Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Sagittarius |
Right ascension | 18h 31m 53.332s[2] |
Declination | −19° 07′ 30.26″[2] |
Apparent magnitude (V) | 6.28 to 7.15[3] |
Characteristics | |
Evolutionary stage | Supergiant |
Spectral type | G1Ib[4] |
U−B color index | +0.85[5] |
B−V color index | +1.06[5] |
Variable type | δ Cep[3] |
Astrometry | |
Radial velocity (Rv) | 2.2±0.3[6] km/s |
Proper motion (μ) | RA: −1.795 mas/yr[2] Dec.: −6.127 mas/yr[2] |
Parallax (π) | 1.5693 ± 0.0224 mas[2] |
Distance | 2,080 ± 30 ly (637 ± 9 pc) |
Absolute magnitude (MV) | −3.86 to −3.10[5] |
Details | |
Mass | 6.54 to 6.64[7] M☉ |
Radius | 55.5 to 56.3[7] R☉ |
Luminosity | 4,370 to 4,650[7] L☉ |
Surface gravity (log g) | 0.99[8] cgs |
Temperature | 5,802[8] K |
Metallicity [Fe/H] | 0.17[8] dex |
Rotational velocity (v sin i) | 15.4[9] km/s |
Age | 91[10] Myr |
Other designations | |
Database references | |
SIMBAD | data |
U Sagittarii is a variable star in the southern constellation of Sagittarius, abbreviated U Sgr. It is a classical Cepheid variable that ranges in brightness from an apparent visual magnitude of 6.28 down to 7.15, with a pulsation period of 6.745226 days.[3] At its brightest, this star is dimly visible to the naked eye. The distance to this star is approximately 2,080 light years based on parallax measurements,[2] and it is drifting further away with a radial velocity of 2 km/s.[6]
The variability of this star was announced by J. Schmidt in 1866, who found a preliminary period of 6.74784 days.[13] It was later determined to be a variable of the Cepheid type.[14] In 1925, P. Doig assumed that the star is a member of the open cluster Messier 25 (M25), but actual evidence of its membership would not be available until 1932 when P. Hayford made radial velocity measurements of the cluster.[15] Membership in this cluster is now reasonably established,[16] and as such this Cepheid serves as one of the anchors for the cosmic distance scale since the distance to the cluster can be determined independently from the star.[17] Indeed, new research indicates U Sgr's host cluster (M25) may constitute a ternary (triple) star cluster together with NGC 6716 and Collinder 394.[18]
This is an evolved G-type supergiant star with a typical stellar classification of G1Ib.[4] It appears to be making its third traversal of the instability strip with its period changing at the rate of +0.073±0.010 s·yr−1. Elemental abundances are similar to those in the Sun.[17] It has an estimated 6.6 times the mass of the Sun and 56 times the Sun's radius. The star is radiating over 4,000[7] times the Sun's luminosity from its photosphere at an effective temperature of 5,802 K.[8]
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