Even in 1928, it was calculated that the size of the star must vary by about 20%. Antares was first reported to have a companion star by Johann Tobias Bürg during an occultation on April 13, 1819, although this was not widely accepted and dismissed as a possible atmospheric effect.
It was then observed by Scottish astronomer James William Grant FRSE while in India on 23 July 1844.
Mitchel in 1846, and measured by William Rutter Dawes in April 1847. In 1952, Antares was reported to vary in brightness.
Mitchel in 1846, and measured by William Rutter Dawes in April 1847. In 1952, Antares was reported to vary in brightness.
Other recent estimates of the period have ranged from 880 years for a calculated orbit, to 2,562 years for a simple Kepler's Law estimate. Early measurements of the pair found them to be about apart in 1847–49, or apart in 1848.
Other recent estimates of the period have ranged from 880 years for a calculated orbit, to 2,562 years for a simple Kepler's Law estimate. Early measurements of the pair found them to be about apart in 1847–49, or apart in 1848.
Even in 1928, it was calculated that the size of the star must vary by about 20%. Antares was first reported to have a companion star by Johann Tobias Bürg during an occultation on April 13, 1819, although this was not widely accepted and dismissed as a possible atmospheric effect.
The brightness has been monitored by the American Association of Variable Star Observers since 1945, and it has been classified as an LC slow irregular variable star, whose apparent magnitude slowly varies between extremes of +0.6 and +1.6, although usually near magnitude +1.0.
Mitchel in 1846, and measured by William Rutter Dawes in April 1847. In 1952, Antares was reported to vary in brightness.
On 31 July 2009, Antares was occulted by the Moon.
The diameter of the limb-darkened disk was measured as in 2009 and in 2010.
The last cycle ended in 2010 and the next begins in 2023.
The diameter of the limb-darkened disk was measured as in 2009 and in 2010.
There is also considerable variation between values published by different authors, for example and published in 2012 and 2013. The mass of the star has been calculated to be about , or .
There is also considerable variation between values published by different authors, for example and published in 2012 and 2013. The mass of the star has been calculated to be about , or .
In 2016, the International Astronomical Union organised a Working Group on Star Names (WGSN) to catalog and standardise proper names for stars.
The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN, which included Antares for the star α Scorpii A.
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Page generated on 2021-08-05