Kappa1 Ceti

Source: Wikipedia, the free encyclopedia.
For other stars with this Bayer designation, see κ Ceti.
κ1 Ceti
Location of κ1 Ceti (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cetus
Right ascension 03h 19m 21.6960s[1]
Declination +03° 22′ 12.712″[1]
Apparent magnitude (V) 4.84[2]
Characteristics
Spectral type G5Vv[3]
U−B color index +0.185[4]
B−V color index +0.674[4]
Variable type BY Dra[5]
Distance
29.81 ± 0.07 ly
(9.14 ± 0.02 pc)
Absolute magnitude (MV)5.16[7]
Details
Myr
LTT
 11094
Database references
SIMBADdata
ARICNSdata

Kappa1 Ceti,

yellow dwarf star approximately 30 light-years away[1] in the equatorial constellation of Cetus
.

The star was discovered to have a rapid rotation, roughly once every nine days. Though there are no

extrasolar planets confirmed to be orbiting the star, Kappa1 Ceti is considered a good candidate to contain terrestrial planets, like the Earth. The system is a candidate binary star, but has not been confirmed.[12]

Description

A light curve for Kappa1 Ceti, plotted from Hipparcos data[13]

Kappa1 Ceti is a

spectrum of this star has served as one of the stable anchor points by which other stars are classified.[14] The star has roughly the same mass as the Sun, with 95% of the Sun's radius[8] but only 85 percent of the luminosity.[9] Its brightness varies by a few hundredths of a magnitude over a period of nine days and it is classified as a BY Draconis variable, a type of variable star where the brightness changes are due to spots on its surface as it rotates.[5]

The rapid rotation rate of this star, approximately once every nine days, is indicative of a relatively youthful body several hundred million years in age. Due to starspots, the star varies slightly over approximately the same period. The variations in the period are thought to be caused by differential rotation at various latitudes, similar to what happens on the surface of the Sun. The starspots on Kappa1 Ceti range in latitude from 10° to 75°[9] The magnetic properties of this star make it "an excellent match for the Sun at a key point in the Earth's past".[15]

According to recent hypotheses, unusually intense stellar flares from a

coronal mass ejections) that release between 100 and 10 million times more energy than the largest flares ever observed on the sun, making them brighten briefly by up to 20 times.[16]

Magnetic field measurements for κ1 Ceti were reported in 2016.[17] These authors used spectropolarimetric observations from NARVAL to reconstruct the magnetic field topology and to quantitatively investigate the interactions between the stellar wind and a possible surrounding planetary system. A magnetic field detection was reported for κ1 Ceti[17]., with an average field strength of 24 G, and a maximum value of 61 G. Stellar wind model [17] shows a mass-loss rate of 9.7×10−13 M☉·yr−1, i.e., 50 times larger than the current solar wind mass-loss rate.[17] Recent data constrained model of the star suggests that its mass loss rate is as high as 100 times of the solar mass-loss rate.[18]

The

moving group of stars.[9]

See also

References

  1. ^
    S2CID 18759600. Vizier catalog entry
  2. ^
    S2CID 18993744
    .
  3. ^
    S2CID 55727428
    .
  4. ^
    Bibcode:1984SAAOC...8...59C
    .
  5. ^
    S2CID 125853869
    .
  6. Bibcode:1967IAUS...30...57E
    .
  7. Bibcode:1999A&A...343..222E
    .
  8. ^
    S2CID 15937336
    .
  9. ^
    S2CID 16930014
    .
  10. ^
    S2CID 16602121
    .
  11. S2CID 27151456
    .
  12. doi:10.1086/131309
    .
  13. ^ "/ftp/cats/more/HIP/cdroms/cats". Centre de Données astronomiques de Strasbourg. Strasbourg astronomical Data Center. Retrieved 15 October 2022.
  14. Bibcode:1993AAS...183.1710G. Archived from the original
    on 2019-06-25. Retrieved 2012-02-04.
  15. doi:10.1017/S1743921309992298
    .
  16. ^
    S2CID 10586370
    .
  17. ^
    S2CID 118483378
    .
  18. S2CID 235294099
    .

External links
Retrieved from "https://en.wikipedia.org/w/index.php?title=Kappa1_Ceti&oldid=1186943571"