Iota Leporis

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Iota Leporis

A light curve for AM Leporis, adapted from Huélamo et al. (2004)[1]
Observation data
Epoch J2000.0      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 mas[2]
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[edit]

  1. ^ Huélamo, N.; Fernández, M.; Neuhäuser, R.; Wolk, S. J. (December 2004). "Rotation periods of Post-T Tauri stars in Lindroos systems" (PDF). Astronomy and Astrophysics. 428 (3): 953–967. arXiv:astro-ph/0408226. Bibcode:2004A&A...428..953H. doi:10.1051/0004-6361:20034442. S2CID 10656237. Retrieved 29 June 2022.
  2. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  3. ^ a b c d e 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. ^ a b 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, Bibcode:1994AJ....107.1556G, doi:10.1086/116967.
  5. ^ a b 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  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, arXiv:0705.0878, Bibcode:2007AN....328..889K, doi:10.1002/asna.200710776, S2CID 119323941.
  7. ^ a b c d 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, arXiv:astro-ph/0103201, Bibcode:2001A&A...372..152H, doi:10.1051/0004-6361:20010452, S2CID 17507782.
  8. ^ a b c d Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  9. ^ a b c d e 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  10. ^ "iot Lep", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-08-18.
  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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