TX Leonis

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TX Leonis

A light curve for TX Leonis, plotted from TESS data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Leo
Right ascension 10h 35m 02.15893s[2]
Declination +08° 39′ 01.5434″[2]
Apparent magnitude (V) 5.66 - 5.75[3]
Characteristics
Spectral type A2V[4]
B−V color index 0.059[5]
Variable type Algol/detached[3][6]
Astrometry
Proper motion (μ) RA: −52.68±0.73[2] mas/yr
Dec.: −4.23±0.46[2] mas/yr
Parallax (π)7.61 ± 0.67 mas[2]
Distance430 ± 40 ly
(130 ± 10 pc)
Absolute magnitude (MV)0.458[5]
Orbit
Period (P)2.4450566 d[7]
Eccentricity (e)0.060±0.010[8]
Inclination (i)66.8[7]°
Argument of periastron (ω)
(secondary)		295.9±9[7]°
Argument of periastron (ω)
(primary)		[8]°
Details
TX Leonis Aa
Mass2.75±0.12[9] M☉
Radius3.49±0.16[9] R☉
Luminosity73[10] L☉
Temperature8,616[11] K
Rotational velocity (v sin i)15[12] km/s
TX Leonis Ab
Mass1.05±0.05[9] M☉
Radius2.10±0.09[9] R☉
Luminosity6.0[10] L☉
Temperature6,266[10] K
Age850[13] Myr
B
Mass1.75[14] M☉
Surface gravity (log g)4.24[11] cgs
Temperature6,338[11] K
Metallicity [Fe/H]−0.24[11] dex
Other designations
49 Leonis, BD+09 2374, HD 91636, HIP 51802, HR 4148, SAO 118380[15]
Database references
SIMBADdata

TX Leonis, also known by its Flamsteed designation 49 Leonis, is a triple star system that includes an eclipsing binary, located in the constellation Leo. It was discovered to be a variable star, showing eclipses, by Ernst-Joachim Meyer in 1933.[16] The apparent magnitude of TX Leonis ranges between 5.66 and 5.75, making it faintly visible to the naked eye for an observer located well outside of urban areas.[3] The star's brightness drops by 0.09 and 0.03 magnitudes during the primary and secondary eclipses respectively, and neither the primary nor the secondary eclipse is total.[6]

TX Leonis is a triple star, consisting of magnitude 8.1 star (component B) separated by 2 arc seconds from the brighter eclipsing pair (components Aa and Ab).[17][18] Although orbital motion has not been detected, the companion shares a common proper motion with the primary star and is at approximately the same distance.[14]

Both stars comprising the eclipsing binary are main sequence stars. Of those two stars, star Aa has been assumed to be 8 times more luminous than star Ab,[7] although newer estimates give the luminosities as 83 L☉ and 6 L☉ respectively.[10]

References[edit]

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 January 2023.
  2. ^ a b c d e van Leeuwen, Floor (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. eISSN 1432-0746. ISSN 0004-6361.
  3. ^ a b c Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ^ Giuricin, G.; Mardirossian, F.; Mezzetti, M. (February 1984). "Synchronization in eclipsing binary stars". Astronomy and Astrophysics. 131: 152–158. Bibcode:1984A&A...131..152G.
  5. ^ a b Bilir, S.; Ak, T.; Soydugan, E.; Soydugan, F.; Yaz, E.; Filiz Ak, N.; Eker, Z.; Demircan, O.; Helvaci, M. (October 2008). "New absolute magnitude calibrations for detached binaries". Astronomische Nachrichten. 329 (8): 835. arXiv:0806.1290. Bibcode:2008AN....329..835B. doi:10.1002/asna.200811002. S2CID 6131326.
  6. ^ a b Avvakumova, E. A.; Malkov, O. Yu.; Kniazev, A. Yu. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten. 334 (8): 860. Bibcode:2013AN....334..860A. doi:10.1002/asna.201311942. hdl:10995/27061.
  7. ^ a b c d Srivastava, J. B.; Kandpal, C. D. (January 1968). "Photoelectric elements of the eclipsing binary TX Leo". Bulletin of the Astronomical Institute of Czechoslovakia. 19: 381. Bibcode:1968BAICz..19..381S.
  8. ^ a b Chamberlin, Carl; McNamara, D. H. (October 1957). "The Orbit of the Eclipsing Binary TX Leonis". Publications of the Astronomical Society of the Pacific. 69 (410): 462. Bibcode:1957PASP...69..462C. doi:10.1086/127125. S2CID 120162415.
  9. ^ a b c d Dryomova, G. N.; Svechnikov, M. A. (April 2007). "Effect of tidal evolution in determining the ages of eclipsing-variable early main sequence close binary systems". Astrophysics. 50 (2): 239–253. Bibcode:2007Ap.....50..239D. doi:10.1007/s10511-007-0023-9. S2CID 121459015.
  10. ^ a b c d De Greve, J. P.; Vanbeveren, D. (1980). "Close Binary Systems Before and after Mass Transfer - a Comparison of Observations and Theory". Astrophysics and Space Science. 68 (2): 433. Bibcode:1980Ap&SS..68..433D. doi:10.1007/BF00639709. S2CID 123281741.
  11. ^ a b c d Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. S2CID 131780028.
  12. ^ Abt, Helmut A.; Boonyarak, Chayan (November 2004). "Tidal Effects in Binaries of Various Periods". The Astrophysical Journal. 616 (1): 562–566. Bibcode:2004ApJ...616..562A. doi:10.1086/423795.
  13. ^ Pan, K. -K (1997). "Synchronization in the early-type detached binary stars". Astronomy and Astrophysics. 321: 202. Bibcode:1997A&A...321..202P.
  14. ^ a b Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. S2CID 119047709.
  15. ^ "49 Leo -- Eclipsing Binary". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-01-08.
  16. ^ Meyer, Ernst-Joachim (May 1933). "Neuer heller Bedeckungsveränderlicher 61.1933 Leonis". Astronomische Nachrichten. 248 (23): 419. Bibcode:1933AN....248..419M. doi:10.1002/asna.19332482308.
  17. ^ 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.
  18. ^ Mason, Brian D.; Hartkopf, William I.; Wycoff, Gary L.; Rafferty, Theodore J.; Urban, Sean E.; Flagg, Laura (December 2004). "Speckle Interferometry at the US Naval Observatory. X.". The Astronomical Journal. 128 (6): 3012–3018. Bibcode:2004AJ....128.3012M. doi:10.1086/425532.
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