V1005 Orionis

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V1005 Orionis

Ultraviolet (U band) light curves for two flares on V1005 Orionis, adapted from Byrne et al. (1984)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Right ascension 04h 59m 34.834s[2]
Declination +01° 47′ 00.67″[2]
Apparent magnitude (V) 10.107±0.053[3] (9.96 to 10.17)[4]
Characteristics
Evolutionary stage Main sequence
Spectral type M0Ve[5]
B−V color index 1.394±0.020[6]
Variable type
UV Cet[4]
Distance
79.57 ± 0.02 ly
(24.396 ± 0.008 pc)
Absolute magnitude (MV)7.96[8]
Details
Myr
HIP 23200[13]
Database references
SIMBADdata

V1005 Orionis is a young

light years from the Sun and is drifting further away with a radial velocity of 19.2 km/s.[7] The star is a possible member of the IC 2391 supercluster.[14][15]

Flare activity was first reported for this star by N. I. Shakhovskaya in 1974.[16] B. W. Bopp found anomalously strong lithium lines in the spectrum of GJ 182, a rarity for stars of this class and a possible indicator of a very young star.[17] Together with F. Espenak, in 1977 Bopp demonstrated the star showed periodic variations similar to BY Draconis.[18] In 1984, Byrne and associates found a preliminary rotation period of 4.55 days and showed the star had a normal flare rate.[1]

The

star spots and undergoes sudden increases in brightness from flares.[12] Because of this activity, the star displays a low level of X-ray emission.[19][9] The surface magnetic field strength is 2.6±0.6 kG and the magnetic field has multiple poles.[20] It shows a possible activity cycle with a period of 38 years and an amplitude of 0.13 in magnitude.[21]

This star is an estimated 25 million years old and is currently about a half magnitude above the

projected rotational velocity of ~9 km/s, and a rotation period of 4.4 days suggests it is being viewed from close to the equatorial plane.[7] The star has less mass, a smaller radius, and a lower luminosity compared to the Sun.[9]

V1005 Ori is surrounded by a

circumstellar disk of dust that indicates planetary formation is under way.[15] This disk has a radius of 60 AU, a mean temperature of 27 K, and a dust mass equal to 3.35 times the mass of the Moon.[22] A candidate sub-stellar companion was identified in 2001, but this was determined to be a background object.[23]

References

  1. ^
    doi:10.1093/mnras/206.4.907
    .
  2. ^
    doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR
    .
  3. ^
    Bibcode:2012AcA....62...67K
    .
  4. ^
    S2CID 125853869
    .
  5. ^
    S2CID 16080025
    . See the online data.
  6. ^
    S2CID 119257644
    .
  7. ^
    doi:10.1093/mnras/stx3246
    .
  8. Bibcode:2007AcA....57..149K
    .
  9. ^
    S2CID 215238408
    , A20.
  10. S2CID 117144290
    .
  11. ^
    S2CID 119234492
    .
  12. ^
    doi:10.1093/pasj/63.2.427
    .
  13. ^ "V1005 Ori", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2022-02-16.
  14. S2CID 55727428
    .
  15. ^
    S2CID 7782631
    .
  16. Bibcode:1974IBVS..897....1S
    .
  17. S2CID 121809163
    .
  18. doi:10.1086/112146
    .
  19. ISBN 1-58381-082-X
    .
  20. S2CID 119182560
    , 0184.
  21. S2CID 227054200
    .
  22. doi:10.1051/0004-6361:20065873
    .
  23. ISBN 1-58381-082-X
    .

Further reading

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