Astronomy:Iota Leporis

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Short description: Star in the constellation Lepus
Iota Leporis
AMLepLightCurve.png
A light curve for AM Leporis, adapted from Huélamo et al. (2004)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Lepus
Right ascension  05h 12m 17.90190s[2]
Declination −11° 52′ 09.1863″[2]
Apparent magnitude (V) 4.45[3]
Characteristics
Spectral type B7.5 Vn[4] + K7.2 XR? + G8 Ve[5]
U−B color index −0.40[3]
B−V color index −0.10[3]
Astrometry
Radial velocity (Rv)+23.50[6] km/s
Proper motion (μ) RA: +24.39[2] mas/yr
Dec.: −31.02[2] mas/yr
Parallax (π)14.07 ± 0.16[2] mas
Distance232 ± 3 ly
(71.1 ± 0.8 pc)
Absolute magnitude (MV)0.01[7]
Details
ι Lep A
Mass3.37±0.02[8] M☉
Luminosity153[8] L☉
Surface gravity (log g)4.25[9] cgs
Temperature13,781±469[9] K
Rotational velocity (v sin i)185[9] km/s
Age94[7] Myr
Other designations
ι Lep, 3 Lep, BD−12° 1095, GC 6374, HD 33802, HIP 24244, HR 1696, SAO 150223, CCDM J05123-1152A, WDS J05123-1152A[10]
Database references
SIMBADdata

Iota Leporis (ι Leporis) is a triple star[5] system in the southern constellation of Lepus. It is visible to the naked eye as a point source of blue-white light with an apparent visual magnitude of 4.45.[3] Based upon an annual parallax shift of 14.07 mas as measured from Earth,[2] the system is located roughly 232 light years from the Sun.

The primary, designated component A, is a B-type main-sequence star with a stellar classification of B7.5 Vn,[4] where the 'n' suffix indicates "nebulous" absorption lines caused by rotation. It is about 94[7] million years old and has a high rate of spin with a projected rotational velocity of 185 km/s.[9] With an estimated 3.4[8] times the mass of the Sun, it is radiating 153[8] times the Sun's luminosity from its photosphere at an effective temperature of around 13,781 K.[9]

There is a close companion that is a source of X-ray emission. Most likely this star has at least 1.05 times the mass of the Sun.[7] The third component, AM Leporis, is a BY Draconis variable[11] of apparent magnitude 9.92,[3] and spectral type G8Ve[12] at an angular separation of 12.7".[13]

References

  1. ↑ Huélamo, N.; Fernández, M.; Neuhäuser, R.; Wolk, S. J. (December 2004). "Rotation periods of Post-T Tauri stars in Lindroos systems". Astronomy and Astrophysics 428 (3): 953–967. doi:10.1051/0004-6361:20034442. Bibcode: 2004A&A...428..953H. https://www.aanda.org/articles/aa/pdf/2004/48/aa0442-03.pdf. Retrieved 29 June 2022. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Ducati, J. R. (2002), "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system", CDS/ADC Collection of Electronic Catalogues 2237: 0, Bibcode: 2002yCat.2237....0D. 
  4. ↑ 4.0 4.1 Garrison, R. F. et al. (1994), "The late B-type stars: refined MK classification, confrontation with Stromgren photometry, and the effects of rotation", The Astronomical Journal 107 (4): 1556–1564, doi:10.1086/116967, Bibcode: 1994AJ....107.1556G. 
  5. ↑ 5.0 5.1 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  6. ↑ Kharchenko, N. V. et al. (2007), "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations", Astronomische Nachrichten 328 (9): 889, doi:10.1002/asna.200710776, Bibcode: 2007AN....328..889K. 
  7. ↑ 7.0 7.1 7.2 7.3 Hubrig, S. et al. (June 2001), "Search for low-mass PMS companions around X-ray selected late B stars", Astronomy and Astrophysics 372: 152–164, doi:10.1051/0004-6361:20010452, Bibcode: 2001A&A...372..152H. 
  8. ↑ 8.0 8.1 8.2 8.3 Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D. 
  10. ↑ "iot Lep". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+Lep. 
  11. ↑ Kazarovets, E. V. et al. (2008), "The 79th name-list of variable stars", Information Bulletin on Variable Stars 5863 (1): 1, Bibcode: 2008IBVS.5863....1K. 
  12. ↑ Gahm, G. F. et al. (1983), "A study of visual double stars with early type primaries. I - Spectroscopic results", Astronomy and Astrophysics Supplement Series 51: 143–159, Bibcode: 1983A&AS...51..143G. 
  13. ↑ Dommanget, J. et al. (2002), "Catalog of Components of Double & Multiple stars", Observations et Travaux 54 (5), Bibcode: 2002yCat.1274....0D.  Vizier result



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