Astronomy:TX Leonis

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Short description: Variable star in the constellation Leo
TX Leonis
TXLeoLightCurve.png
A light curve for TX Leonis, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
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 periapsis (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

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Template:Cite New HIP red.
  3. ↑ 3.0 3.1 3.2 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. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  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. ↑ 5.0 5.1 Bilir, S.; Ak, T.; Soydugan, E.; Soydugan, F.; Yaz, E.; Filiz Ak, N.; Eker, Z.; Demircan, O. et al. (October 2008). "New absolute magnitude calibrations for detached binaries". Astronomische Nachrichten 329 (8): 835. doi:10.1002/asna.200811002. Bibcode: 2008AN....329..835B. 
  6. ↑ 6.0 6.1 Avvakumova, E. A.; Malkov, O. Yu.; Kniazev, A. Yu. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten 334 (8): 860. doi:10.1002/asna.201311942. Bibcode: 2013AN....334..860A. 
  7. ↑ 7.0 7.1 7.2 7.3 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. ↑ 8.0 8.1 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. doi:10.1086/127125. Bibcode: 1957PASP...69..462C. 
  9. ↑ 9.0 9.1 9.2 9.3 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. doi:10.1007/s10511-007-0023-9. Bibcode: 2007Ap.....50..239D. 
  10. ↑ 10.0 10.1 10.2 10.3 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. doi:10.1007/BF00639709. Bibcode: 1980Ap&SS..68..433D. 
  11. ↑ 11.0 11.1 11.2 11.3 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A. et al. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. Bibcode: 2019A&A...628A..94A. 
  12. ↑ Abt, Helmut A.; Boonyarak, Chayan (November 2004). "Tidal Effects in Binaries of Various Periods". The Astrophysical Journal 616 (1): 562–566. doi:10.1086/423795. Bibcode: 2004ApJ...616..562A. 
  13. ↑ Pan, K. -K (1997). "Synchronization in the early-type detached binary stars". Astronomy and Astrophysics 321: 202. Bibcode: 1997A&A...321..202P. 
  14. ↑ 14.0 14.1 Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series 235 (1): 6. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. Bibcode: 2018ApJS..235....6T. 
  15. ↑ "49 Leo -- Eclipsing Binary". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=49+Leo+--+Eclipsing+Binary. 
  16. ↑ Meyer, Ernst-Joachim (May 1933). "Neuer heller Bedeckungsveränderlicher 61.1933 Leonis". Astronomische Nachrichten 248 (23): 419. doi:10.1002/asna.19332482308. Bibcode: 1933AN....248..419M. 
  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. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  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. doi:10.1086/425532. Bibcode: 2004AJ....128.3012M. 



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