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] |
Distance | 430 ± 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 | |
Mass | 2.75±0.12 [9] M☉ |
Radius | 3.49±0.16 [9] R☉ |
Luminosity | 73 [10] L☉ |
Temperature | 8,616 [11] K |
Rotational velocity (v sin i) | 15 [12] km/s |
TX Leonis Ab | |
Mass | 1.05±0.05 [9] M☉ |
Radius | 2.10±0.09 [9] R☉ |
Luminosity | 6.0 [10] L☉ |
Temperature | 6,266 [10] K |
Age | 850 [13] Myr |
B | |
Mass | 1.75 [14] M☉ |
Surface gravity (log g) | 4.24 [11] cgs |
Temperature | 6,338 [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 | |
SIMBAD | data |
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]