Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cepheus [1] |
Right ascension | 20h 45m 53.943s [2] |
Declination | +67° 57′ 38.66″ [2] |
Apparent magnitude (V) | 14.58 - 18.08 [3] |
Characteristics | |
Spectral type | A5Ve [4] |
Variable type | T Tau [5] |
Astrometry | |
Proper motion (μ) | RA: 8.228 [6] mas/yr Dec.: −1.976 [6] mas/yr |
Parallax (π) | 2.9100 ± 0.0593 mas [6] |
Distance | 1,120 ± 20 ly (344 ± 7 pc) |
Details | |
Mass | 2.6 [7] M☉ |
Radius | 2.9 [7] R☉ |
Luminosity | 1 [8] - 100 [3] L☉ |
Temperature | 8,150 [8] K |
Age | <1 [3] Myr |
Database references | |
SIMBAD | data |
PV Cephei is a variable star of Orion type located in the constellation of Cepheus at a distance of about 1,100 light-years from Earth. [9] In visible light it varies in brightness from magnitude 17 to 19, making it far too faint to be seen by the naked eye. [10]
PV Cephei's variability was first detected by Martin Cohen, Leonard Vello Kuhi and Eugene A. Harlan, and was announced in 1977. [11] It was given its variable star designation in 1978. [12] The star is embedded within Gyulbudaghian's Nebula, a reflection nebula. As the star's brightness changes, the nebula's shape changes dramatically. [11] [13]
Omicron Persei is a triple star system in the constellation of Perseus. From parallax measurements taken during the Hipparcos mission it is approximately 1,100 light-years from the Sun.
W Sagittarii is a multiple star system star in the constellation Sagittarius, and a Cepheid variable star.
Mu Columbae is a star in the constellation of Columba. It is one of the few O-class stars that are visible to the unaided eye. The star is known to lie approximately 1,900 light years from the Solar System.
CS Camelopardalis is a binary star in reflection nebula VdB 14, in the constellation Camelopardalis.
V354 Cephei is a red supergiant star located within the Milky Way. It is an irregular variable located over 13,000 light-years away from the Sun. It has an estimated radius of 1,139 solar radii. If it were placed in the center of the Solar System, it would extend to between the orbits of Mars and Jupiter.
S Monocerotis, also known as 15 Monocerotis, is a massive multiple and variable star system located in the constellation Monoceros. It is the brightest star in the Christmas Tree open cluster in the area catalogued as NGC 2264.
V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.
HD 110432 is a Be star in the south-east of Crux, behind the center of the southern hemisphere's dark Coalsack Nebula. It has a stellar classification of B1IVe, which means it is a subgiant star of class B that displays emission lines in its spectrum. This is a variable star of the Gamma Cassiopeiae type, indicating it is a shell star with a circumstellar disk of gas about the equator, and has the variable star designation BZ Crucis. It is not known to be a member of a binary system, although it is probably a member of the open cluster NGC 4609. This star is moderately luminous in the X-ray band, with a variable energy emission of 1032–33 erg s−1 in the range 0.2−12 keV. The X-ray emission may be caused by magnetic activity, or possibly by accretion onto a white dwarf companion.
1 Camelopardalis is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately 800 parsecs (2,600 ly) away.
9 Cephei, also known as V337 Cephei, is a variable star in the constellation Cepheus.
Delta Coronae Borealis, Latinized from δ Coronae Borealis, is a variable star in the constellation Corona Borealis. Its apparent magnitude varies regularly between apparent magnitude 4.57 and 4.69, and it is around 170 light-years distant.
Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.
QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.
9 Persei is a single variable star in the northern constellation Perseus, located around 4,300 light years away from the Sun. It has the Bayer designation i Persei; 9 Persei is the Flamsteed designation. This body is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of about 5.2. It is moving closer to the Sun with a heliocentric radial velocity of −15.2 km/s. The star is a member of the Perseus OB1 association of co-moving stars.
HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the Galactic Center.
HD 87643 is a B[e] class binary star embedded in a reflection nebula.
HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.
V419 Cephei is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.
S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.
HD 150193 is a binary star system in the constellation of Ophiuchus. The primary star was identified as a Herbig Ae/Be star with a strong solar wind, losing approximately a tenth of solar mass per million years. It does host a very small debris disk, likely due to disk truncation by the nearby stellar companion. The disk is inclined 38±9° to the plane of sky. It appears to be highly evolved and asymmetric, with indications of flattening and grains growth.