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Beta Herculis
Beta Herculis (β Herculis, abbreviated Beta Her, β Her), formally named Kornephoros /kɔːrˈnɛfərəs/, is a binary star and the brightest star in the northern constellation of Hercules at a base apparent visual magnitude of 2.81. This is a suspected variable star with an apparent magnitude that may rise as high as 2.76. Based upon parallax measurements, it is located at a distance of 139 light-years (43 parsecs) from the Sun.
Although Beta Herculis appears to the naked eye to be a single star, in July 1899 the American astronomer W. W. Campbell discovered from spectroscopic measurements that its radial velocity varies, and concluded that it has a companion.
At Palomar Observatory, Antoine Labeyrie and others used speckle interferometry with the Hale Telescope to resolve the system in 1977. The Hipparcos satellite observed the orbital motion of the primary relative to other stars, and an orbit was computed in 2005 using spectroscopic data together with these measurements. The period of the system is around 410 days. They have a high orbital eccentricity of 0.55 and the orbital plane is inclined 53.8° to the line of sight from the Earth.
The primary star has a stellar classification of G7 IIIa, indicating that it is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. It is most likely fusing helium into carbon and oxygen in its core, qualifying it as a horizontal branch or red clump star. With a mass nearly three times the mass of the Sun, it was most likely a B-type main-sequence star similar to Beta Librae prior to core hydrogen exhaustion. It is comparable to the main component of Capella, albeit warmer and brighter. Being 420 million years old, it has expanded to 16 times the Sun's radius and is radiating 150 times its luminosity. The effective temperature of the star's outer envelope is about 5,100 K, which gives it the yellow hue of a G-type star. The secondary star has a mass only 90% that of the Sun.
With insufficient mass to explode as a supernova, Beta Herculis will most likely become a white dwarf similar to Sirius B, but less massive.
β Herculis (Latinised to Beta Herculis) is the star's Bayer designation.
It bore the traditional names Kornephoros, a Greek word meaning "club bearer", and Rutilicus, a corruption of the Latin word titillicus, meaning "armpit". In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name Kornephoros for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
It was a member of the indigenous Arabic asterism al-Nasaq al-Shāmī, "the Northern Line" of al-Nasaqān "the Two Lines", along with Gamma Herculis, Gamma Serpentis and Beta Serpentis. Though, according to a 1971 NASA catalog, al-Nasaq al-Sha'āmī or Nasak Shamiya was the title for three other stars: Beta Serpentis as Nasak Shamiya I, Gamma Serpentis as Nasak Shamiya II and Gamma Herculis as Nasak Shamiya III.
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Beta Herculis
Beta Herculis (β Herculis, abbreviated Beta Her, β Her), formally named Kornephoros /kɔːrˈnɛfərəs/, is a binary star and the brightest star in the northern constellation of Hercules at a base apparent visual magnitude of 2.81. This is a suspected variable star with an apparent magnitude that may rise as high as 2.76. Based upon parallax measurements, it is located at a distance of 139 light-years (43 parsecs) from the Sun.
Although Beta Herculis appears to the naked eye to be a single star, in July 1899 the American astronomer W. W. Campbell discovered from spectroscopic measurements that its radial velocity varies, and concluded that it has a companion.
At Palomar Observatory, Antoine Labeyrie and others used speckle interferometry with the Hale Telescope to resolve the system in 1977. The Hipparcos satellite observed the orbital motion of the primary relative to other stars, and an orbit was computed in 2005 using spectroscopic data together with these measurements. The period of the system is around 410 days. They have a high orbital eccentricity of 0.55 and the orbital plane is inclined 53.8° to the line of sight from the Earth.
The primary star has a stellar classification of G7 IIIa, indicating that it is a giant star that has exhausted the hydrogen at its core and evolved away from the main sequence. It is most likely fusing helium into carbon and oxygen in its core, qualifying it as a horizontal branch or red clump star. With a mass nearly three times the mass of the Sun, it was most likely a B-type main-sequence star similar to Beta Librae prior to core hydrogen exhaustion. It is comparable to the main component of Capella, albeit warmer and brighter. Being 420 million years old, it has expanded to 16 times the Sun's radius and is radiating 150 times its luminosity. The effective temperature of the star's outer envelope is about 5,100 K, which gives it the yellow hue of a G-type star. The secondary star has a mass only 90% that of the Sun.
With insufficient mass to explode as a supernova, Beta Herculis will most likely become a white dwarf similar to Sirius B, but less massive.
β Herculis (Latinised to Beta Herculis) is the star's Bayer designation.
It bore the traditional names Kornephoros, a Greek word meaning "club bearer", and Rutilicus, a corruption of the Latin word titillicus, meaning "armpit". In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name Kornephoros for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
It was a member of the indigenous Arabic asterism al-Nasaq al-Shāmī, "the Northern Line" of al-Nasaqān "the Two Lines", along with Gamma Herculis, Gamma Serpentis and Beta Serpentis. Though, according to a 1971 NASA catalog, al-Nasaq al-Sha'āmī or Nasak Shamiya was the title for three other stars: Beta Serpentis as Nasak Shamiya I, Gamma Serpentis as Nasak Shamiya II and Gamma Herculis as Nasak Shamiya III.
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