AK Leporis

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AK Leporis
AKLepLightCurve.png
A visual band light curve for AK Leporis, adapted from Nitschelm et al. (2000) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Lepus
Right ascension 05h 44m 26.537s [2]
Declination −22° 25′ 18.61″ [2]
Apparent magnitude  (V)6.141 [3]
Characteristics
Evolutionary stage main sequence [2]
Spectral type K2V [4]
U−B color index +0.74 [5]
B−V color index +0.96 [5]
Variable type BY Draconis [4]
Astrometry
Radial velocity (Rv)−9.80±0.12 [2] km/s
Proper motion (μ)RA: −304.905 [2] mas/yr
Dec.: −352.606 [2] mas/yr
Parallax (π)112.4661±0.0151  mas [2]
Distance 29.000 ± 0.004  ly
(8.892 ± 0.001  pc)
Absolute magnitude  (MV)6.31 [3]
Details
Mass 0.800+0.040
−0.048 [2]   M☉
Radius 0.793±0.017 [2]   R☉
Luminosity 0.300±0.005 [2]   L☉
Surface gravity (log g)4.66±0.01 [6]   cgs
Temperature 4,869±61 [6]   K
Metallicity [Fe/H]0.01±0.06 [6]   dex
Rotation 17.3 days [7]
Rotational velocity (v sin i)2.8±1.8 [8]  km/s
Age 0.9 [9]   Gyr
Other designations
γ Lep B, AK Lep, BD−22 1210, GJ 216 B, HD 38392, HR 1982, SAO 170757, LTT 2363 [10]
Database references
SIMBAD data

AK Leporis, also known as Gamma Leporis B, is a variable star in the southern constellation of Lepus the hare. It has an apparent visual magnitude of 6.141, [3] so, according to the Bortle scale, it is faintly visible from rural skies at night. This star forms a wide binary star system with Gamma Leporis—the two have an angular separation of 97″, making them difficult to separate with the naked eye even under the best conditions. [11] [12] Both Gamma Leporis and AK Leporis are members of the Ursa Major Moving Group of stars that share a common motion through space. [8]

This is a BY Draconis variable star that undergoes slight brightness variations due to stellar activity. Differential rotation causes changes to the periodicity of the variation depending on the latitude of the activity. [4] X-ray emission has been detected from AK Leporis, and it is located at or near a radio source. [13]

Infrared observation of this star shows a large excess at a wavelength of 24 μm. This may be explained by the proximity of Gamma Leporis to the line of sight, or there may be a red dwarf companion or a dust disc. There is no excess observed at 70 μm. [9]

See also

References

  1. ↑ Nitschelm, C.; des Etangs, A. Lecavelier; Vidal-Madjar, A.; Ferlet, R.; Olsen, E. H.; Dennefeld, M. (August 2000), "A three-year Strömgren photometric survey of suspected β Pictoris-like stars", Astronomy and Astrophysics Supplement Series, 145 (2): 275–281, Bibcode:2000A&AS..145..275N, doi: 10.1051/aas:2000243 .
  2. 1 2 3 4 5 6 7 8 9 10 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 Nordström, Andersen; et al. (2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Publications of the Astronomical Society of Australia, 21 (2): 129–133, Bibcode:2004PASA...21..129N, doi: 10.1071/AS04013 .
  4. 1 2 3 Lecavelier Des Etangs, A.; et al. (August 2005), "A photometric survey of stars with circumstellar material", Astronomy and Astrophysics, 439 (2): 571–574, Bibcode:2005A&A...439..571L, doi: 10.1051/0004-6361:20042401 .
  5. 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  6. 1 2 3 Prugniel, Ph.; et al. (July 2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics, 531: A165, arXiv: 1104.4952 , Bibcode:2011A&A...531A.165P, doi:10.1051/0004-6361/201116769, S2CID   54940439.
  7. ↑ Cincunegui, C.; Díaz, R. F.; Mauas, P. J. D. (2007). "Hα and the Ca II H and K lines as activity proxies for late-type stars". Astronomy and Astrophysics. 469 (1): 309. arXiv: astro-ph/0703511 . Bibcode:2007A&A...469..309C. doi:10.1051/0004-6361:20066503.
  8. 1 2 Biazzo, K.; et al. (December 2012), "Elemental abundances of low-mass stars in nearby young associations: AB Doradus, Carina Near and Ursa Major", Monthly Notices of the Royal Astronomical Society, 427 (4): 2905–2916, arXiv: 1209.2591 , Bibcode:2012MNRAS.427.2905B, doi: 10.1111/j.1365-2966.2012.22132.x , S2CID   118617986.
  9. 1 2 Lawler, S. M.; et al. (November 2009), "Explorations Beyond the Snow Line: Spitzer/IRS Spectra of Debris Disks Around Solar-type Stars", The Astrophysical Journal, 705 (1): 89–111, arXiv: 0909.0058 , Bibcode:2009ApJ...705...89L, doi:10.1088/0004-637X/705/1/89, S2CID   1272803.
  10. ↑ "V* AK Lep", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2015-04-02.
  11. ↑ Kaler, James B., "Gamma Leporis", Stars, University of Illinois , retrieved 2015-04-02.
  12. ↑ Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021), "The 10 parsec sample in the Gaia era", Astronomy & Astrophysics , 650: A201, arXiv: 2104.14972 , Bibcode:2021A&A...650A.201R, doi:10.1051/0004-6361/202140985, S2CID   233476431. Data available at https://gruze.org/10pc/ Archived 12 March 2023 at the Wayback Machine
  13. ↑ Lazio, T. Joseph W.; et al. (January 2010), "A Blind Search for Magnetospheric Emissions from Planetary Companions to Nearby Solar-Type Stars", The Astronomical Journal, 139 (1): 96–101, arXiv: 0910.3938 , Bibcode:2010AJ....139...96L, doi:10.1088/0004-6256/139/1/96, S2CID   118537554.
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