TX Leonis

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]

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  16. ^ Cite error: The named reference Meyer1933 was invoked but never defined (see the help page).
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  18. ^ Cite error: The named reference Mason was invoked but never defined (see the help page).