Algol

Beta Persei A/B/C
Position Beta Per.png
The position of Algol.
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 08m 10.1315s[1]
Declination +40° 57′ 20.332″[1]
Apparent magnitude (V) 2.12[1]
Characteristics
Spectral type B8V (A)[1] /K02IV (B)[2] /A5V (C)
U−B color index -0.37
B−V color index -0.05
Variable type Eclipsing binary
Astrometry
Radial velocity (Rv) 3.7 km/s
Proper motion (μ) RA: 2.39 mas/yr
Dec.: -1.44 mas/yr
Parallax (π) 35.14 ± 0.90 mas
Distance 93 ± 2 ly
(28.5 ± 0.7 pc)
Absolute magnitude (MV) -0.15
Details
Mass 3.59/0.79/1.67 M☉
Radius 2.3/3.0/0.9 R☉
Luminosity 98/3.4/4.1 L☉
Temperature 12,000/4,500/8,500 K
Metallicity Not available
Rotation 65 km/s.
Age < 3 × 108 years
Other designations
Algol, Gorgona, Gorgonea Prima, Demon Star, El Ghoul, 26 Per, GJ 9110, HR 936, BD +40°673, HD 19356, GCTP 646.00, SAO 38592, FK5 111, Wo 9110, ADS 2362, WDS 03082+4057A, HIP 14576.

Algol (β Per / Beta Persei), known colloquially as the Demon Star, is a bright star in the constellation Perseus. It is one of the best known eclipsing binaries, the first such star to be discovered, and also one of the first (non-nova) variable stars to be discovered. Algol is actually a three-star system (Beta Persei A, B, and C) in which the large and bright primary Beta Persei A is regularly eclipsed by the dimmer Beta Persei B. Thus, Algol's magnitude is usually near-constant at 2.1, but regularly dips to 3.4 every two days, 20 hours and 49 minutes during the roughly 10-hour long partial eclipses. There is also a secondary eclipse when the brighter star occults the fainter secondary. This secondary eclipse can only be detected photoelectrically.[3] Algol gives its name to its class of eclipsing variable, known as Algol variables.

Contents

Observation history

The variability of Algol was first recorded in 1667 by Geminiano Montanari, but it is probable that this property was noticed long before this time. The first person to propose a mechanism for the variability of this star was the British amateur astronomer John Goodricke. In May 1783 he presented his findings to the Royal Society, suggesting that the periodic variability was caused by a dark body passing in front of the star (or else that the star itself has a darker region that is periodically turned toward the Earth.) For his report he was awarded the Copley Medal.[4]

In 1881, the Harvard astronomer Edward Charles Pickering presented evidence that Algol was actually an eclipsing binary.[5] This was confirmed a few years later, in 1889, when the Potsdam astronomer Hermann Carl Vogel found periodic doppler shifts in the spectrum of Algol, inferring variations in the radial velocity of this binary system.[6] Thus Algol became one of the first known spectroscopic binaries.

System

Algol A and Algol B are an eclipsing binary, because their orbital plane coincidentally contains the Earth's line of sight. To be more precise, however, Algol is a triple-star system: the eclipsing binary pair is separated by only 0.062 AU, while the third star in the system (Algol C) is at an average distance of 2.69 AU from the pair and the mutual orbital period is 681 days (1.86 years). The total mass of the system is about 5.8 solar masses, and the mass ratios of A, B and C are about 4.5 : 1 : 2.

Orbital Elements of the Algol System
Components Semimajor axis Ellipticity Period Inclination
A—B[7] 0.00218″ 0.00 2.87 days 97.69°
(AB)—C[8] 0.09461″ 0.225 680.05 days 83.98°

Studies of Algol led to the Algol paradox in the theory of stellar evolution: although components of a binary star form at the same time, and massive stars evolve much faster than the less massive ones, it was observed that the more massive component Algol A is still in the main sequence, while the less massive Algol B is a subgiant star at a later evolutionary stage. The paradox can be solved by mass transfer: when the more massive star became a subgiant, it filled its Roche lobe, and most of the mass was transferred to the other star, which is still in the main sequence. In some binaries similar to Algol, a gas flow can be seen.[9]

This system also exhibits variable activity in the form of x-ray and radio flares. The former is thought to be caused by the magnetic fields of the AB components interacting with the mass transfer.[10] The radio emissions may be created by magnetic cycles similar to sunspots, but, as the magnetic fields around these stars are up to ten times stronger than that of the Sun, these radio flares are more powerful and longer lasting.[11]

Algol is 92.8 light years from Earth; however, about 7.3 million years ago it passed within 9.8 light years[12] and its apparent magnitude was approximately −2.5, considerably brighter than Sirius is today. Because the total mass of the system is 5.8 solar masses, and despite the fairly large distance at closest approach, this may have been enough to perturb the solar system's Oort cloud slightly and to increase the number of comets entering the inner solar system. However, the actual increase in net cratering rate is believed to have been quite small.[13]

Etymology and cultural significance

The name Algol derives from Arabic رأس الغول ra's al-ghūl : head (ra's) of the ogre (al-ghūl) (see "ghoul") which was given from its position in the constellation Perseus, representing the head of Gorgon Medusa. The English names of Demon Star and Blinking Demon are direct translations.[14] In Hebrew folklore it was known as Rōsh ha Sāṭān 'Satan's Head', via Edmund Chilmead, who called it 'Divels head' or Rosch hassatan. A Latin term from the 16th century was Caput Larvae 'Spectre's Head'. It was also linked with Lilith.[14]. Hipparchus and Pliny made this a separate, though connected, constellation.[14]

It is known as 大陵五 (the Fifth Star of the Mausoleum) in Chinese astronomy, and also bore the grim name Tseih She (叠尸 - die2 shi1 in Modern Pinyin), meaning 'piled up corpses'.[14]

Astrology

Astrologically, Algol is considered the most unfortunate star in the sky.[14] In the Middle Ages it was one of the 15 Behenian stars,[15] associated with the diamond and hellebore, and marked with the kabbalistic sign: Algol symbol (Agripe 1531).svg

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 Database entry for Algol A, SIMBAD. Accessed online February 9, 2008.
  2. ↑ Database entry for Algol B, SIMBAD. Accessed online February 9, 2008.
  3. ↑ Beta Persei, American Association of Variable Star Observers. http://www.aavso.org/vstar/vsots/0199.shtml
  4. ↑ "John Goodricke, The Discovery of the Occultating Variable Stars". 2003-08-06. http://www.surveyor.in-berlin.de/himmel/Bios/Goodricke-e.html. Retrieved 2006-07-31. 
  5. ↑ Pickering, Edward C. (1881). "Dimensions of the Fixed Stars, with especial reference to Binaries and Variables of the Algol type". Astronomical register 50: 253–256. doi:10.1007/BF00215914. http://adsabs.harvard.edu/abs/1881AReg...19..253.. 
  6. ↑ A. H. Batten (1989). "Two Centuries of Study of Algol Systems". Space Science Reviews 50 (1/2): 1–8. doi:10.1007/BF00215914. http://adsabs.harvard.edu/abs/1989SSRv...50....1B. 
  7. ↑ L. A. Molnar, R. L. Mutel (1996). "Dynamical Evolution of the Algol Triple System". Bulletin of the American Astronomical Society 28: 921. doi:10.1007/BF00215914. http://adsabs.harvard.edu/abs/1996AAS...188.6014M. 
  8. ↑ W.I. Hartkopf, B.D. Mason (2006-07-30). "Sixth Catalog of Orbits of Visual Binary Stars". U.S. Naval Observatory. http://ad.usno.navy.mil/wds/orb6.html. Retrieved 2006-07-31. 
  9. ↑ Pustylnik, Izold (1995). "On Accretion Component of the Flare Activity in Algol". Baltic Astronomy 4: 64–78. doi:10.1007/BF00215914. http://adsabs.harvard.edu/abs/1995BaltA...4...64P. 
  10. ↑ M.J. Sarna, S.K. Yerli, A.G. Muslimov (1998). "Magnetic activity and evolution of Algol-type stars - II". Monthly Notices of the Royal Astronomical Society 297 (3): 760–768. doi:10.1046/j.1365-8711.1998.01539.x. http://adsabs.harvard.edu/abs/1998MNRAS.297..760S. 
  11. ↑ Blue, Charles E. (2002-06-03). "Binary Stars "Flare" With Predictable Cycles, Analysis of Radio Observations Reveals". National Radio Astronomy Observatory. http://www.nrao.edu/pr/2002/algol/. Retrieved 2006-07-31. 
  12. ↑ Garcia-Sanchez, J.; Preston, R. A.; Jones, D. L.; Lestrade, J.-F.; Weissman, P. R.; Latham, D. W. (August 25, 1997). "A Search for Stars Passing Close to the Sun". The First Results of Hipparcos and Tycho. Kyoto, Japan: IAU. http://adsabs.harvard.edu/abs/1997IAUJD..14E..51G. Retrieved 2007-06-01. 
  13. ↑ J. García-Sánchez, R.A. Preston, D.L. Jones, P.R. Weissman (1999). "Stellar Encounters with the Oort Cloud Based on Hipparcos Data". The Astronomical Journal 117: 1042–1055. doi:10.1086/300723. http://www.iop.org/EJ/article/1538-3881/117/2/1042/980216.html. 
  14. ↑ 14.0 14.1 14.2 14.3 14.4 Allen, Richard Hinckley (1963). Star Names: Their Lore and Meaning (revised edition). Dover. pp. 332–33. ISBN 0-486-21079-0. OCLC 637940 185804232 637940. , also online on Bill Thayer's site Lacus Curtius: Star Names: Their Lore and Meaning
  15. ↑ Tyson, Donald; Freake, James (1993). Three Books of Occult Philosophy. Llewellyn Worldwide. ISBN 0875428320. OCLC 41597186 26634250 41597186. 

External links

Coordinates: Sky map 03h 08m 10.1315s, +40° 57′ 20.332″

Stars of Perseus
Bayer
α (Mirfak / Algenib) • β (Algol) • γ • δ • ε • ζ • η (Miram) • θ • ι • κ (Misam) • λ • μ • ν • ξ (Menkib) • ο (Atik) • π (Gorgonea Secunda) • ρ (Gorgonea Tertia) • σ • τ • φ • χ (also NGC 884) • ψ (Seif) • ω (Gorgonea Quarta) • b • c • d • e • f • g • i • k • l • m • n • o • A
Flamsteed
1 • 2 • 3 • 4 (g) • 5 • 7 (χ) • 8 • 9 (i) • 10 • 11 • 12 • 13 (θ) • 14 • 15 (η, Miram) • 16 • 17 • 18 (τ) • 20 • 21 • 22 (π, Gorgonea Secunda) • 23 (γ) • 24 • 25 (ρ, Gorgonea Tertia) • 26 (β, Algol) • 27 (κ, Misam) • 28 (ω, Gorgonea Quarta) • 29 • 30 • 31 • 32 (l) • 33 (α, Mirfak / Algenib) • 34 • 35 (σ) • 36 • 37 (ψ, Seif) • 38 (ο, Atik) • 39 (δ) • 40 (o) • 41 (ν) • 42 (n) • 43 (A) • 44 (ζ) • 45 (ε) • 46 (ξ, Menkib) • 47 (λ) • 48 (c) • 49 • 50 • 51 (μ) • 52 (f) • 53 (d) • 54 • 55 • 56 • 57 (m) • 58 (e) • 59 • 1 Aur
Nearby
GJ 1068
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