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Star in the constellation of Leo Minor From Wikipedia, the free encyclopedia
8 Leonis Minoris (8 LMi) is a solitary,[14] red hued star located in the northern constellation Leo Minor. It has an apparent magnitude 5.37,[2] making it faintly visible to the naked eye. Based on parallax measurements from the Gaia satellite, the object is estimated to be 492 light years distant.[1] It is receding with a heliocentric radial velocity of 40 km/s.[6] At its current distance, 8 LMi is diminshed by 0.12 magnitudes due to interstellar dust.[15]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Leo Minor |
Right ascension | 09h 31m 32.41045s[1] |
Declination | +35° 06′ 11.7793″[1] |
Apparent magnitude (V) | 5.37[2] |
Characteristics | |
Evolutionary stage | AGB[3] |
Spectral type | M1 IIIab[4] |
U−B color index | +1.81[2] |
B−V color index | +1.53[2] |
Variable type | suspected[5] |
Astrometry | |
Radial velocity (Rv) | 39.83±0.18[6] km/s |
Proper motion (μ) | RA: −54.488 mas/yr[1] Dec.: −97.434 mas/yr[1] |
Parallax (π) | 6.6271 ± 0.0238 mas[1] |
Distance | 492 ± 2 ly (150.9 ± 0.5 pc) |
Absolute magnitude (MV) | −0.43[7] |
Details | |
Mass | 1.59[8] M☉ |
Radius | 48.5[9] R☉ |
Luminosity | 417±17[10] L☉ |
Surface gravity (log g) | 1.153[11] cgs |
Temperature | 3,978±122[12] K |
Metallicity [Fe/H] | −0.25[1] dex |
Other designations | |
Database references | |
SIMBAD | data |
This is an asymptotic giant branch star[3] with stellar classification of M1 IIIab.[4] It has 1.59 times the mass of the Sun[8] but has expanded to 48.5 times its girth.[9] It radiates 417 times the luminosity of the Sun[10] from its enlarged photosphere at an effective temperature of 3,978 K.[12] 8 LMi has an iron abundance only half of the Sun's, making it metal deficient.[1]
8 LMi's variability was first observed to be variable in 1930 by Joel Stebbins.[16] However, Eggen (1967) instead lists it as an ordinary M-type giant and used the object for comparison.[17] In 1978-9, 8 LMi was again listed as a variable star but did not provide further insight.[18] As of 2017, the star has not been confirmed to be variable.[5]
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