Astronomy:AK Leporis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[2] mas |
| 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 | |
| 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
- ↑ 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, doi:10.1051/aas:2000243, Bibcode: 2000A&AS..145..275N.
- ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 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, doi:10.1071/AS04013, Bibcode: 2004PASA...21..129N.
- ↑ 4.0 4.1 4.2 Lecavelier Des Etangs, A. et al. (August 2005), "A photometric survey of stars with circumstellar material", Astronomy and Astrophysics 439 (2): 571–574, doi:10.1051/0004-6361:20042401, Bibcode: 2005A&A...439..571L.
- ↑ 5.0 5.1 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M.
- ↑ 6.0 6.1 6.2 Prugniel, Ph. et al. (July 2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics 531: A165, doi:10.1051/0004-6361/201116769, Bibcode: 2011A&A...531A.165P.
- ↑ 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. doi:10.1051/0004-6361:20066503. Bibcode: 2007A&A...469..309C.
- ↑ 8.0 8.1 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, doi:10.1111/j.1365-2966.2012.22132.x, Bibcode: 2012MNRAS.427.2905B.
- ↑ 9.0 9.1 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, doi:10.1088/0004-637X/705/1/89, Bibcode: 2009ApJ...705...89L.
- ↑ "V* AK Lep". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+AK+Lep.
- ↑ Kaler, James B., "Gamma Leporis", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/gammalep.html, retrieved 2015-04-02.
- ↑ 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, doi:10.1051/0004-6361/202140985, Bibcode: 2021A&A...650A.201R. Data available at https://gruze.org/10pc/
- ↑ 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, doi:10.1088/0004-6256/139/1/96, Bibcode: 2010AJ....139...96L.
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