Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Vulpecula |
Right ascension | 19h 36m 37.7281s [2] |
Declination | 20° 19′ 58.5692″ [2] |
Apparent magnitude (V) | 6.73 - 7.54 [3] |
Characteristics | |
Spectral type | F6Iab-G2 [4] |
Variable type | δ Cep [3] |
Astrometry | |
Proper motion (μ) | RA: 0.906±0.050 [2] mas/yr Dec.: −0.960±0.062 [2] mas/yr |
Parallax (π) | 1.0530 ± 0.0390 mas [2] |
Distance | 3,100 ± 100 ly (950 ± 40 pc) |
Absolute magnitude (MV) | -3.69 [5] |
Orbit [6] | |
Period (P) | 2,510 days |
Eccentricity (e) | 0.675 |
Periastron epoch (T) | 2444800 |
Argument of periastron (ω) (secondary) | 353° |
Semi-amplitude (K1) (primary) | 3.64 km/s |
Details | |
Mass | 6.5 [7] M☉ |
Radius | 60 [7] R☉ |
Surface gravity (log g) | 1.75 - 1.85 [8] cgs |
Temperature | 5,655 - 5,965 [8] K |
Metallicity [Fe/H] | 0.09 [9] dex |
Age | 82 [9] Myr |
Other designations | |
Database references | |
SIMBAD | data |
U Vulpeculae is a variable and binary star in the constellation Vulpecula.
It is a classical Cepheid variable and its apparent magnitude ranges from 6.73 to 7.54 over a precise cycle of 7.99 days. [4] Its variable nature was discovered in 1898 at Potsdam Observatory by Gustav Müller and Paul Kempf. [11]
In 1991 a study of radial velocities showed that it U Vulpeculae is a spectroscopic binary and a full orbit with a period of 2510 days (6.9 years) was first calculated in 1996. [12] [7] The secondary star is invisible and is only known from its effect on the motion of the primary. [6]
W Sagittarii is a multiple star system star in the constellation Sagittarius, and a Cepheid variable star.
RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.
HD 95109 is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude is 6.86.
Y Carinae is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48.
V Centauri is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years away based on parallax.
31 Vulpeculae is a binary star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.56. The system is located approximately 228 light years away from the Sun based on parallax, and it is drifting further away with a radial velocity of +2.25 km/s.
1 Vulpeculae is a class B4IV star in the constellation Vulpecula. Its apparent magnitude is 4.77 and it is approximately 780 light years away based on parallax.
12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.
9 Vulpeculae is a star in the northern constellation of Vulpecula, located about 560 light years away based on parallax. It is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 5.01. The star is moving further from the Earth with a heliocentric radial velocity of +5 km/s.
RS Puppis is a Cepheid variable star around 6,000 ly away in the constellation of Puppis. It is one of the biggest and brightest known Cepheids in the Milky Way galaxy and has one of the longest periods for this class of star at 41.5 days.
S Normae is a yellow supergiant variable star in the constellation Norma. It is the brightest member of the open cluster NGC 6087.
V636 Scorpii is a multiple star system in the constellation Scorpius, 3,000 light years away. The primary is a Classical Cepheid variable and its visual magnitude varies from 6.4 to 6.9.
U Aquilae is a binary star system in the constellation Aquila, Located approximately 614 parsecs (2,000 ly) away from Earth.
TT Aquilae is a Classical Cepheid variable star in the constellation Aquila.
106 Herculis is a variable star in the northern constellation Hercules. It is visible to the naked eye as a faint, red-hued point of light with a baseline apparent visual magnitude of 4.96. Based on its parallax, it is estimated to lie 383 light-years away from the Sun. The star is moving closer to the Earth with a heliocentric radial velocity of -35 km/s.
S Vulpeculae is a variable star located in the constellation Vulpecula. A supergiant star, it is around 382 times the diameter of the Sun.
SV Vulpeculae is a classical Cepheid variable star in the constellation Vulpecula. It is a supergiant at a distance of 8,700 light years.
ZZ Boötis is a star system in the constellation Boötes. It varies from magnitude 6.79 to 7.44 over five days. Based on its parallax, measured by the Gaia spacecraft, it is about 350 light-years away.
U Microscopii is a Mira variable star in the constellation Microscopium. It ranges from magnitude 7 to 14.4 over a period of 334 days. The Astronomical Society of Southern Africa in 2003 reported that observations of U Microscopii were very urgently needed as data on its light curve was incomplete.
HD 62058, is a variable star in the constellation Puppis. It is a rare yellow hypergiant and a candidate member of the open cluster NGC 2439. It is also an MK spectral standard for the class G2 0-Ia.