Right ascension||21h 06m 53.940s|
|Declination||+38° 44′ 57.90″|
|Apparent magnitude (V)||5.21|
|61 Cygni B|
|Right ascension||21h 06m 55.31s|
|Declination||+38° 44′ 31.4″|
|Apparent magnitude (V)||6.05|
|Spectral type||K5V / K7V|
|U−B color index||+1.155 / +1.242|
|B−V color index||+1.139 / +1.320|
|Variable type||A: BY Draconis|
B: Flare star
|Radial velocity (Rv)||-64.3/-63.5 km/s|
|Proper motion (μ)|| RA: 4156.93/|
|Parallax (π)||285.88 ± 0.54 mas|
|Distance||11.41 ± 0.02 ly |
(3.498 ± 0.007 pc)
|Absolute magnitude (MV)||7.506/8.228|
|61 Cygni A|
|Radius||0.665 ±0.005 R☉|
|Luminosity||0.153 ±0.01 L☉|
|Surface gravity (log g)||4.40 cgs|
|Temperature||4,526 ±66 K|
|Metallicity [Fe/H]||–0.20 dex|
|Age||6.1 ±1 Gyr|
|61 Cygni B|
|Radius||0.595 ±0.008 R☉|
|Luminosity||0.085 ±0.007 L☉|
|Surface gravity (log g)||4.20 cgs|
|Temperature||4,077 ±59 K|
|Metallicity [Fe/H]||–0.27 dex|
|Age||6.1 ±1 Gyr|
|Companion||61 Cygni B|
|Period (P)||678 ±34 yr|
|Semi-major axis (a)||24.272 ±0.592″|
|Eccentricity (e)||0.49 ±0.03|
|Inclination (i)||51 ±2°|
|Longitude of the node (Ω)||178 ±2°|
|Periastron epoch (T)||1709 ±16|
|Argument of periastron (ω)|
61 Cygni first attracted the attention of astronomers when its large proper motion was first demonstrated by Giuseppe Piazzi in 1804. In 1838, Friedrich Bessel measured its distance from Earth at about 10.4 light-years, very close to the actual value of about 11.4 light-years; this was the first distance estimate for any star other than the Sun, and first star to have its stellar parallax measured. Among all stars or stellar systems listed in the modern Hipparcos Catalogue, 61 Cygni has the seventh-highest proper motion, and the highest among all visible stars or systems.
Over the course of the twentieth century, several different astronomers reported evidence of a massive planet orbiting one of the two stars, but recent high-precision radial velocity observations have shown that all such claims were unfounded. No planets have been confirmed in this stellar system to date.
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".
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's repeated measurements led to a definitive value of its motion, which he published in 1804. It was in this record he christened the system as the "Flying Star".
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.
A number of astronomers soon took up the task, including attempts by François Arago and Claude-Louis Mathieu in 1812, who recorded the parallax at 500 milliarcseconds (mas), and Christian Heinrich Friedrich Peters used Arago's data to calculate a value of 550 mas. Peters calculated a better value based on observations made by Bernhard von Lindenau at Seeburg between 1812 and 1814; he calculated it to be 470 ±510 mas. Von Lindenau had already noted that he had seen no parallax, and as Friedrich Georg Wilhelm von Struve pointed out after his own test series between 1818 and 1821, all of these numbers are more accurate than the accuracy of the instrument used.
Friedrich Wilhelm Bessel made a notable contribution in 1812 when he used a different method to measure distance. Assuming the orbital period of the two stars in the binary to be 400 years, he estimated the distance between the two this would require, and then measured the angular distance between the stars. This led to a value of 460 mas. He then followed this up with direct parallax measurements in a series of observations between 1815 and 1816, comparing it with six other stars. The two sets of measurements produced values of 760 and 1320 mas. All of these estimates, like earlier attempts by others, retained inaccuracies greater than the measurements.
When Joseph von Fraunhofer invented a new type of heliometer, Bessel carried out another set of measurements using this device in 1837 and 1838 at Königsberg. He published his findings in 1838 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. This is close to the currently accepted value of 287.18 mas (yielding 11.36 light-years).
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 seventh highest proper motion of all stellar systems listed in the modern Hipparcos Catalogue, but retains the title of highest proper motion among visible stars.
Due to the wide angular separation between 61 Cygni A and B, and the correspondingly slow orbital motion, it was initially unclear whether the two stars in the 61 Cygni system were a gravitationally bound system or simply a juxtaposition of stars. von Struve first argued for its status as a binary in 1830, but the matter remained open.
However, by 1917 refined measured parallax differences demonstrated that the separation was significantly less. 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.
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.[note 1] 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.
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. The system has a net space velocity of 108 km/s relative to the Sun, which results in the high proper motion across the sky. 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. This system will make its closest approach at about 20,000 CE, when the separation from the Sun will be about 9 light-years. Smaller and dimmer than the Sun, 61 Cygni A has about 70 percent of a solar mass, 72 percent of its diameter and about 8.5 percent of its luminosity and 61 Cygni B has about 63 percent of a solar mass, 67 percent of its diameter, and 3.9 percent of its luminosity. 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. Starting in 1953, 61 Cygni B has been considered a K7 V standard star (Johnson & Morgan 1953, 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.[note 2] 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 A has about 11% more mass than 61 Cygni B.
The system has an activity cycle that is much more pronounced than the solar sunspot cycle. This is a complex activity cycle that varies with a period of about 7.5±1.7 years. The starspot activity combined with rotation and chromospheric activity is a characteristic of a BY Draconis variable. Because of differential rotation, this star's surface rotation period varies by latitude from 27 to 45 days, with an average period of 35 days.
The outflow of the stellar wind from component A produces a bubble within the local interstellar cloud. Along the direction of the star's motion within the Milky Way, this extends out to a distance of 30 AU, or roughly the orbital distance of Neptune from the Sun. This is lower than the separation between the two components of 61 Cygni, and so the two most likely do not share a common atmosphere. The compactness of the astrosphere is likely due to the low mass outflow and the relatively high velocity through the local interstellar medium.
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. Both stars exhibit stellar flare activity, but the chromosphere of B is 25% more active than for 61 Cygni A. 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.
There is some disagreement over the evolutionary age of this system. Kinematic data gives an age estimate of about 10 Gyr. Gyrochronology, or the age determination of a star based on its rotation and color, results in an average age of 2.0 ±0.2 Gyr. The ages based on chromospheric activity for A and B are 2.36 Gyr and 3.75 Gyr, respectively. Finally the age estimates using the isochrone method, which involve fitting the stars to evolutionary models, yield upper limits of 0.44 Gyr and 0.68 Gyr. However, a 2008 evolutionary model using the CESAM2k code from the Côte d'Azur Observatory gives an age estimate of 6.0 ±1.0 Gyr for the pair.
Claims of a planetary systemEdit
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.
Refining planetary boundariesEdit
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.
- Fischer, Mark (2019-02-09). "61 Cygni". Mark Fisher. Retrieved 2019-02-09.
- "61 Cygni". The Internet Stellar Database. 2011-04-04. Retrieved 2019-02-03. External link in
- Blanco, C.; Marilli, E.; Catalano, S. (1979-01-05). "Photoelectric observations of stars with variable H and K emission components. III". Astronomy and Astrophysics Supplement Series. 36: 297–306. Bibcode:1979A&AS...36..297B.
- "SIMBAD Query Result: V* V1803 Cyg -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2019-02-03. (61 Cygni A)
- "SIMBAD Query Result: NSV 13546 -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2019-02-03. (61 Cygni B)
- van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357
- Kovtyukh, V. V.; Soubiran, C., Belik, S. I.; Gorlova, N. I. (December 2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth", Astronomy and Astrophysics, 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378 See Mv values in Table 1, p. 9.
- Staff (2007-08-07), RECONS Mission Statement, Research Consortium on Nearby Stars, Georgia State University, archived from the original on 2012-01-01, retrieved 2019-02-11
- Kervella, P.; Mérand, A.; Pichon, B.; Thévenin, F.; Heiter, U.; Bigot, L.; Ten Brummelaar, T. A.; McAlister, H. A.; Ridgway, S. T.; Turner, N. (September 2008), "The radii of the nearby K5V and K7V stars 61 Cygni A & B. CHARA/FLUOR interferometry and CESAM2k modeling", Astronomy and Astrophysics, 488 (2): 667–674, arXiv:0806.4049, Bibcode:2008A&A...488..667K, doi:10.1051/0004-6361:200810080
- Luck, R. Earle; Heiter, Ulrike (2005), "Stars within 15 Parsecs: Abundances for a Northern Sample", The Astronomical Journal, 129 (2): 1063–1083, Bibcode:2005AJ....129.1063L, doi:10.1086/427250
- van Belle, Gerard T.; von Braun, Kaspar (2009), "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars", The Astrophysical Journal, 694 (2): 1085–109, arXiv:0901.1206, Bibcode:2009ApJ...694.1085V, doi:10.1088/0004-637X/694/2/1085
- Böhm-Vitense, Erika (March 2007), "Chromospheric Activity in G and K Main-Sequence Stars, and What It Tells Us about Stellar Dynamos", The Astrophysical Journal, 657 (1): 486–493, Bibcode:2007ApJ...657..486B, doi:10.1086/510482
- Hartkopf, W. I.; Mason, Brian D. "Sixth Catalog of Orbits of Visual Binary Stars". U.S. Naval Observatory. Retrieved 2008-07-12.
- "SIMBAD Query Result: ADS 14636 AB -- Double or multiple star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2019-02-03. (61 Cygni)
- Not to be confused with 16 Cygni, a more distant system containing two G-type stars harboring the gas giant planet 16 Cygni Bb.
- Staff (6 July 2007). "High Proper Motion Stars: Interesting Areas to View". ESA. Retrieved 2015-06-14.
- Wittenmyer, R. A.; Endl, M.; Cochran, W.D.; Hatzes , A.; Walker, G. A. H.; Yang, S. L. S.; Paulson, D. B. (2006). "Detection limits from the McDonald Observatory planet search program". Astronomical Journal. 132 (1): 177–188. arXiv:astro-ph/0604171. Bibcode:2006AJ....132..177W. doi:10.1086/504942.
- Allen, Richard Hinckley (2003). Star Names and Their Meanings. Kessinger. p. 219. ISBN 978076614028-8.
- Sun, Xiaochun; Kistemaker, Jacob (1997). The Chinese Sky During the Han: Constellating Stars and Society. Brill. Bibcode:1997csdh.book.....S. ISBN 9789004107373.
- "Naming Objects Outside the Solar System-Stars". IAU. Retrieved 2019-02-03.
- Kaler, Jim (2009-07-08). "61 Cygni". Stars. Retrieved 2019-02-03.
- Flamsteed, John (1725). Historia Coelestis Britannica. Meere. p. 5.
- Dibon-Smith, Richard (1998). The Flamsteed Collection. Clear Skies. p. xi.
- "61 Cyg (Piazzi's Flying Star)". Science&Space News. Retrieved 2019-02-03.
- Covington, Michael (2002-09-26). Celestial Objects for Modern Telescopes: Practical Amateur Astronomy. Cambridge University Press. ISBN 9780521524193.
- Hopkins, Mary Murray (1916-11-01). "The Parallax of 61 Cygni". Journal of the Royal Astronomical Society of Canada: 498–504.
- Piazzi, Giuseppe (1803). Præcipuarum stellarum inerrantium positiones mediae ineunte seculo XIX: ex observationibus habitis in specula Panormitana ab anno 1792 ad annum 1802. Typis regiis. p. 111.
- Fodera-Serio, G. (1990). "Giuseppe Piazzi and the Discovery of the Proper Motion of 61-Cygni". Journal for the History of Astronomy (in Latin). 21 (3): 275–282. Bibcode:1990JHA....21..275F. doi:10.1177/002182869002100302.
- Hirshfeld, Alan (2001). Parallax: The Race to Measure the Cosmos. Macmillan. ISBN 978-0716737117.
- Frommert, Hartmut; Kronberg, Christine. "Friedrich Wilhelm Bessel". Students for the Exploration and Development of Space. Archived from the original on 2012-02-04. Retrieved 2009-04-03.
- Hughes, Stefan (2012). Catchers of the Light. ArtDeCiel Publishing. p. 702. ISBN 9781620509616.
- Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen – Rath und Ritter Bessel" [Determining the distance of the 61st star of Cygnus. From Mr Geheimen, Rath and Ritter Bessel]. Astronomische Nachrichten (in German). 16 (5–6): 65–96. Bibcode:1838AN.....16...65B. doi:10.1002/asna.18390160502.
(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist
- Davis, Merhan S. (1898). "Remarks regarding the parallaxes of 61 Cygni and the probable physical connection of these two stars". Astrophysical Journal. 8: 246–247. Bibcode:1898ApJ.....8..246D. doi:10.1086/140527.
- Adams, W. S.; Joy, A. H. (1917). "The luminosities and parallaxes of five hundred stars". Astrophysical Journal. 46: 313–339. Bibcode:1917ApJ....46..313A. doi:10.1086/142369.—See Table I, page 326
- Baize, P. (1950). "Second catalogue d'orbites d'Etoiles Doubles visuelles" [Second catalog of orbits of visual double stars]. Journal des Observateurs (in French). 33: 1–31. Bibcode:1950JO.....33....1B.—on page 19, the authority is listed as Zagar (1934).
- Boss, Benjamin (1911). "Community of motion among several stars of large proper-motion". Astronomical Journal. 27 (629): 33–37. Bibcode:1911AJ.....27...33B. doi:10.1086/103931.
- Eggen, O. J. (1959). "White dwarf members of the 61 Cygni group". The Observatory. 79: 135–139. Bibcode:1959Obs....79..135E. – Gives space velocity components of U=+94, V=–53 and W=–7 for HD 201091/2.
- Sol Company. "System Summary Pi Mensae". Sol Company. Retrieved May 1, 2015.
- Howard, Andrew W.; Fulton, Benjamin J. (2016). "Limits on Planetary Companions from Doppler Surveys of Nearby Stars". Publications of the Astronomical Society of the Pacific. 128 (969). 114401. arXiv:1606.03134. Bibcode:2016PASP..128k4401H. doi:10.1088/1538-3873/128/969/114401.
- Espenak, Fred (1996-07-25). "Twelve Year Planetary Ephemeris: 1995–2006". NASA. Retrieved 2019-02-03.
- Adler, Alan (2006-07-26). "More Pretty Double Stars". SAT.com. Sky and Telescope. Retrieved 2019-02-03.
- Gudel, M. (1992). "Radio and X-ray emission from main-sequence K stars". Astronomy and Astrophysics. 264 (2): L31–L34. Bibcode:1992A&A...264L..31G.
- Eggen, Olin J. (October 1969), "Stellar Groups in the Old Disk Population", Publications of the Astronomical Society of the Pacific, 81 (482): 553, Bibcode:1969PASP...81..553E, doi:10.1086/128823
- Anonymous (2006-03-18). "Long-Term Stellar Motions, part 2: Shortcuts". The Astronomy Nexus. Archived from the original on 9 November 2007. Retrieved 2019-02-03.
- Affer, L.; Micela, G.; Morel, T.; Sanz-Forcada, J.; Favata, F. (2005). "Spectroscopic determination of photospheric parameters and chemical abundances of 6 K-type stars" (PDF). Astronomy and Astrophysics. 433 (2): 647–658. Bibcode:2005A&A...433..647A. doi:10.1051/0004-6361:20041308.
- Nave, Rod. "61 Cygni". HyperPhysics. Retrieved 2019-02-03.
- Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society, 25: 1319, Bibcode:1993AAS...183.1710G, retrieved 2012-02-04
- Johnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". Astrophysical Journal. 117: 313. Bibcode:1953ApJ...117..313J. doi:10.1086/145697.
- Keenan, P. C.; McNeil, R. C. (October 1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". Astrophysical Journal Supplement Series. 71: 245–266. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- "SIMBAD Query Result : HD 201092". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2019-02-03.
- Frick, P.; Baliunas, S. L.; Galyagin, D.; Sokoloff, D.; Soon, W. (1997). "Wavelet Analysis of Chromospheric Activity". Astrophysical Journal. 483 (1): 426–434. Bibcode:1997ApJ...483..426F. doi:10.1086/304206.
- Hempelmann, A.; Schmitt, J. H. M. M.; Baliunas, S. L.; Donahue, R. A. (2003). "Evidence for coronal activity cycles on 61 Cygni A and B". Astronomy and Astrophysics. 406 (2): L39–L42. Bibcode:2003A&A...406L..39H. doi:10.1051/0004-6361:20030882.
- Wood, Brian E.; Müller, Hans-Reinhard; Zank, Gary P.; Linsky, Jeffrey L. (July 2002). "Measured Mass-Loss Rates of Solar-like Stars as a Function of Age and Activity". The Astrophysical Journal. 574 (1): 412–425. arXiv:astro-ph/0203437. Bibcode:2002ApJ...574..412W. doi:10.1086/340797.
- Hempelmann, A.; Robrade, J.; Schmitt, J. H. M. M.; Favata, F.; Baliunas, S. L.; Hall, J. C. (2006). "Coronal activity cycles in 61 Cygni". Astronomy and Astrophysics. 460 (1): 261–267. Bibcode:2006A&A...460..261H. doi:10.1051/0004-6361:20065459.
- Barnes, Sydney A. (November 2007). "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors". The Astrophysical Journal. 669 (2): 1167–1189. arXiv:0704.3068. Bibcode:2007ApJ...669.1167B. doi:10.1086/519295.
- Strand, K. Aa. (1943). "61 Cygni as a Triple System". Publications of the Astronomical Society of the Pacific. 55 (322): 29–32. Bibcode:1943PASP...55...29S. doi:10.1086/125484.
- Darrell Schweitzer; Theodore Sturgeon; Alfred Bester (2009). Science Fiction Voices #1. Wildside Press LLC. p. 64. ISBN 9781434407849. Retrieved 2019-02-03.
- Strand, K. Aa. (1957). "The orbital motion of 61 Cygni". The Astronomical Journal. 62: 35. Bibcode:1957AJ.....62Q..35S. doi:10.1086/107588.
- Cumming, A.; Marcy, G. W.; Butler, R. P. (1999). "The Lick planet search: detectability and mass thresholds". Astrophysical Journal. 526 (2): 890–915. arXiv:astro-ph/9906466. Bibcode:1999ApJ...526..890C. doi:10.1086/308020.
- Deich, A. N. (1977). "Invisible companions of the binary star 61 Cygni". [Soviet Astronomy]. 21: 182–188. Bibcode:1977SvA....21..182D.
- Heintz, W. D. (1978). "Reexamination of suspected unresolved binaries". The Astrophysical Journal. 220: 931–934. Bibcode:1978ApJ...220..931H. doi:10.1086/155982.
- Walker, G. A. H.; Walker, A. R.; Irwin, A. W.; Larson, A. M.; Yang, S. L. S.; Richardson, D. C. (1995). "A search for Jupiter-mass companions to nearby stars". Icarus. 116 (2): 359–375. Bibcode:1995Icar..116..359W. doi:10.1006/icar.1995.1130.
- Cantrell, Justin R.; Henry, Todd J.; White, Russel J. (October 2013), "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors", The Astronomical Journal, 146 (4), p. 99, arXiv:1307.7038, Bibcode:2013AJ....146...99C, doi:10.1088/0004-6256/146/4/99
- Wittenmyer, R. A.; Endl, M.; Cochran, W.D.; Hatzes , A.; Walker, G. A. H.; Yang, S. L. S.; Paulson, D. B. (May 2006). "Detection Limits from the McDonald Observatory Planet Search Program". The Astronomical Journal. 132 (1): 177–188. arXiv:astro-ph/0604171. Bibcode:2006AJ....132..177W. doi:10.1086/504942.
- McCarthy, Christopher (2005). "SIM Planet Search Tier 1 Target Stars". San Francisco State University. Archived from the original on 2007-08-04. Retrieved 2007-07-23.
- Kuchner, Marc J.; Brown, Michael E.; Koresko, Chris D. (1998). "An 11.6 Micron Keck Search for Exo-Zodiacal Dust". The Publications of the Astronomical Society of the Pacific. 110 (753): 1336–1341. arXiv:astro-ph/0002040. Bibcode:1998PASP..110.1336K. doi:10.1086/316267.
- Millan-Gabet, R.; Serabyn, E.; Mennesson, B.; Traub, W. A.; Barry, R. K.; Danchi, W. C.; Kuchner, M.; Stark, C. C.; Ragland, S.; Hrynevych, M.; Woillez, J.; Stapelfeldt, K.; Bryden, G.; Colavita, M. M.; Booth, A. J. (June 2011), "Exozodiacal Dust Levels for Nearby Main-sequence Stars: A Survey with the Keck Interferometer", The Astrophysical Journal, 734 (1): 67, arXiv:1104.1382, Bibcode:2011ApJ...734...67M, doi:10.1088/0004-637X/734/1/67. See Table 5, p. 58.