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Suspected variable in Sextans. From Wikipedia, the free encyclopedia
HD 85709 (HR 3915; 14 G. Sextantis; NSV 18292) is a solitary star[15] located in the equatorial constellation Sextans. It is faintly visible to the naked eye as a red-hued point of light with an apparent magnitude of 5.95.[2] The object is located relatively far at a distance of 1,100 light-years based on Gaia DR3 parallax measurements but it is slowly drifting closer with a heliocentric radial velocity of −0.66 km/s.[8] At its current distance, HD 85709's brightness is diminished with an interstellar extinction of two-tenths of a magnitude[16] and it has an absolute magnitude of −1.30.[9]
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Sextans |
Right ascension | 09h 53m 42.92424s[1] |
Declination | +05° 57′ 30.8742″[1] |
Apparent magnitude (V) | 5.95[2] (5.89 - 5.95)[3] |
Characteristics | |
Evolutionary stage | AGB[4] |
Spectral type | M2.5 III[5] |
U−B color index | +1.93[6] |
B−V color index | +1.66[6] |
Variable type | suspected[7] |
Astrometry | |
Radial velocity (Rv) | −0.66±0.40[8] km/s |
Proper motion (μ) | RA: −3.026 mas/yr[1] Dec.: +1.315 mas/yr[1] |
Parallax (π) | 2.9474 ± 0.107 mas[1] |
Distance | 1,110 ± 40 ly (340 ± 10 pc) |
Absolute magnitude (MV) | −1.30[9] |
Details | |
Radius | 133±7[10] R☉ |
Luminosity | 1,918±144[11] L☉ |
Surface gravity (log g) | 0.469[12] cgs |
Temperature | 3,622±125[12] K |
Metallicity [Fe/H] | +0.23[13] dex |
Other designations | |
Database references | |
SIMBAD | data |
HD 85709 has a stellar classification of M2.5 III,[5] indicating that it is an evolved M-type giant star. It is currently on the asymptotic giant branch,[4] the point where it is generating energy via the fusion of hydrogen and helium shells around an inert carbon core. Having expanded to 133 times the radius of the Sun,[10] it now radiates 1,918 times the luminosity of the Sun[11] from its enlarged photosphere at an effective temperature of 3,622 K.[12] HD 85709 is metal enriched with an iron abundance 1.58 times that of the Sun's.[13]
In 1991, astronomer V.G. Kornilov and colleagues observed that HD 85709 fluctuated between magnitudes 5.89 and 5.95 in optical light during a photometry survey.[3] As of 2004 however, its variability has not been confirmed.[17]
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