Английская Википедия:AE Ursae Majoris

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Шаблон:Short description Шаблон:Starbox begin Шаблон:Starbox image Шаблон:Starbox observe Шаблон:Starbox character Шаблон:Starbox astrometry Шаблон:Starbox detail Шаблон:Starbox catalog Шаблон:Starbox reference Шаблон:Starbox end

AE Ursae Majoris is a star in the northern circumpolar constellation of Ursa Major, abbreviated AE UMa. It is a variable star that ranges in brightness from a peak apparent visual magnitude of 10.86 down to 11.52.[1] The distance to this star is approximately 2,400 light years based on parallax measurements.[2]

The variability of this star was announced by E. Geyer and associates in 1955.[3] V. P. Tsesevich in 1973 found it to be a dwarf cepheid with a period of 0.086017 days, and he noticed it showed amplitude variations in the light curve.[4] In 1974, B. Szeidl determined a secondary period of 0.066529 days,[5] while P. Broglia and P. Conconi found a beat period of 0.294 days.[6] It belonged to a group of high amplitude, double mode Delta Scuti variables that included SX Phoenicis,[7] and by 1995 it was classified as a SX Phoenicis variable and a possible halo object. However, E. Hintz and associates in 1997 found strong evidence against this classification.[4][8]

In 2001, the overtone pulsation period of this star was shown to change at the rate of Шаблон:Val.[9] In addition, possible sudden jumps in the period have been observed, a property it has in common with VZ Cancri.[10] With an estimated mass 1.8 times that of the Sun and an age of a billion years, it is an evolved star that has left the main sequence and is generating energy on a hydrogen-burning shell surrounding a helium core. The metallicity suggests it is a population I Delta Scuti variable. Currently it is crossing the Hertzsprung gap.[8]

References

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Further reading

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Шаблон:Stars of Ursa Major

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