Algol: Difference between revisions

The constellation Perseus and Algol, the Bright Star in the Gorgon's head
The constellation Perseus and Algol, the Bright Star in the Gorgon's head
	Johannes Hevelius, Uranographia, 1690

Algol
	Location of β Persei (circled)
Observation data; Epoch J2000 Equinox J2000
Constellation	Perseus
Right ascension	03h 08m 10.13245s
Declination	+40° 57′ 20.3280″
Apparent magnitude (V)	2.12 (- 3.39)
Characteristics
Spectral type	Aa1: B8V; Aa2: K0IV; Ab: F1V (kA4hA9.5mF0:)
U−B colour index	−0.37
B−V colour index	−0.05
Variable type	EA/SD
Astrometry
Radial velocity (Rv)	3.7 km/s
Proper motion (μ)	RA: 2.99 mas/yr ; Dec.: −1.66 mas/yr
Parallax (π)	34.7 ± 0.6 mas
Distance	94 ± 2 ly ; (28.8 ± 0.5 pc)
β Per Aa1
Absolute magnitude (MV)	−0.07
β Per Aa2
Absolute magnitude (MV)	2.9
β Per Ab
Absolute magnitude (MV)	2.3
Orbit
Primary	β Per Aa1
Companion	β Per Aa2
Period (P)	2.867328 days
Semi-major axis (a)	0.00215″
Eccentricity (e)	0
Inclination (i)	98.70°
Longitude of the node (Ω)	43.43°
Orbit
Primary	β Per A
Companion	β Per B
Period (P)	680.168 days
Semi-major axis (a)	0.09343″
Eccentricity (e)	0.227
Inclination (i)	83.66°
Longitude of the node (Ω)	132.66°
Periastron epoch (T)	2446927.22
Argument of periastron (ω); (primary)	310.02°
Details
β Per Aa1
Mass	3.17 ± 0.21 M☉
Radius	2.73 ± 0.20 R☉
Luminosity	182 L☉
Surface gravity (log g)	4.0 cgs
Temperature	13,000 K
Rotational velocity (v sin i)	49 km/s
Age	570 Myr
β Per Aa2
Mass	0.70±0.08 M☉
Radius	3.48±0.28 R☉
Luminosity	6.92 L☉
Surface gravity (log g)	3.5 cgs
Temperature	4,500 K
β Per Ab
Mass	1.76±0.15 M☉
Radius	1.73±0.33 R☉
Luminosity	10.0 L☉
Surface gravity (log g)	4.5 cgs
Temperature	7,500 K
Other designations
	Algol, Gorgona, Gorgonea Prima, Demon Star, El Ghoul, β Persei, β Per, 26 Persei, BD+40°673, FK5 111, GC 3733, HD 19356, HIP 14576, HR 936, PPM 45864, SAO 38592.
Database references
SIMBAD	data

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Algol /ˈælɡɒl/,^[12] designated Beta Persei (β Persei, abbreviated Beta Per, β Per), known colloquially as the Demon Star, is a bright multiple star in the constellation of Perseus and one of the first non-nova variable stars to be discovered.

Algol is a three-star system, consisting of Beta Persei Aa1, Aa2, and Ab – in which the hot luminous primary β Persei Aa1 and the larger, but cooler and fainter, β Persei Aa2 regularly pass in front of each other, causing eclipses. Thus Algol's magnitude is usually near-constant at 2.1, but regularly dips to 3.4 every 2.86 days during the roughly 10-hour-long partial eclipses. The secondary eclipse when the brighter primary star occults the fainter secondary is very shallow and can only be detected photoelectrically.^[13]

Algol gives its name to its class of eclipsing variable, known as Algol variables.

Observation history

The Algol system on 12 August 2009. This is a CHARA interferometer image with ⁠1/2⁠-milliarcsecond resolution in the near-infrared H-band. The elongated appearance of Algol Aa2 (labelled B) and the round appearance of Algol Aa1 (labelled A) are real, but the form of Algol Ab (labelled C) is an artifact.

An ancient Egyptian calendar of lucky and unlucky days composed some 3,200 years ago is said to be the oldest historical documentation of the discovery of Algol.^[14]^[15] ^[16]

The association of Algol with a demon-like creature (Gorgon in the Greek tradition, ghoul in the Arabic tradition) suggests that its variability was known long before the 17th century,^[17] but there is still no indisputable evidence for this.^[18] The Arabic astronomer al-Sufi said nothing about any variability of the star in his Book of Fixed Stars published c.964.^[19]

The variability of Algol was noted in 1667 by Italian astronomer Geminiano Montanari,^[20] but the periodic nature of its variations in brightness was not recognized until more than a century later, when the British amateur astronomer John Goodricke also proposed a mechanism for the star's variability.^[21]^[22] 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.^[23]

In 1881, the Harvard astronomer Edward Charles Pickering presented evidence that Algol was actually an eclipsing binary.^[24] 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.^[25] Thus, Algol became one of the first known spectroscopic binaries. Joel Stebbins at the University of Illinois Observatory used an early selenium cell photometer to produce the first-ever photoelectric study of a variable star. The light curve revealed the second minimum and the reflection effect between the two stars.^[26] Some difficulties in explaining the observed spectroscopic features led to the conjecture that a third star may be present in the system; four decades later this conjecture was found to be correct.^[27]

System

Algol is a multiple-star system with three confirmed and two suspected stellar components.^[28] From the point of view of the Earth, Algol Aa1 and Algol Aa2 form an eclipsing binary because their orbital plane contains the line of sight to the Earth. The eclipsing binary pair is separated by only 0.062 astronomical units (au) from each other, whereas the third star in the system (Algol Ab) is at an average distance of 2.69 au from the pair, and the mutual orbital period of the trio is 681 Earth days. The total mass of the system is about 5.8 solar masses, and the mass ratios of Aa1, Aa2, and Ab are about 4.5 to 1 to 2.

The three components of the bright triple star used to be, and still sometimes are, referred to as β Per A, B, and C. The Washington Double Star Catalog lists them as Aa1, Aa2, and Ab, with two very faint stars B and C about one arcmin distant. A further five faint stars are also listed as companions.^[29]

The close pair consists of a B8 main sequence star and a much less massive K0 subgiant, which is highly distorted by the more massive star. These two orbit every 2.9 days and undergo the eclipses that cause Algol to vary in brightness. The third star orbits these two every 680 days and is an A or F-type main sequence star. It has been classified as an Am star, but this is now considered doubtful.^[5]^[30]

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 stars, the more massive component Algol Aa1 is still in the main sequence, but the less massive Algol Aa2 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.^[31] The gas flow between the primary and secondary stars in Algol has been imaged using Doppler Tomography.^[32]^[33]

This system also exhibits x-ray and radio wave^[34] flares. The x-ray flares are thought to be caused by the magnetic fields of the A and B components interacting with the mass transfer.^[35] The radio-wave flares might be created by magnetic cycles similar to those of sunspots, but because the magnetic fields of these stars are up to ten times stronger than the field of the Sun, these radio flares are more powerful and more persistent.^[36]^[37] The secondary component was identified as the radio emitting source in Algol using Very-long-baseline interferometry by Lestrade and co-authors.^[4]

Magnetic activity cycles in the chromospherically active secondary component induce changes in its radius of gyration that have been linked to recurrent orbital period variations on the order of ⁠ΔP/P⁠ ≈ 10⁻⁵ via the Applegate mechanism.^[38] Mass transfer between the components is small in the Algol system^[39] but could be a significant source of period change in other Algol-type binaries.

The distance to Algol has been measured using very-long baseline interferometry, giving a value of 94 light-years.^[7] About 7.3 million years ago it passed within 9.8 light-years of the Solar System^[40] and its apparent magnitude was about −2.5, which is considerably brighter than the star Sirius is today. Because the total mass of the Algol system is about 5.8 solar masses, at the closest approach this might have given enough gravity to perturb the Oort cloud of the Solar System somewhat and hence increase the number of comets entering the inner Solar System. However, the actual increase in net cometary collisions is thought to have been quite small.^[41]

Names

Algol is a bright star in the constellation of Perseus (upper right).

Beta Persei is the star's Bayer designation.

The official name Algol

The name Algol derives from Arabic رأس الغول raʾs al-ghūl : head (raʾs) of the ogre (al-ghūl) (see "ghoul").^[42] The English name Demon Star was taken from the Arabic name.^[43] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)^[44] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016^[45] included a table of the first two batches of names approved by the WGSN; which included Algol for this star. It is so entered on the IAU Catalog of Star Names.^[46]

Ghost and demon star

Algol was called Rōsh ha Sāṭān or "Satan's Head" in Hebrew folklore, as stated by Edmund Chilmead, who called it "Divels head" or Rosch hassatan. A Latin name for Algol from the 16th century was Caput Larvae or "the Spectre's Head".^[43] Hipparchus and Pliny made this a separate, though connected, constellation.^[43]

First star of Medusa's head

Earlier the name of the constellation Perseus was Perseus and Medusa's Head where an asterism representing the head of Medusa after Perseus has cut it off already known in ancient Rome.^[47] Medusa is a gorgon so the star is also called Gorgonea Prima meaning the first star of the gorgon.^[43]

Chinese names

In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of β Persei, 9 Persei, τ Persei, ι Persei, κ Persei, ρ Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for β Persei itself is 大陵五 (Dà Líng wu, English: The Fifth Star of Mausoleum.).^[48] According to R.H. Allen the star bore the grim name of Tseih She 積屍 (Zhi Shī), meaning "Piled up Corpses"^[43] but this appears to be a misidentification, and Dié Shī is correctly π Persei, which is inside the Mausoleum.^[49]

Observing Algol

The Algol system usually has an apparent magnitude of 2.1, similar to those of Mirfak (α Persei) at 1.9 and Almach (γ Andromedae) at 2.2, with whom it forms a right triangle. During eclipses it dims to 3.4, making it as faint as nearby ρ Persei at 3.3.

Observing Algol's Eclipses in 2025 ^[50]^[51]
Date	Time
December 1, 2024	18:52
January 2, 2025	07:53
February 2, 2025	20:55
March 3, 2025	13:09
April 1, 2025	05:22
May 2, 2025	18:23
June 3, 2025	07:22
July 1, 2025	23:30
August 2, 2025	12:25
September 3, 2025	17:35
October 1, 2025	01:20
November 2, 2025	06:23
December 3, 2025	19:22

Listed are the first eclipse dates and times of each month, with all times in UT. β Persei Aa2 eclipses β Persei Aa1 every 2.867321 days (2 days 20 hours 49 min). To determine subsequent eclipses, add this interval to each listed date and time. For example, the Jan 2 eclipse at 8h will result in consecutive eclipse times on Jan 5 at 5h, Jan 8 at 1h, Jan 10 at 22h, and so on (all times approximate).

Cultural significance

Historically, the star has received a strong association with bloody violence across a wide variety of cultures. In the Tetrabiblos, the 2nd-century astrological text of the Alexandrian astronomer Ptolemy, Algol is referred to as "the Gorgon of Perseus" and associated with death by decapitation: a theme which mirrors the myth of the hero Perseus's victory over the snake-haired Gorgon Medusa.^[52] In the astrology of fixed stars, Algol is considered one of the unluckiest stars in the sky,^[43] and was listed as one of the 15 Behenian stars.^[53]

References

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^ ^a ^b ^c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
^ ^a ^b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: 02025. Bibcode:2009yCat....102025S.
^ ^a ^b ^c Lestrade, Jean-Francois; Phillips, Robert B.; Hodges, Mark W.; Preston, Robert A. (June 1993). "VLBI astrometric identification of the radio emitting region in Algol and determination of the orientation of the close binary". The Astrophysical Journal. 410: 808. Bibcode:1993ApJ...410..808L. doi:10.1086/172798. ISSN 0004-637X.
^ ^a ^b Frank, M. G.; Whelan, D. G.; Junginger, J. C. (2022). "Spectral Classification of Algol C". Journal of the American Association of Variable Star Observers (Jaavso). 50 (1): 123. arXiv:2205.06229. Bibcode:2022JAVSO..50..123F.
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^ J. Stebbins (1910). "The Measurement of the Light of Stars with a Selenium Photometer with an Application to the Variation of Algol". Astrophysical Journal. 32: 185–214. Bibcode:1910ApJ....32..185S. doi:10.1086/141796.
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^ Pustylnik, Izold (1995). "On Accretion Component of the Flare Activity in Algol". Baltic Astronomy. 4 (1–2): 64–78. Bibcode:1995BaltA...4...64P. doi:10.1515/astro-1995-0106.
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External links

"Algol 3". SolStation. Retrieved 31 July 2006.
"4C02517". ARICNS. 4 March 1998. Archived from the original on 10 February 2006. Retrieved 31 July 2006.
"Algol". Alcyone ephemeris. Retrieved 8 June 2006.
Bezza, Giuseppe. "Al-ghûl, the ogre". Translated by Daria Dudziak. Cielo e Terra. Archived from the original on 20 June 2006. Retrieved 8 June 2006.

[hipparcos-1] Van Leeuwen, F. (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. S2CID 18759600.

[ducati-2] Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.

[gcvs-3] Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: 02025. Bibcode:2009yCat....102025S.

[lestrade1993-4] Lestrade, Jean-Francois; Phillips, Robert B.; Hodges, Mark W.; Preston, Robert A. (June 1993). "VLBI astrometric identification of the radio emitting region in Algol and determination of the orientation of the close binary". The Astrophysical Journal. 410: 808. Bibcode:1993ApJ...410..808L. doi:10.1086/172798. ISSN 0004-637X.

[frank2022-5] Frank, M. G.; Whelan, D. G.; Junginger, J. C. (2022). "Spectral Classification of Algol C". Journal of the American Association of Variable Star Observers (Jaavso). 50 (1): 123. arXiv:2205.06229. Bibcode:2022JAVSO..50..123F.

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Observation data Epoch J2000 Equinox J2000
Location of β Persei (circled)
Constellation	Perseus
Right ascension	03^h 08^m 10.13245^s^[1]
Declination	+40° 57′ 20.3280″^[1]
Apparent magnitude (V)	2.12^[2] (- 3.39^[3])
Characteristics
Spectral type	Aa1: B8V^[4] Aa2: K0IV^[4] Ab: F1V^[5] (kA4hA9.5mF0:^[6])
U−B colour index	−0.37^[2]
B−V colour index	−0.05^[2]
Variable type	EA/SD^[3]
Astrometry

Radial velocity (R_v)	3.7 km/s
Proper motion (μ)	RA: 2.99^[1] mas/yr Dec.: −1.66^[1] mas/yr
Parallax (π)	34.7 ± 0.6 mas^[7]
Distance	94 ± 2 ly (28.8 ± 0.5 pc)^[7]


β Per Aa1
Absolute magnitude (M_V)	−0.07^[8]


β Per Aa2
Absolute magnitude (M_V)	2.9^[8]


β Per Ab
Absolute magnitude (M_V)	2.3^[8]

Orbit^[9]
Primary	β Per Aa1
Companion	β Per Aa2
Period (P)	2.867328 days
Semi-major axis (a)	0.00215″
Eccentricity (e)	0
Inclination (i)	98.70°
Longitude of the node (Ω)	43.43°
Orbit^[9]
Primary	β Per A
Companion	β Per B
Period (P)	680.168 days
Semi-major axis (a)	0.09343″
Eccentricity (e)	0.227
Inclination (i)	83.66°
Longitude of the node (Ω)	132.66°
Periastron epoch (T)	2446927.22
Argument of periastron (ω) (primary)	310.02°
Details
β Per Aa1
Mass	3.17 ± 0.21^[9] `M`_☉
Radius	2.73 ± 0.20^[9] `R`_☉
Luminosity	182^[8] `L`_☉
Surface gravity (log g)	4.0^[10] cgs
Temperature	13,000^[10] K
Rotational velocity (v sin i)	49^[11] km/s
Age	570^[8] Myr


β Per Aa2
Mass	0.70±0.08^[9] `M`_☉
Radius	3.48±0.28^[9] `R`_☉
Luminosity	6.92^[8] `L`_☉
Surface gravity (log g)	3.5^[10] cgs
Temperature	4,500^[10] K


β Per Ab
Mass	1.76±0.15^[9] `M`_☉
Radius	1.73±0.33^[9] `R`_☉
Luminosity	10.0^[8] `L`_☉
Surface gravity (log g)	4.5^[10] cgs
Temperature	7,500^[10] K

Other designations
Algol, Gorgona, Gorgonea Prima, Demon Star, El Ghoul, β Persei, β Per, 26 Persei, BD+40°673, FK5 111, GC 3733, HD 19356, HIP 14576, HR 936, PPM 45864, SAO 38592.
Database references
SIMBAD	data