Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Vela |
HD 92449 | |
Right ascension | 10h 39m 18.3925s [1] |
Declination | −55° 36′ 11.765″ [1] |
Apparent magnitude (V) | 4.29 [2] |
HD 92463 | |
Right ascension | 10h 39m 24.2778s [3] |
Declination | −55° 36′ 25.642″ [3] |
Characteristics | |
Spectral type | G5 IIa [4] + B8 V [5] |
B−V color index | 1.025±0.003 [2] |
Astrometry | |
HD 92449 | |
Radial velocity (Rv) | +20.1±0.7 [6] km/s |
Proper motion (μ) | RA: −19.032(91) mas/yr [1] Dec.: 5.032(90) mas/yr [1] |
Parallax (π) | 4.1595 ± 0.0940 mas [1] |
Distance | 780 ± 20 ly (240 ± 5 pc) |
Absolute magnitude (MV) | −2.76 [2] |
HD 92463 | |
Proper motion (μ) | RA: −18.941(40) mas/yr [3] Dec.: 5.386(42) mas/yr [3] |
Parallax (π) | 4.2647 ± 0.0405 mas [3] |
Distance | 765 ± 7 ly (234 ± 2 pc) |
Details | |
Luminosity | 1370.29 [7] L☉ |
Temperature | 5,100 [7] K |
Other designations | |
A: CD−54 3915, HD 92449, HIP 52154, SAO 238309 | |
B: CD−54 3675, HD 92463, SAO 238313 | |
Database references | |
SIMBAD | HD 92449 |
HD 92463 |
HR 4180 is a double star with components HD 92449 and HD 92463 in the southern constellation of Vela. They are probably members of a binary star system. [8] HR 4180 can be viewed with the naked eye, having an apparent visual magnitude of 4.29. [2] Based upon the annual parallax shift of the two stars it is located approximately 780 light years from the Sun. [1] [3] The system is moving further from the Earth with a heliocentric radial velocity of +20 km/s. [6]
The primary component of this system, HD 92449, is a bright giant with a stellar classification of G5 IIa. [4] The star radiates 1,370 times the Sun's luminosity from its photosphere at an effective temperature of 5,100 K. [7] It shares a common proper motion with the magnitude 6.06 [9] star HD 92463, [10] and the pair likely form a binary system. [8] This secondary component is a B-type main-sequence star with a class of B8 V. [5] As of 2000, it had an angular separation of 51.70″ along a position angle of 105° from the primary. [9]
Zeta Andromedae is a star system in the constellation Andromeda. It is approximately 189 light-years from Earth.
8 Andromedae, abbreviated 8 And, is a probable triple star system in the northern constellation of Andromeda. 8 Andromedae is the Flamsteed designation. It is visible to the naked eye with an apparent visual magnitude of 4.82. Based upon an annual parallax shift of 5.7 mas, it is located about 570 light years from the Earth. It is moving closer with a heliocentric radial velocity of −8 km/s.
9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.
24 Cancri is a triple star system in the constellation Cancer. The system is located about 226 light-years away, based on its parallax. The system has a combined apparent magnitude of 6.5, and the two components A and B are separated by 5.7″.
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.
IC 2391 is an open cluster in the constellation Vela consisting of hot, young, blueish stars, some of which binaries and one of which is a quadruple. Persian astronomer A. a.-R. al-Sufi first described it as "a nebulous star" in c. 964. It was re-found by Abbe Lacaille and cataloged as Lac II 5.
HD 115404 is a binary star system located in the constellation Coma Berenices. Parallax measurements made by Hipparcos put the system at 36 light-years, or 11 parsecs, away. The combined apparent magnitude of the system is 6.52, with the magnitudes of the components being 6.66 and 9.50.
HD 1185 is a double star in the northern constellation of Andromeda. The primary, with an apparent magnitude of 6.15, is a white main-sequence star of spectral type A2VpSi, indicating it has stronger silicon absorption lines than usual, thus making it also an Ap star. The secondary companion, which is 9.08 arcseconds away, is not visible to the naked eye at an apparent magnitude of 9.76. It shares common proper motion and parallax with the primary star but orbital parameters are still unknown.
HD 88836, also known as HR 4019, is a solitary, yellow-hued star located in the southern constellation Antlia. It has an apparent magnitude of 6.32, placing it near the limit for naked eye visibility. Based on an annual parallax shift of 7.019 mas, the object is estimated to be 465 light years away from the Solar System. Its distance from the Sun does not appear to be changing, having a radial velocity of 0 km/s.
HD 156768 is a double star in the southern constellation of Ara, with a combined apparent magnitude of 5.86. The brighter component is a sixth magnitude bright giant or supergiant star with a stellar classification of G8Ib/II. The magnitude 9.6 companion lies at an angular separation of 1.81″ along a position angle of 184°.
HD 158476 is a supergiant star in the southern constellation of Ara. There is a faint magnitude 10.5 companion at an angular separation of 20.0″ along a position angle of 209°.
HD 93607 is a star in the constellation Carina. Its apparent magnitude is 4.87. Its parent cluster is IC 2602.
HD 165189 and HD 165190 are components of a visual binary star system located 143 light years away in the southern constellation of Corona Australis. It is visible to the naked eye with the primary having an apparent visual magnitude of 4.929±0.025. The system is a member of the Beta Pictoris Moving Group.
HD 59612 is a class A5Ib supergiant star in the constellation Puppis. Its apparent magnitude is 4.86 and it is approximately 4,300 light years away based on parallax.
57 Persei, or m Persei, is a suspected triple star system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08. The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).
31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.
HD 53367 is a triple star system in the constellation of Monoceros. The primary star was identified as a variable Herbig Ae/Be star in 1989. Its companion, spectroscopically discovered in 2006, is a pre-main-sequence star star with an average separation of 1.7 AU. The star system is embedded in the extended nebula IC 2177.
7 Tauri is a multiple star in the northern constellation of Taurus. It has a combined apparent visual magnitude of 5.95, so, according to the Bortle scale, it is faintly visible from suburban skies at night. Measurements made with the Gaia spacecraft show an annual parallax shift of 5.5 mas, which is equivalent to a distance of around 593 light years from the Sun.
HD 195479, also designated as HR 7839, is a solitary star located in the northern constellation Delphinus, the dolphin. It has an apparent magnitude of 6.20, placing it near the limit for naked eye visibility, even under ideal conditions. The object is located relatively close at a distance of 288 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −40.1 km/s. At its current distance, HD 195479's brightness is diminished by an interstellar extinction of 0.27 magnitudes and it has an absolute magnitude of +1.53.