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Kruger 60

Encyclopedia : K : KR : KRU : Kruger 60


|- style="vertical-align: top;" | B-V color index | |- style="vertical-align: top;" | U-B color index | |- style="vertical-align: top;" | Variable type |

|- ! style="background-color: #FFFFC0;" colspan="2" | Details |- |style="vertical-align: baseline;" | Mass | M |- |style="vertical-align: baseline;" | Radius | R |- |style="vertical-align: baseline;" | Luminosity | L |- |style="vertical-align: baseline;" | Temperature | K |- |style="vertical-align: baseline;" | Metallicity | |- |style="vertical-align: baseline;" | Rotation | |- |style="vertical-align: baseline;" | Age | })<()or(}})=()and(}})<())}}} years

|- ! style="background-color: #FFFFC0;" colspan="2" | Visual binary orbit |- style="vertical-align: top;" | Companion | Kruger 60 B |- style="vertical-align: top;" | Period (P) | 44.67 years |- style="vertical-align: top;" | Semimajor axis (a) | 2.383" |- style="vertical-align: top;" | Eccentricity (e) | 0.41 |- style="vertical-align: top;" | Inclination (i) | 167.2° |- style="vertical-align: top;" | Node (Ω) | 154.5° |- style="vertical-align: top;" | Periastron epoch (T) | 1970.22

|- ! style="background-color: #FFFFC0;" colspan="2" | Other designations |- | colspan="2" |

DO Cephei, Gl 232-075, GJ 860 A/B, BD +56°2783, HD 239960, LHS 3814/3815, GCTP 5438.00, ADS 15972, Vys 207 A/B, HIP 239960.
|} Kruger 60 is a binary star system composed of A and B components, both of which are red dwarf stars. These stars orbit each other every 44.6 years. The fainter companion B is a flare star and has been given the variable star designation "DO Cephei". It is an irregular flare that typically doubles in brightness and then returns to normal over an 8 minute period.

On average, the two stars are separated by 9.5 AUs, which is roughly the average distance of Saturn from the Sun. However, their eccenctric mutual orbit causes their distance to vary between 5.5 AUs at periastron, to 13.5 at apastron.

Reference

James Kaler, Extreme Stars, (Cambridge: Cambridge UP, 2001), p. 32.

See also

 


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