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List Of Stars In Antlia ...
This is the list of notable stars in the constellation Antlia, sorted by decreasing brightness. See also * List of stars by constellation References * * * * * * * * {{Portal bar, Astronomy, Stars, Spaceflight, Outer space, Solar System * List Antlia Antlia (; from Ancient Greek ''ἀντλία'') is a constellation in the Southern Celestial Hemisphere. Its name means "pump" in Latin and Greek; it represents an air pump. Originally Antlia Pneumatica, the constellation was established by Nic ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star
A star is an astronomical object comprising a luminous spheroid of plasma held together by its gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night, but their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated to stars. Only about 4,000 of these stars are visible to the naked eye, all within the Milky Way galaxy. A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Its total mass is the main factor determining its evolution and eventual fate. A star shines for most of its active life due t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Antliae
Epsilon Antliae, Latinized from ε Antliae, is the Bayer designation for a single star in the southern constellation of Antlia, being positioned near the western constellation border and forming part of the main asterism. The apparent visual magnitude of this star is +4.51, which means it is visible to the naked eye. From parallax measurements, the distance to this star is known to be . It is drifting further away from the Sun with a radial velocity of +22 km/s. The stellar classification of this star is K3 IIIa, where the luminosity class of III indicates that this is an evolved giant star that has exhausted the supply of hydrogen at its core. It has expanded to around 56 times the radius of the Sun and radiates approximately 919 times the Sun's luminosity from its photosphere at an effective temperature of 4,237 K. Photometry measurements during the Hipparcos mission indicate that this star is undergoing periodic variability by 0.0034 magnitudes ov ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Antliae
Delta Antliae (δ Ant, δ Antliae) is the Bayer designation for a binary star system in the southern constellation of Antlia. The combined apparent visual magnitude of the system is +5.57, allowing it to be viewed from the suburbs with the naked eye. Judging by the parallax shift of this system, it is located at a distance of 450 ± 10 light-years from Earth. The system is reduced in magnitude by 0.03 due to extinction caused by intervening gas and dust. The primary component of the system has a stellar classification of B9.5 V, indicating that it is a B-type main sequence star. The companion is an F-type main sequence star with a classification of F9 Ve, where the 'e' indicates that there are emission lines in the spectrum. The two stars are separated by 11 arcseconds. Delta Antliae A, the brighter member of this system, has an estimated 3.4 times the mass of the Sun. It is radiating around 200 times as much luminosity as the Sun from its outer atmosphere at ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HR 4049
HR 4049, also known as HD 89353 and AG Antliae, is a binary post- asymptotic-giant-branch (post-AGB) star in the constellation Antlia. A very metal-poor star, it is surrounded by a thick unique circumbinary disk enriched in several molecules. With an apparent magnitude of about 5.5, the star can readily be seen under ideal conditions. It is located approximately distant. HR 4049 has a peculiar spectrum. The star appears, based on its spectrum in the Balmer series, to be a blue supergiant, although in reality it is an old low-mass star on the post-AGB phase of its life. Its atmosphere is extremely deficient in heavy elements, over with a metallicity over 30,000 lower than the Sun. It also shows a strong infrared excess, corresponding closely to a blackbody produced by a disk of material surrounding the star. The star is also undergoing intense mass-loss HR 4049 has an unseen companion, detected from variations in the doppler shift of its spectral lines. The prope ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Slow Irregular Variable
A slow irregular variable (ascribed the GCVS types L, LB and LC) is a variable star that exhibit no or very poorly defined periodicity in their slowly changing light emissions. These stars have often been little-studied, and once more is learnt about them, they are reclassified into other categories such as semiregular variables. Nomenclature Irregular variable stars were first given acronyms based on the letter "I": ''Ia'', ''Ib''. and ''Ic''. These were later refined so that the I codes were used "nebular" or "rapidly irregular" variable stars such as T Tauri and Orion variables. The remaining irregular stars, cool slowly varying giants and supergiants of type Ib or Ic were reassigned to Lb and Lc. When the General Catalogue of Variable Stars standardised its acronyms to be all uppercase, the codes LB and LC were used. Type Lb ''Slow irregular variables of late spectral types ( K, M, C, S); as a rule, they are giants'' The GCVS also claims to give this type to slow irregula ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
U Antliae
U Antliae (U Ant) is a variable star in the constellation Antlia. It is a carbon star surrounded by two thin shells of dust. U Antliae is an extremely red C-type carbon star. These cool stars on the asymptotic giant branch are further reddened by strong mass loss and dust that forms around the star. U Antliae is calculated to have an effective surface temperature of , although the light that reaches us has an appearance more like that from a black body with a temperature of surrounded by dust at a temperature of . It emits most of its radiation in the infrared and although it is only about 500 times brighter than the sun at visual wavelengths, its bolometric luminosity is 8,000 times higher than the Sun's. U Antliae is an irregular variable star with an apparent magnitude that varies between 5.27 and 6.04. Approximately 900 light years from Earth, it is surrounded by two shells of dust, thought to have been ejected 14,000 and 10,000 years ago. The exact origin ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 82205
HD 82205 (HR 3770) is a solitary star in the southern constellation Antlia. It is faintly visible to the naked eye with an apparent magnitude of 5.48 and is estimated to be 810 light years distant based on parallax measurements. However, it is receding with a heliocentric radial velocity of . HD 82205 has a general stellar classification of K3 III, indicating that it is a red giant. However, Houk and Cowley (1982) found a slightly warmer class of K2 III CNII, which also suggests a strong overabundance of cyano radicals in the stellar atmosphere. At present it has 4.46 times the mass of the Sun but has expanded to 38.9 times its girth. It shines with a luminosity of from its enlarged photosphere at an effective temperature of , giving an orange hue. HD 82205 has a metallicity 123% that of the Sun and is believed to be a member of the thin disk population. Currently, it spins with a projected rotational velocity lower than . There is a 14th magnitude optical companion sep ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 96146
HD 96146 (HR 4313) is a binary star located in the southern constellation Antlia. The system has a combined apparent magnitude of 5.41, making it visible to the naked eye under ideal conditions. Parallax measurements from the Gaia spacecraft place the pair at a distance of 710 light years with a large margin of error. It is currently receding with a poorly constrained heliocentric radial velocity of . The object's status as a double star was not known until a 1991 Hipparcos survey of double stars. Since the pair's current projected separation is around , it makes it difficult to distinguish both components. Nevertheless, they are located along a position angle of . The secondary has been observed using speckle interferometry to be 1.8 magnitudes fainter than the visible star. The primary has a stellar classification of A0 V, indicating that it is an ordinary A-type main-sequence star. Zorec and Royer (2012) model it as a dwarf star that is 99.5% through its main sequence ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 90132
HD 90132 (HR 4086) is a solitary white hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.33, making it one of the brighter members of this generally faint constellation. The star is relatively close at a distance of 135 light years but is receding with a heliocentric radial velocity of . HD 90132 has a stellar classification of A8 V, indicating that it is an ordinary A-type main-sequence star. At present it has 1.69 times the mass of the Sun and 1.87 times the radius of the Sun. Despite a young age of 70 million years, the star has a lower surface gravity than expected. This is due to the equator being 18% larger than the poles, which is due to a high projected rotational velocity of . Nevertheless, it shines with a luminosity of from its photosphere at an effective temperature of . HD 90132 is slightly metal deficient with a metallicity 74% that of Sun. This star was observed for infrared excess suggesting the presence of a circu ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Double Star
In observational astronomy, a double star or visual double is a pair of stars that appear close to each other as viewed from Earth, especially with the aid of optical telescopes. This occurs because the pair either forms a binary star (i.e. a binary system of stars in mutual orbit, gravitationally bound to each other) or is an ''optical double'', a chance line-of-sight alignment of two stars at different distances from the observer. Binary stars are important to stellar astronomers as knowledge of their motions allows direct calculation of stellar mass and other stellar parameters. The only (possible) case of "binary star" whose two components are separately visible to the naked eye is the case of Mizar and Alcor (though actually a multiple-star system), but it is not known for sure whether Mizar and Alcor are gravitationally bound. Since the beginning of the 1780s, both professional and amateur double star observers have telescopically measured the distances and angles betwe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Antliae
Eta Antliae (η Ant, η Antliae) is the Bayer designation for a double star in the southern constellation of Antlia. The brighter component has an apparent visual magnitude of 5.222, making it visible to the naked eye. Parallax measurements of the system yield a distance estimate of from Earth. The main component has a stellar classification of F1 V, which indicates that it is an F-type main sequence star. This star has 55% more mass than the Sun. It shines with 6.6 times the Sun's luminosity at an effective temperature of 7,132 K. This heat gives it the yellow-white glow of an F-type star. It has a faint companion located 31 arcseconds away with an apparent magnitude of +11.3. Most likely this pair form a binary star A binary star is a system of two stars that are gravitationally bound to and in orbit around each other. Binary stars in the night sky that are seen as a single object to the naked eye are often resolved using a telescope as separate stars, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
