AK Leporis: Difference between revisions

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'''AK Leporis''' is a [[star]] in the southern [[constellation]] of [[Lepus (constellation)|Lepus]] the hare. It has an [[apparent visual magnitude]] of 6.141,<ref name=paas21_2_129/> so, according to the [[Bortle scale]], it is faintly visible from rural skies at night. This star forms a [[double star|visual double]] with [[Gamma Leporis]]—the two have an [[angular separation]] of 97[[arcsecond|″]], making them difficult to separate with the naked eye even under the best conditions.<ref name=kaler/> Both Gamma Leporis and AK Leporis are members of the [[Ursa Major Moving Group]] of stars that share a common motion through space.<ref name=mnras427_4_2905/>
'''AK Leporis''' is a [[variable star]] in the southern [[constellation]] of [[Lepus (constellation)|Lepus]] the hare. It has an [[apparent visual magnitude]] of 6.141,<ref name=paas21_2_129/> so, according to the [[Bortle scale]], it is faintly visible from rural skies at night. This star forms a [[double star|visual double]] with [[Gamma Leporis]]—the two have an [[angular separation]] of 97[[arcsecond|{{pprime}}]], making them difficult to separate with the naked eye even under the best conditions.<ref name=kaler/> Both Gamma Leporis and AK Leporis are members of the [[Ursa Major Moving Group]] of stars that share a common motion through space.<ref name=mnras427_4_2905/>


This is a [[BY Draconis variable]] star that undergoes brightness variations due to stellar activity. [[Differential rotation]] causes changes to the periodicity of the variation depending on the latitude of the activity.<ref name="aa439_2_571"/> [[X-ray astronomy|X-ray emission]] has been detected from AK Leporis, and it is located at or near a [[Radio astronomy|radio]] source.<ref name=aj139_1_96/>
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.<ref name="aa439_2_571"/> [[X-ray astronomy|X-ray emission]] has been detected from AK Leporis, and it is located at or near a [[Radio astronomy|radio]] source.<ref name=aj139_1_96/>


Infrared observation of this star shows a large excess at a wavelength of 24&nbsp;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&nbsp;µm.<ref name=apj705_1_89/>
Infrared observation of this star shows a large excess at a wavelength of 24&nbsp;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&nbsp;μm.<ref name=apj705_1_89/>


==References==
==References==
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| doi=10.1051/0004-6361:20042401
| doi=10.1051/0004-6361:20042401
| postscript=.
| postscript=.
| doi-access=free
| doi-access=free
}}</ref>
}}</ref>


<ref name="Nitschelm">{{cite journal |last1=Nitschelm |first1=C. |last2=des Etangs |first2=A. Lecavelier |last3=Vidal-Madjar |first3=A. |last4=Ferlet |first4=R. |last5=Olsen |first5=E. H. |last6=Dennefeld |first6=M. |title=A three-year Strömgren photometric survey of suspected β Pictoris-like stars |journal=Astronomy and Astrophysics Supplement Series |date=August 2000 |volume=145 |pages=275–281 |doi=10.1051/aas:2000243 |url=https://ui.adsabs.harvard.edu/abs/2000A&AS..145..275N |access-date=19 January 2022}}</ref>
<ref name="Nitschelm">{{citation |postscript=. |last1=Nitschelm |first1=C. |last2=des Etangs |first2=A. Lecavelier |last3=Vidal-Madjar |first3=A. |last4=Ferlet |first4=R. |last5=Olsen |first5=E. H. |last6=Dennefeld |first6=M. |title=A three-year Strömgren photometric survey of suspected β Pictoris-like stars |journal=Astronomy and Astrophysics Supplement Series |date=August 2000 |volume=145 |issue=2 |pages=275–281 |doi=10.1051/aas:2000243 |bibcode=2000A&AS..145..275N |doi-access=free }}</ref>


<ref name=SIMBAD>{{cite simbad
<ref name=SIMBAD>{{cite simbad
| title=V* AK Lep
| title=V* AK Lep
| access-date=2015-04-02
| access-date=2015-04-02
| postscript=.
| mode=cs2 | postscript=.
}}</ref>
}}</ref>


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[[Category:Lepus (constellation)]]
[[Category:Lepus (constellation)]]
[[Category:Double stars]]
[[Category:Double stars]]
[[Category:Ursa Major Moving Group]]
[[Category:Ursa Major moving group]]
[[Category:K-type main-sequence stars]]
[[Category:K-type main-sequence stars]]
[[Category:Objects with variable star designations|Leporis, AK]]
[[Category:Objects with variable star designations|Leporis, AK]]

Latest revision as of 03:13, 11 February 2024

AK Leporis

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
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)9.57±0.13[6] 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]
Distance29.000 ± 0.004 ly
(8.892 ± 0.001 pc)
Absolute magnitude (MV)6.31[3]
Details
Mass0.8[2] M☉
Radius0.8[2] R☉
Luminosity0.3[2] L☉
Surface gravity (log g)4.66±0.01[7] cgs
Temperature4,869±61[7] K
Metallicity [Fe/H]0.01±0.06[7] dex
Rotational velocity (v sin i)2.8±1.8[6] km/s
Age0.9[8] Gyr
Other designations
BD−22 1210, GJ 216 B, HD 38392, HR 1982, LTT 2363, SAO 170757,[9] γ Leporis B[1]
Database references
SIMBADdata

AK Leporis 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 visual double 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.[10] Both Gamma Leporis and AK Leporis are members of the Ursa Major Moving Group of stars that share a common motion through space.[6]

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.[11]

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.[8]

References[edit]

  1. ^ a b 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. ^ a b c d e f g h 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. ^ a b c 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. ^ a b c 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. ^ a b 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. ^ a b c 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.
  7. ^ a b c 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.
  8. ^ a b 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.
  9. ^ "V* AK Lep", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2015-04-02.
  10. ^ Kaler, James B., "Gamma Leporis", Stars, University of Illinois, retrieved 2015-04-02.
  11. ^ 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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