Astronomy:AO Mensae

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AO Mensae
Observation data
[[Astronomy:Epoch|Epoch J2000]]      Equinox J2000
Constellation Mensa
Right ascension  06h 18m 28.20850s[1]
Declination −72° 02′ 41.4464″[1]
Apparent magnitude (V) 9.96 to 10.18[2]
Characteristics
Spectral type K4Ve[3]
B−V color index +1.13[4]
Variable type BY Dra[2]
Astrometry
Radial velocity (Rv)+16.2±1.0[5] km/s
Proper motion (μ) RA: −7.908[1] mas/yr
Dec.: +74.295[1] mas/yr
Parallax (π)25.4695 ± 0.0254[1] mas
Distance128.1 ± 0.1 ly
(39.26 ± 0.04 pc)
Absolute magnitude (MV)7.02[6]
Details[5]
Mass0.69 M
Radius0.91±0.29[7] R
Luminosity0.26 L
Surface gravity (log g)4.38 cgs
Temperature4,384±59 K
Metallicity [Fe/H]0.24 dex
Rotation2.673 d
Rotational velocity (v sin i)16.4 km/s
Age23±3[8] Myr
Other designations
AO Men, CD−71°333, CPD−71° 427, HD 45081, HIP 29964[9]
Database references
SIMBADdata

AO Mensae is a single[7] variable star in the southern circumpolar constellation of Mensa. It is too faint to be viewed with the naked eye, having an apparent visual magnitude that ranges from 9.96 down to 10.18.[2] The star is 128 light years distant from the Sun based on parallax,[1] and is drifting further away with a radial velocity of +16 km/s.[5] It is a member of the Beta Pictoris moving group, a loose association of young stars moving through the galaxy.[7]

This is an orange-hued K-type main-sequence star with a stellar classification of K4Ve,[3] where the 'e' suffix indicates emission features in the spectrum. It is young star and an X-ray source, one of the brightest such X-ray emitters in the solar neighborhood,[10] and is categorized as a BY Draconis variable, although there is some uncertainty in this assignment.[2] It is spinning with a period of 2.7[5] days and is about 23[8] million years old. The star has 69%[5] of the mass of the Sun and 91%[7] of the Sun's radius. It is radiating 26% of the luminosity of the Sun on average, at an effective temperature of 4,384 K.

References

  1. 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. 2.0 2.1 2.2 2.3 Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode2017ARep...61...80S. 
  3. 3.0 3.1 Torres, C. A. O. et al. (2006). "Search for associations containing young stars (SACY)". Astronomy & Astrophysics 460 (3): 695. doi:10.1051/0004-6361:20065602. Bibcode2006A&A...460..695T. 
  4. Messina, S. et al. (2010). "RACE-OC project: Rotation and variability of young stellar associations within 100 pc". Astronomy and Astrophysics 520: A15. doi:10.1051/0004-6361/200913644. Bibcode2010A&A...520A..15M. 
  5. 5.0 5.1 5.2 5.3 5.4 Luck, R. Earle (March 2018). "Abundances in the Local Region. III. Southern F, G, and K Dwarfs". The Astronomical Journal 155 (3): 31. doi:10.3847/1538-3881/aaa9b5. 111. Bibcode2018AJ....155..111L. 
  6. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode2012AstL...38..331A. 
  7. 7.0 7.1 7.2 7.3 Messina, S. et al. (April 2017). "The β Pictoris association: Catalog of photometric rotational periods of low-mass members and candidate members". Astronomy & Astrophysics 600: 72. doi:10.1051/0004-6361/201629152. A83. Bibcode2017A&A...600A..83M. 
  8. 8.0 8.1 Meshkat, Tiffany et al. (December 2017). "A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems". The Astronomical Journal 154 (6): 21. doi:10.3847/1538-3881/aa8e9a. 245. Bibcode2017AJ....154..245M. 
  9. "AO Men". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=AO+Men. 
  10. Makarov, Valeri V. (October 2003). "The 100 Brightest X-Ray Stars within 50 Parsecs of the Sun". The Astronomical Journal 126 (4): 1996–2008. doi:10.1086/378164. Bibcode2003AJ....126.1996M.