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Binary star system in the constellation of Leo Minor From Wikipedia, the free encyclopedia
40 Leonis Minoris (40 LMi) is a white hued star located in the northern constellation Leo Minor. It is rarely called 14 H. Leonis Minoris, which is the designation given by Polis astronomer Johann Hevelius.[13]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Leo Minor |
Right ascension | 10h 43m 01.88241s[1] |
Declination | +26° 19′ 32.0287″[1] |
Apparent magnitude (V) | 5.51±0.01[2] |
Characteristics | |
Evolutionary stage | main sequence star[3] |
Spectral type | A4 Vn[4] |
U−B color index | +0.19[5] |
B−V color index | +0.17[5] |
Astrometry | |
Radial velocity (Rv) | 10±4.3[6] km/s |
Proper motion (μ) | RA: −98.971 mas/yr[1] Dec.: −65.543 mas/yr[1] |
Parallax (π) | 21.2215 ± 0.0816 mas[1] |
Distance | 153.7 ± 0.6 ly (47.1 ± 0.2 pc) |
Absolute magnitude (MV) | +2.23[7] |
Details | |
Mass | 1.69[8] M☉ |
Radius | 1.54±0.04[9] R☉ |
Luminosity | 14.3+1.8 −1.6[3] L☉ |
Surface gravity (log g) | 4.30±0.04[9] cgs |
Temperature | 7834±108[10] K |
Metallicity [Fe/H] | −0.15[11] dex |
Rotational velocity (v sin i) | 211[12] km/s |
Age | 207[8] Myr |
Other designations | |
Database references | |
SIMBAD | data |
It has an apparent magnitude of 5.51,[2] making it faintly visible to the naked eye. The object is located relatively close at a distance of 154 light years based on Gaia DR3 parallax measurements[1] but is receding with a somewhat constrained heliocentric radial velocity of 10 km/s.[6] At 40 LMi's current distance, its brightness is diminished by only 0.02 magnitudes due to interstellar dust.[15]
40 LMi is a chemically peculiar A-type main-sequence star with a stellar classification of A4 Vn.[4] This indicates that it is an A4 dwarf with nebulous absorption lines due to rapid rotation. It has 1.69 times the mass of the Sun[8] and 1.54 times its girth.[9] It radiates 14.3 times the luminosity of the Sun[3] from its photosphere at an effective temperature of 7,834 K.[10] The star is estimated to be 207 million years old, having completed 54.6% of its main sequence lifetime.[3] 40 LMi is slightly metal deficient and spins rapidly with a projected rotational velocity of 211 km/s.[12]
This star was part of a 2005 survey regarding proper motions from the Hipparcos satellite.[16] Its proper motion varied, indicating that an unseen companion may cause it. This led to Peter P. Eggleton and Andrei Tokovinin classifying it as an astrometric binary.[17] There also 3 optical companions located near 40 LMi. Their relative positions and brightness are listed below.[18]
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