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In observational astronomy, a double star is a pair of stars which appear to lie close together in the sky. This can happen either because the pair forms a binary system of stars in mutual orbit, gravitationally bound to each other, or because it is an optical double, a chance alignment of two stars in the sky that lie at different distances.12
Since the beginning of the 1780s, both professional and amateur double star observers have telescopically measured the distances and angles between double stars to determine the relative motions of the pairs.3 If the relative motion of a pair determines a curved arc of an orbit, or if the relative motion is small compared to the common proper motion of both stars, it may be concluded that the pair is in mutual orbit as a binary star. Otherwise, the pair is optical.2 Multiple stars are also studied in this way, although the dynamics of multiple stellar systems are more complex than those of binary stars.
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History
Mizar, in the Big Dipper (Ursa Major), was observed to be double by Giovanni Battista Riccioli in 165014 (and probably earlier by Benedetto Castelli and Galileo).5 The bright southern star Acrux, in the Southern Cross, was discovered to be double by Father Fontenay in 1685.1 Since that time, the search has been carried out thoroughly and the entire sky has been examined for double stars down to a limiting apparent magnitude of about 9.0.6 At least 1 in 18 stars brighter than 9.0 magnitude in the northern half of the sky are known to be double stars visible with a 36-inch (910 mm) telescope.7
Observation
Visual double stars can be defined as those double stars which are visible in an optical telescope. This is the majority of known double stars.8 If visual doubles show similar properties, such as similar proper motion through space, trigonometric parallaxes, or radial velocities, this is evidence that they are gravitationally attached and form a binary system; in this case, the visual double star is called a visual binary.82
Telescopic observation of a visual double star will yield the separation, or angular distance, between the two component stars in the sky and the position angle. The position angle specifies the direction in which the stars are separated and is defined as the bearing from the brighter component to the fainter, where north is 0°.9 These measurements are called measures. In the measures of a visual binary, the position angle will change progressively and the separation between the two stars will oscillate between maximum and minimum values. Plotting the measures in the plane will produce an ellipse. This is the apparent orbit, the projection of the orbit of the two stars onto the plane of the sky; the true orbit can be computed from it.10 Although it is expected that the majority of catalogued visual doubles are visual binaries,8 orbits have been computed for only a few thousand of the over 100,000 known visual double stars.1112
Visual double stars can also be optical doubles, two stars that appear to be close together by chance. These pairs are actually separated by a great distance in space and are not gravitationally bound to each other, but happen to lie in the same line-of-sight when viewed from the Earth. Optical doubles may be distinguished from binary stars by observing their relative motion. If the motion is part of an orbit, or if the stars have similar radial velocities and the difference in their proper motions is small compared to their common proper motion, the pair is probably physical. When observed over a short period of time, the components of both optical doubles and long-period visual binaries will appear to be moving in straight lines; for this reason, it can be difficult to distinguish between these two possibilities.13
Designations
Some bright visual double stars have a Bayer designation. In this case, the components may be denoted by superscripts. An example of this is α Crucis (Acrux), whose components are α1 Crucis and α2 Crucis. Since α1 Crucis is a spectroscopic binary, this is actually a multiple star. Superscripts are also used to distinguish more distant, physically unrelated, pairs of stars with the same Bayer designation, such as α1,2 Capricorni (separated by 0.11°), ξ1,2 Centauri (separated by 0.66°), and ξ1,2 Sagittarii (separated by 0.46°.) These optical pairs are resolvable by the naked eye.
Apart from these pairs, the components of a double star are generally denoted by the letters A (for the brighter, primary, star) and B (for the fainter, secondary, star) appended to the designation, of whatever sort, of the double star. For example, the components of α Canis Majoris (Sirius) are α Canis Majoris A and α Canis Majoris B; the components of 44 Boötis are 44 Boötis A and 44 Boötis B; the components of ADS 16402 are ADS 16402A and ADS 16402B; and so on. The letters AB may be used together to designate the pair. In the case of multiple stars, the letters C, D, and so on may be used to denote additional components, often in order of increasing separation from the brightest star, A.14
| Discoverer | Traditional code | WDS code |
|---|---|---|
| Brisbane Observatory | Brs0 | BSO |
| S. W. Burnham | β | BU |
| James Dunlop | Δ | DUN |
| William Herschel | H I, II, etc. | H 1, 2, etc. |
| N. Lacaille | Lac | LCL |
| F. G. W. Struve | Σ | STF |
| Struve Appendix Catalogue I | Σ I | STFA |
| Struve Appendix Catalogue I | Σ II | STFB |
| Otto Struve | OΣ | STT |
| Pulkova Appendix Catalogue | OΣΣ | STTA |
Visual doubles are also designated by an abbreviation for the name of their discoverer followed by a catalogue number unique to that observer. For example, the pair α Centauri AB was discovered by Father Richaud in 1689, and so is designated RHD 1.116 Other examples include Δ65, the 65th double discovered by James Dunlop, and Σ2451, discovered by F. G. W. Struve.
The Washington Double Star Catalog, a large database of double and multiple stars, currently contains over 100,000 entries,11 each of which gives measures for the separation of two components. Each double star forms one entry in the catalog; multiple stars with n components will be represented by entries in the catalog for n−1 pairs, each giving the separation of one component of the multiple star from another. Codes such as AC are used to denote which components are being measured—in this case, component C relative to component A. This may be altered to a form such as AB-D to indicate the separation of a component from a close pair of components (in this case, component D relative to the pair AB.) Codes such as Aa may also be used to denote a component which is being measured relative to another component, A in this case.17 Discoverer designations are also listed; however, traditional discoverer abbreviations such as Δ and Σ have been encoded into a string of uppercase Roman letters, so that, for example, Δ65 has become DUN 65 and Σ2451 has become STF2451. Further examples of this are shown in the table to the right.1815
Examples
Visual binaries
- Alpha Centauri AB
- Sirius AB
- Procyon AB
- Capella AB
- p Eridani
- Polaris or α Ursa Minor is α UMi
- Acrux or α Crucis or α Cru
Optical doubles
Uncertain
- Alpha Centauri system (A and B) or α Centauri AB (visual binary), while the visual pair Proxima Centauri (= Alpha Centauri C) association is generally considered likely.
- Castor system (Aa/Ab/Ba/Bb and YY Geminorum (= Castor Ca/Cb?) All generally considered likely.
- Mizar system (Aa/Ab/Ba/Bb) and Alcor (= Mizar C) Component "C" is generally considered unlikely. (optical double)
See also
References
- ^ a b c d The Binary Stars, Robert Grant Aitken, New York: Dover, 1964, p. 1.
- ^ a b c Heintz, W. D. (1978). Double Stars. D. Reidel Publishing Company, Dordrecht. p. 17. ISBN 9027708851.
- ^ Heintz, W. D. (1978). Double Stars. D. Reidel Publishing Company, Dordrecht. p. 4–10. ISBN 9027708851.
- ^ Vol. 1, part 1, p. 422, Almagestum Novum, Giovanni Battista Riccioli, Bononiae: Ex typographia haeredis Victorij Benatij, 1651.
- ^ A New View of Mizar, Leos Ondra, accessed on line May 26, 2007.
- ^ See The Binary Stars, Robert Grant Aitken, New York: Dover, 1964, pp. 24–25, 38, and The present status of double star astronomy, K. Aa. Strand, Astronomical Journal 59 (March 1954), pp. 61–66, Bibcode: 1954AJ.....59...61S, p. 61.
- ^ The Binary Stars, Robert Grant Aitken, New York: Dover, 1964, p. 260.
- ^ a b c Heintz, W. D. (1978). Double Stars. Dordrecht: D. Reidel Publishing Company. p. 12. ISBN 9027708851.
- ^ p. 2, Observing and Measuring Double Stars, Bob Argyle, ed., London: Springer-Verlag, 2004, ISBN 1-85233-558-0.
- ^ p. 53–55, 65–67, Observing and Measuring Double Stars, Bob Argyle, ed., London: Springer-Verlag, 2004, ISBN 1-85233-558-0.
- ^ a b "Introduction and Growth of the WDS", The Washington Double Star Catalog, Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf, Astrometry Department, United States Naval Observatory, accessed on line August 20, 2008.
- ^ Sixth Catalog of Orbits of Visual Binary Stars, William I. Hartkopf and Brian D. Mason, United States Naval Observatory, accessed on line August 20, 2008.
- ^ Heintz, W. D. (1978). Double Stars. Dordrecht: D. Reidel Publishing Company. p. 17–18. ISBN 9027708851.
- ^ Heintz, W. D. (1978). Double Stars. Dordrecht: D. Reidel Publishing Company. p. 19. ISBN 9027708851.
- ^ a b p. 307–308, Observing and Measuring Double Stars, Bob Argyle, ed., London: Springer-Verlag, 2004, ISBN 1-85233-558-0.
- ^ Entry 14396-6050, discoverer code RHD 1AB,The Washington Double Star Catalog, United States Naval Observatory. Accessed on line August 20, 2008.
- ^ Format of the current WDS, Washington Double Star Catalog, United States Naval Observatory. Accessed on line August 26, 2008.
- ^ References and discoverer codes, The Washington Double Star Catalog, United States Naval Observatory. Accessed on line August 20, 2008.
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