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Iota Apodis
Iota Apodis is a binary star system in the southern circumpolar constellation of Apus. Its identifier is a Bayer designation that is Latinized from ι Apodis, and abbreviated Iot Aps or ι Aps, respectively. This system is a faint target at an apparent visual magnitude of 5.41, but still visible to the naked eye from suitably dark skies. The distance to this star can be gauged from parallax measurements, yielding an estimate of with a 6% margin of error. The system is drifting closer with a heliocentric radial velocity of −4.3 km/s. The dual nature of this system was announced by W. S. Finsen in 1960, who reported an angular separation of . Their orbit has an angular separation of 0.091 arcseconds with an estimated orbital period of 59.32 years and an eccentricity (ovalness) of 0.17. Both stars are B-type main sequence stars, which indicates they shine with a blue-white hue. The brighter component has a stellar classification of B9 V and an appa ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Apus
Apus is a small constellation in the Southern Celestial Hemisphere, southern sky. It represents a bird-of-paradise, and its name means "without feet" in Greek language, Greek because the bird-of-paradise was once wrongly believed to lack feet. First depicted on a celestial globe by Petrus Plancius in 1598, it was charted on a star atlas by Johann Bayer in his 1603 ''Uranometria''. The French explorer and astronomer Nicolas Louis de Lacaille charted and gave the brighter stars their Bayer designations in 1756. The five brightest stars are all reddish in hue. Shading the others at apparent magnitude 3.8 is Alpha Apodis, an orange giant that has around 48 times the diameter and 928 times the luminosity of the Sun. Marginally fainter is Gamma Apodis, another aging giant star. Delta Apodis is a double star, the two components of which are 103 Minute and second of arc, arcseconds apart and visible with the naked eye. Two star systems have been found to have exoplanet, planets. Histo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Chinese Constellations
Traditional Chinese astronomy has a system of dividing the celestial sphere into asterisms or constellations, known as "officials" ( Chinese ''xīng guān''). The Chinese asterisms are generally smaller than the constellations of Hellenistic tradition. The Song dynasty (13th-century) Suzhou planisphere shows a total of 283 asterisms, comprising a total of 1,565 individual stars. The asterisms are divided into four groups, the Twenty-Eight Mansions (, ''Èrshíbā Xiù'') along the ecliptic, and the Three Enclosures of the northern sky. The southern sky was added as a fifth group in the late Ming dynasty based on European star charts, comprising an additional 23 asterisms. The Three Enclosures (, ''Sān Yuán'') include the Purple Forbidden Enclosure, which is centered on the north celestial pole and includes those stars which could be seen year-round,Needham, J.Astronomy in Ancient and Medieval China. ''Philosophical Transactions of the Royal Society of London''. Ser ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Binary Stars
A binary star or binary star system 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 as separate stars using a telescope, in which case they are called ''visual binaries''. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known. They may also be detected by indirect techniques, such as spectroscopy (''spectroscopic binaries'') or astrometry (''astrometric binaries''). If a binary star happens to orbit in a plane along our line of sight, its components will eclipse and transit each other; these pairs are called ''eclipsing binaries'', or, together with other binaries that change brightness as they orbit, ''photometric binaries''. If components in binary star systems are close enough, they can gravitationally distort each other's outer stellar atmospheres. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
B-type Main-sequence Stars
A B-type main-sequence star (B V) is a main-sequence (hydrogen-burning) star of spectral type B and luminosity class V. These stars have from 2 to 16 times the mass of the Sun and surface temperatures between 10,000 and 30,000 K. B-type stars are extremely luminous and blue. Their spectra have strong neutral helium absorption lines, which are most prominent at the B2 subclass, and moderately strong hydrogen lines. Examples include Regulus, Algol A and Acrux. History This class of stars was introduced with the Harvard sequence of stellar spectra and published in the ''Revised Harvard photometry'' catalogue. The definition of type B-type stars was the presence of non-ionized helium lines with the absence of singly ionized helium in the blue-violet portion of the spectrum. All of the spectral classes, including the B type, were subdivided with a numerical suffix that indicated the degree to which they approached the next classification. Thus B2 is 1/5 of the way from type B (or ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Commonwealth Scientific And Industrial Research Organisation
The Commonwealth Scientific and Industrial Research Organisation (CSIRO) is an Australian Government agency that is responsible for scientific research and its commercial and industrial applications. CSIRO works with leading organisations around the world. From its headquarters in Canberra, CSIRO maintains more than 50 sites across Australia as well as in France and the United States, employing over 6,500 people. Federally funded scientific research in Australia began in 1916 with the creation of the Advisory Council of Science and Industry. However, the council struggled due to insufficient funding. In 1926, research efforts were revitalised with the establishment of the Council for Scientific and Industrial Research (CSIR), which strengthened national science leadership and increased research funding. CSIR grew rapidly, achieving significant early successes. In 1949, legislative changes led to the renaming of the organisation as Commonwealth Scientific and Industrial Research ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Monthly Notices Of The Royal Astronomical Society
''Monthly Notices of the Royal Astronomical Society'' (MNRAS) is a peer-reviewed scientific journal in astronomy, astrophysics and related fields. It publishes original research in two formats: papers (of any length) and letters (limited to five pages). MNRAS publishes more articles per year than any other astronomy journal. The learned society journal has been in continuous existence since 1827 and became online only in 2020. It operates as a partnership between the Royal Astronomical Society (RAS), who select and peer-review the contents, and Oxford University Press (OUP), who publish and market the journal. Despite its name, MNRAS is no longer monthly, nor does it carry the notices of the RAS. In 2024 MNRAS became a purely gold open access journal. History The first issue of MNRAS was published on 9 February 1827 as ''Monthly Notices of the Astronomical Society of London'' and it has been in continuous publication ever since. It took its current name from the second vo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Carnegie Institution Of Washington
The Carnegie Institution for Science, also known as Carnegie Science and the Carnegie Institution of Washington, is an organization established to fund and perform scientific research in the United States. This institution is headquartered in Washington, D.C. , the Institution's endowment was valued at $926.9 million. In 2018, the expenses for scientific programs and administration were $96.6 million. American astrophysicist John Mulchaey is the current president of the institution. Name More than 20 independent organizations were established through the philanthropy of Andrew Carnegie and feature his surname. In 2024, the "Carnegie Institution for Science" officially adopted the name "Carnegie Science", a name which has been used informally since 2007 when they first changed the name from "Carnegie Institution of Washington" to "Carnegie Institution for Science". History It is proposed to found in the city of Washington, an institution which ... shall in the broad ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Apodis
Epsilon Apodis is a star in the southern circumpolar constellation of Apus. Its identifier is a Bayer designation that is Latinized from ε Apodis, and abbreviated Eps Aps or ε Aps, respectively. This star has an apparent visual magnitude of 5.06, which is bright enough to be viewed from dark suburban skies. Based upon parallax measurements, it is at a distance of roughly from Earth. The star is drifting further away with a heliocentric radial velocity of +4.5 km/s. Based upon a stellar classification of B3 V, this is a massive, B-type main sequence star that is generating energy through the fusion of hydrogen at its core. Epsilon Apodis has more than six times the mass of the Sun and over four times the Sun's radius. It is radiating 1,614 times as much luminosity as the Sun from its photosphere at an effective temperature of 17,100 K. At this heat, it has a blue-white glow that is a characteristic of B-type stars. Epsilon Apodis is spinning rapidly, w ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpha Apodis
Alpha Apodis, also named Paradys, is the brightest star in the southern circumpolar constellation of Apus (constellation), Apus. It had the Greek alpha designation as part of the constellation which Johann Bayer called Apis Indica in his 1603 ''Uranometria'' star atlas. This identifier is a Bayer designation that is Romanization of Greek, Latinied from α Apodis, and abbreviated Alpha Aps or α Aps, respectively. The star has an apparent visual magnitude of approximately 3.825, which can be viewed with the naked eye. With a declination of –79°, this is a circumpolar star for much of the southern hemisphere. It can be identified on the night sky by drawing an imaginary line through Alpha Centauri and Alpha Circini then extending it toward the south celestial pole. This is a giant star with a stellar classification of K3IIICN0.5, indicating that this star has consumed the hydrogen at its core and has stellar evolution, evolved away from the main seque ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Apodis
Eta Apodis is a star in the southern circumpolar constellation Apus. Its identifier is a Bayer designation that is Latinized from η Apodis, and abbreviated Eta Aps or η Aps, respectively. Based upon parallax measurements from Gaia Data Release 3, it is from Earth. It is drifting closer with a heliocentric radial velocity of −9 km/s. With an apparent visual magnitude of +4.9, it can be viewed with the naked eye from the southern hemisphere. Properties This star has about 1.77 times the mass of the Sun and 2.13 times the Sun's radius. It is radiating 15.5 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 7,860 K. Eta Apodis is a young star with an age of about 250 million years, and is spinning with a projected rotational velocity of 17 km/s. The stellar classification of Eta Apodis shows this to be an Am star, which means the spectrum shows chemically peculiarities. In particular, it is an A2-type star showing a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Apodis
Delta Apodis is a double star in the southern constellation of Apus. Its identifier is a Bayer designation that is Romanization of Greek, Latinized from δ Apodis, and abbreviated Del Aps or δ Aps, respectively. Based on stellar parallax, parallax measurements, the distance to δ Apodis is approximately 620 light years, while δ Apodis is found to be around 563 light years from Earth. They may form a common proper motion pair. The brighter star, δ Apodis, has an apparent magnitude that varies from +4.66 to +4.87. It is a red giant with a stellar classification of M5 IIIb, and is classified as a semiregular variable with pulsations of multiple periods of 68.0, 94.9 and 101.7 days. δ Apodis has an apparent magnitude of +5.27 and is an orange stellar classification, K-type giant star, giant with a class of K3 III. Both stars are bright enough to be seen with the naked eye under good observing conditions. The pair have an angular separation of 103.4 arcs ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Octantis
δ Octantis, Latinised as Delta Octantis, has the distinction of being Saturn's southern pole star A pole star is a visible star that is approximately aligned with the axis of rotation of an astronomical body; that is, a star whose apparent position is close to one of the celestial poles. On Earth, a pole star would lie directly overhead when .... An orange giant of class K2III, it has 1.2 times the mass of the Sun and about 25 times the Sun's radius. This star is about 4.3 billion years old, which is similar to the age of the Sun. Naming In Chinese caused by adaptation of the European southern hemisphere constellations into the Chinese system, (), meaning '' Exotic Bird'', refers to an asterism consisting of δ Octantis, ζ Apodis, ι Apodis, β Apodis, γ Apodis, δ1 Apodis, η Apodis, α Apodis and ε Apodis. Consequently, δ Octantis itself is known as (, ). [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
