61 Cygni

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61 Cygni

Expanded view of the star field around 61 Cygni. This system is located at the end of the arrow above.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
61 Cygni A
Right ascension 21h 06m 53.9434s1
Declination +38° 44′ 57.898″1
Apparent magnitude (V) 5.211
61 Cygni B
Right ascension 21h 06m 55.2648s2
Declination +38° 44′ 31.400″2
Apparent magnitude (V) 6.032
Characteristics
Spectral type K5V1 / K7V2
U-B color index +1.155 / +1.2423
B-V color index +1.139 / +1.3203
Variable type A: BY Draconis1
B: Flare star2
Astrometry
Radial velocity (Rv) -64.31/-63.52 km/s
Proper motion (μ) RA: 4156.931/
 4109.172 mas/yr
Dec.: 3259.391/
 3144.172 mas/yr
Parallax (π) 287.18 ± 1.511 mas
Distance 11.36 ± 0.06 ly
(3.48 ± 0.02 pc)
Absolute magnitude (MV) 7.48/8.33
Details
61 Cygni A
Mass 0.704 M☉
Radius 0.725 R☉
Surface gravity (log g) 4.406
Luminosity 0.085 L☉
Temperature 4,6406 K
Metallicity [Fe/H] = -0.206
Rotation 377
Age ~10108 years
61 Cygni B
Mass 0.634 M☉
Radius 0.675 R☉
Surface gravity (log g) 4.206
Luminosity 0.039 L☉
Temperature 4,640/4,4406 K
Metallicity [Fe/H] = -0.276
Orbit9
Companion 61 Cygni B
Period (P) 678 ± 34 yr
Semimajor 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)
(secondary)		 149 ± 6°
Other designations

61 Cygni,note 1 sometimes called Bessel's Star10 or Piazzi's Flying Star,11 is a binary star system in the constellation Cygnus. It consists of a pair of K-type dwarf stars that orbit each other in a period of about 659 years, forming a visual binary. At fifth and sixth apparent magnitudes, they are among the least conspicuous stars visible in the night sky to an observer without an optical instrument.

61 Cygni first attracted the attention of astronomers because of its large proper motion. In 1838, Friedrich Wilhelm 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.12 Over the course of the twentieth century, several different astronomers reported detections of a massive planet orbiting one of the two stars, but recent high-precision radial velocity observations have shown that all such claims were erroneous.131415 To date, no planets have been confirmed in this system.

Contents

Observation history

The large proper motion of 61 Cygni was first demonstrated by Giuseppe Piazzi in 1804, who christened it the "Flying Star".11 Piazzi's result, however, received little attention at the time due to the relatively short time span of his observations—a mere 10 years. It would take a publication by Friedrich Wilhelm Bessel in 1812 to bring this star to the widespread attention of astronomers.16

Friedrich Georg Wilhelm von Struve first argued for its status as a binary in 1830. For many years thereafter, however, some uncertainty remained as to whether this pair was a mere juxtaposition of stars or a gravitationally bound system.17

The system's large proper motion, the largest known for any star at the time, made 61 Cygni a candidate for the determination of its distance by the method of parallax when the quality of astronomical observations first made this possible. The system therefore has the distinction of being the first star (excluding the Sun) to have its distance from Earth measured. This was accomplished in 1838 by Bessel, who arrived at a parallax of 313.6 mas, close to the currently accepted value of 287.18 mas (yielding 11.36 light years).18

Only a few years later, however, Groombridge 1830 was discovered to have a larger proper motion. 61 Cygni retains the distinction of having the largest proper motion of any star visible to the unaided eye (although Groombridge 1830 at magnitude 6.4 can be seen with the naked eye under exceptionally dark skies). It has the seventh highest proper motion of all stellar systems listed in the Hipparcos Catalogue.19

By 1911 Bessel's parallax of 0.3136 had only slightly improved to 0.310, and observations at Yerkes Observatory had measured its radial velocity as 62 km/s20 which together with its proper motion—transverse to our line of sight—of around 79 km/s yielded a space velocity of about 100 km/s towards a point about 12 degrees west of Orion's belt.note 2note 3

In 1911, Benjamin Boss published data indicating that the 61 Cygni system was a member of a comoving group of stars.20 This was group later expanded to include 26 potential members. Possible members include Beta Columbae, Pi Mensae, 14 Taurus and 68 Virginis. The typical space velocities of this group of stars is 105–114 km/s relative to the Sun. 21

Because of their wide angular separation (and correspondingly slow orbital motion), it was initially unclear whether the two stars in this system were physically connected. The respective parallax measurements of 0.360″ and 0.288″ gave a separation of more than two light years.22 However, by 1917 refined measured parallax differences demonstrated that the separation was significantly less.23. The binary nature of this system was clear by 1934, and orbital elements were published.24

Properties

Although it appears to be a single star to the naked eye, 61 Cygni is in fact a widely separated binary system, composed of two K class (orange) main sequence stars, 61 Cygni A and 61 Cygni B. The brighter star 61 Cygni A is of apparent magnitude 5.2, the fainter 61 Cygni B is 6.1. Both appear to be old disk stars,25 with an estimated age that is older than the Sun. The system has a net space velocity of 108 km/s26 relative to the Sun, which results in the high proper motion across the sky.8 At a distance of just over 11 light years, it is one of the nearest star systems to the Earth.4 This system will make its closest approach at about 20,000 CE, when the separation from the Sun will be about 9 light years.26

A size comparison between the Sun (left), 61 Cygni A (bottom) and 61 Cygni B (upper right).

The two orbit their common barycenter in a period of 659 years, with a mean separation of about 84 A.U.—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 A.U. at periapsis and 124 A.U. at apoapsis.note 4

Component A is the slightly more massive of the pair. It 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.27 (An earlier estimate gave a period of 7.3 years.)28 The combination of starspot activity combined with rotation and chromospheric activity is characteristic of a BY Draconis variable.

Component 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.28 Both stars exhibit stellar flare activity, but the chromosphere of component B is 25% more active than for component A.29

An observer using 7×50 binoculars can find 61 Cygni two binocular fields south-east of the bright star Deneb. The angular separation of the two stars is slightly greater than the angular size of Saturn (16–20″).30 So, under ideal seeing conditions, the binary system can be resolved by a telescope with a 6 mm aperture.note 5 This is well within the capability of a typical pair of binoculars.

Possible low-mass companions

On several occasions it has been claimed that 61 Cygni has unseen low-mass companions, planets or a brown dwarf. Kaj Strand 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 was orbiting 61 Cygni A.31 In 1957 additional data allowed him to narrow his uncertainties, claiming that the object appeared to have about eight times the mass of Jupiter. With a calculated orbital period of 4.8 years, the estimated semi-major axis of 2.4 A.U.32 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.33 In 1978 Wulff Dieter Heintz suggested these claims were "spurious", having failed 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.34

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.35 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 A.U. from the star. Measurements of this system 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 yet been resolved with a telescope.36

See also

Notes

  1. ^ Not be confused with 16 Cygni, a more distant system containing two G-type stars harboring the gas giant planet 16 Cygni Bb.
  2. ^ The space velocity calculated from 1911 data: parallax 310 mas yields 10.5 light years; total proper motion= 5.205 arcsec/year (average by mass) or 79.4 km/s; and radial velocity = -62 km/s.
  3. ^ This yields a 1911 space velocity of \begin{smallmatrix}\sqrt{79.4^2\ +\ 62^2}\ =\ 100\end{smallmatrix} km/s. Compare with more accurate 1953, 1997 data: parallax 287.18 yields 11.36 ly and so an increased proper motion velocity of 87km/s; radial velocity -64km/s yields a net space velocity of \begin{smallmatrix}\sqrt{87^2\ +\ 64^2}\ =\ 106\end{smallmatrix} km/s.
  4. ^ At periapsis: \begin{smallmatrix}r_{per}\ =\ (1\ -\ e)\cdot a\ \approx\ 44\end{smallmatrix} A.U.
    At apoasis: \begin{smallmatrix}r_{ap}\ =\ (1\ +\ e)\cdot a\ \approx\ 124\end{smallmatrix} A.U.
  5. ^ Per the Rayleigh criterion: \begin{smallmatrix}\alpha_R\ =\ \frac{138}{D}\end{smallmatrix} mm.

References

  1. ^ a b c d e f g h i j "SIMBAD Query Result: V* V1803 Cyg -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved on 2007-07-15. (61 Cygni A)
  2. ^ a b c d e f g h i "SIMBAD Query Result: NSV 13546 -- Flare Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved on 2007-07-15. (61 Cygni B)
  3. ^ a b Blanco, C.; Marilli, E.; Catalano, S. (1979). "Photoelectric observations of stars with variable H and K emission components. III". Astronomy and Astrophysics Supplement Series 36: 297–306, http://adsabs.harvard.edu/abs/1979A%26AS...36..297B. Retrieved on 4 February 2007. 
  4. ^ a b c Staff (June 8, 2007). "List of the Nearest 100 Stellar Systems". Research Consortium on Nearby Stars, Georgia State University. Retrieved on 2007-07-15.
  5. ^ a b Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". Astrophysical Journal Supplement Series 53: 643–711. doi:10.1086/190905, http://adsabs.harvard.edu/abs/1983ApJS...53..643J. Retrieved on 5 September 2007. 
  6. ^ a b c d e f Luck, R. Earle; Heiter, Ulrike (2005). "Stars within 15 Parsecs: Abundances for a Northern Sample". The Astronomical Journal 129 (2): 1063–1083. doi:10.1086/427250, http://adsabs.harvard.edu/abs/2005AJ....129.1063L. Retrieved on 17 July 2007. 
  7. ^ Dorren, J. D.; Guinan, E. F. (1982). "Evidence for starspots on single solar-like stars". Astrophysical Journal 87: 1546–1557. doi:10.1086/113245, http://adsabs.harvard.edu/abs/1982AJ.....87.1546D. Retrieved on 15 July 2007. 
  8. ^ a b 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". Astronomy and Astrophysics 433 (2): 647–658. doi:10.1051/0004-6361:20041308, http://adsabs.harvard.edu/abs/2005A&A...433..647A. Retrieved on 25 July 2007. 
  9. ^ Hartkopf, W. I.; Brian D. Mason, B. D.. "Sixth Catalog of Orbits of Visual Binary Stars". U.S. Naval Observatory. Retrieved on 2008-07-12.
  10. ^ Pannekoek, Anton (1989). A History of Astronomy, Courier Dover Publications. pp.343. ISBN 0486659941. 
  11. ^ a b Hirshfeld, Alan (2001). Parallax: The Race to Measure the Cosmos, Macmillan. ISBN 0716737116. 
  12. ^ Friedrich Wilhelm Bessel, at http://www.seds.org/MESSIER/xtra/Bios/bessel.html.
  13. ^ Walker GAH, Walker AR, Irwin AW, Larson AM, Yang SLS, Richardson DC. (1995) A search for Jupiter-mass companions to nearby stars. Icarus, 116 (2) 359-375. Abstract at http://adsabs.harvard.edu/abs/1995Icar..116..359W.
  14. ^ Cumming A, Marcy GW, Butler RP. (1999) The Lick planet search: detectability and mass thresholds. Astrophysical Journal, 526: 890-915. Abstract at http://adsabs.harvard.edu/abs/1999ApJ...526..890C.
  15. ^ Wittenmyer RA, Endl M, Cochran WD, Hatzes A, Walker GAH, Yang SLS, Paulson DB.(2006) Detection limits from the McDonald Observatory planet search program. Astronomical Journal, 132: 177–188. Abstract at http://adsabs.harvard.edu/abs/2006AJ....132..177W.
  16. ^ Fodera-Serio, G. (1990). "Giuseppe Piazzi and the Discovery of the Proper Motion of 61-Cygni". Journal of the History of Astronomy 21 (3): 275, http://adsabs.harvard.edu/abs/1990JHA....21..275F. Retrieved on 14 July 2007. 
  17. ^ 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. doi:10.1086/140527, http://adsabs.harvard.edu/abs/1898ApJ.....8..246D. Retrieved on 15 July 2007. 
  18. ^ Bessel, F. W. (1839). "Bestimmung der Entfernung des 61sten Sterns des Schwans. Von Herrn Geheimen - Rath und Ritter Bessel" (in German). Astronomische Nachrichten 16: 65, http://adsabs.harvard.edu/abs/1839AN.....16...65B. Retrieved on 17 July 2007. "(page 92) Ich bin daher der Meinung, daß nur die jährliche Parallaxe = 0"3136 als das Resultat der bisherigen Beobachtungen zu betrachten ist".  A parallax of 313.6 mas yields a distance of 10.4 light years
  19. ^ Staff (May 4, 2007). "High Proper Motion Stars: Interesting Areas to View". ESA. Retrieved on 2007-07-16.
  20. ^ a b Boss, Benjamin (1911). "Community of motion among several stars of large proper-motion". Astronomical Journal 27 (629): 33–37. doi:10.1086/103931, http://adsabs.harvard.edu/abs/1911AJ.....27...33B. Retrieved on 17 July 2007. 
  21. ^ Eggen, O. J. (1959). "White dwarf members of the 61 Cygni group". The Observatory 79: 135–139, http://adsabs.harvard.edu/abs/1959Obs....79..135E. Retrieved on 17 July 2007.  – Gives space velocity components of U=+94, V=-53 and W=-7 for HD 201091/2.
  22. ^ Davis, H. S. (1898). "Remarks regarding the parallaxes of 61 Cygni and the probable physical connection of these two stars". Astrophysical Journal 61 (2): 246–247. doi:10.1086/140527, http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1898ApJ.....8..246D. Retrieved on 11 September 2007. 
  23. ^ Adams, W. S.; Joy, A. H. (1917). "The luminosities and parallaxes of five hundred stars". Astrophysical Journal 46: 313–339. doi:10.1086/142369, http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1917ApJ....46..313A&db_key=AST&nosetcookie=1. Retrieved on 11 September 2007. —See Table I, page 326
  24. ^ Baize, P. (1950). "Second catalogue d'orbites d'Etoiles Doubles visuelles" (in French). Journal des Observateurs 33: 1–31, http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1917ApJ....46..313A&db_key=AST&nosetcookie=1. Retrieved on 11 September 2007. —on page 19, the authority is listed as Zagar (1934).
  25. ^ Gudel, M. (1992). "Radio and X-ray emission from main-sequence K stars". Astronomy and Astrophysics 264 (2): L31–L34, http://adsabs.harvard.edu/abs/1992A&A...264L..31G. Retrieved on 16 July 2007. 
  26. ^ a b Anonymous (March 18, 2006). "Long-Term Stellar Motions, part 2: Shortcuts". The Astronomy Nexus. Retrieved on 2007-10-21.
  27. ^ Frick, P.; Baliunas, S. L.; Galyagin, D.; Sokoloff, D.; Soon, W. (1997). "Wavelet Analysis of Chromospheric Activity". Astrophysical Journal 483: 426–434. doi:10.1086/304206, http://adsabs.harvard.edu/abs/1997ApJ...483..426F. Retrieved on 15 July 2007. 
  28. ^ a b 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: L39–L42. doi:10.1051/0004-6361:20030882, http://adsabs.harvard.edu/abs/2003A&A...406L..39H. Retrieved on 15 July 2007. 
  29. ^ 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. doi:10.1051/0004-6361:20065459, http://adsabs.harvard.edu/abs/2006A&A...460..261H. Retrieved on 16 July 2007. 
  30. ^ Espenak, Fred (July 25, 1996). "Twelve Year Planetary Ephemeris: 1995 - 2006". NASA. Retrieved on 2007-07-25.
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  32. ^ Strand, K. Aa. (1957). "The orbital motion of 61 Cygni.". Astronomical Journal 62: 35. doi:10.1086/107588, http://adsabs.harvard.edu/abs/1957AJ.....62Q..35S. Retrieved on 15 July 2007. 
  33. ^ Asimov, Isaac (1981). Extraterrestrial Civilizations. London: Pan Books Ltd. ISBN 0330262491. 
  34. ^ Heintz, W. D. (1978). "Reexamination of suspected unresolved binaries". Astrophysical Journal 220: 931–934. doi:10.1086/155982, http://adsabs.harvard.edu/abs/1978ApJ...220..931H. Retrieved on 15 July 2007. 
  35. ^ "SIM Planet Search Tier 1 Target Stars". San Francisco State University. Retrieved on 2007-07-23.
  36. ^ 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. doi:10.1086/316267, http://adsabs.harvard.edu/cgi-bin/bib_query?1998PASP..110.1336K. Retrieved on 25 July 2007. 

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