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Variable Star Of The Month
January, 1999: Beta Persei (Algol)
BETA PERSEI "...the
Gorgon's head, a ghastly sight, deformed and dreadful, and a sight of woe". - Homer, writing of Algol
in the Iliad.
This is a PSPC image of a portion of the Perseus
region of the sky. The image was taken by the ROSAT spacecraft and is courtesy of the Max
Planck Institute. A Look at
Algol Algol is one of the most popular and well known variable stars in the sky. One of
the reasons for this is that it is a star which can be observed with the unaided eye. Another
reason is because it has a relatively short period of less than three days. This means a new observer can
go outside everynight and see a complete cycle of Algol in their first week of observing if the star is
visible at night in their location. Algol is an eclipsing binary star system 93 light-years away as
determined by the Hipparcos satellite. The main star is a B8 main-sequence star 3 times as large as our sun
and the secondary star is a K2-type subgiant. Together they rotate around each other. As seen from Earth,
when one star blocks our view of the other star its overall brightness changes. There is a very faint third
star in the system. It is an F1 main-sequence star orbiting the inner pair every 1.86 years.
Algol's variability was discovered in 1667 by the Italian astronomer Geminiano Montanari making it one of
the first ever non-nova variable stars discovered. John Goodricke of England is credited with the discovery
of Algol's periodicity in 1782-83. It was apparently also independently discovered by a German farmer named
Palitzch. At first it was believed that a planet was causing the eclipses. In 1881 astronomers theorized it
was actually an eclipsing binary system based on evidence presented by Edward Pickering, the Director of
the Harvard College Observatory (HCO). In 1889 this
theory was proven through spectrographic analysis by H.C. Vogel at Potsdam. "The Demon Star" Human history has not been kind to this star.
Homer wrote of Algol in the Iliad: "...the Gorgon's head, a ghastly sight, deformed and dreadful, and a
sight of woe". Some common names for Algol are The Demon, the Demon Star, the Blinking Demon, the Ghoul,
and the Spectre's Head. Sounds rather more like members of a hard rock goth band than a beautiful
astronomical object. The earliest known maligning of this star is from the Arabian name Ri'B al Ohill, the
Demon's Head. We also have Al Ghul meaning Mischief-maker. In Hebrew it is called Rosh ha Sitan, Satan's
Head, and also Lilith, Adam's legendary demonic first wife (predecessor to Eve) according to Babylonian
myth. 17th century maps referred to it as Caput Larvae, a translation of "The Spectre's Head". The Chinese
referred to it as Tseih She, the Piled-up Corpses. Even astrologers refer to it as the worst star in the
heavens to be involved with. More recently, the name Algol has been given to a violent video game. What does a star have to do to get respect? "The Algol Paradox" One way is to excite scientists. Despite its popularity and the attention focused on Algol, it still is not fully understood and has a few surprises for researchers. Recently, "The Algol Paradox" is a term that has been used to describe a discrepancy in our theories of stellar evolution. The primary star should expand first due to its greater mass, yet we find that the secondary is the older star in the Algol system. Many theories abound about how this can be. The most popular is that the secondary star is indeed older than the primary. It is only smaller because it dumped a lot of its mass onto the younger star, making it more massive and subsequently to look beyond it's years. The above light curve is based upon observations of Algol made and submitted by John Isles. It is printed in Chapter 11 of the Hands-On Astrophysics manual. More Info The text below was written by Dr. John R. Percy, former AAVSO president, and Dr. Janet A. Mattei, AAVSO director. It was originally published in the Royal Astronomical Society of Canada Observer's Handbook in 1995. Algol (ß Persei) is the brigh eclipsing binary with deep eclipses. It is also the brightest and closest semi-detached binary, a type of binary system in which one component has filled its Roche lobe (the volume within which gas is gravitationally bound to the star) and is now transferring material to its companion. Algol varies in V magnitude from 2.1 at maximum to 3.4 at primary minimum, with a period of 2.867315 days; this period, however, is slowly lengthening. The primary eclipse occurs when the fainter K2IV star passes in front of the brighter B8V star, and lasts for some 10 hours in total. Because the eclipse is partial, the minimum is not flat, but rounded. There is also a shallow secondary eclipse when the B8V star passes in front of the K2IV star. It can only be detected photoelectrically. The primary eclipse, however, can easily be detected with the unaided eye, and the magnitude and the time of minimum can be measured. These images reflect modelled theories of the circumstellar flow of Algol. Results were published in the The Astrophysical Journal, 1995, 445, 889. The authors are John M. Blondin, Mercedes T. Richards & Michael L. Malinowski. For More Information For more information on observing eclipsing binaries contact the AAVSO Eclipsing Binary Committee Chairperson Marvin Baldwin (mbaldwin00@hsonline.net). This month's Variable Star of the Month was prepared by Aaron Price.
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