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Pavo (Chinese Astronomy)
The modern constellation Pavo is not included in the Three Enclosures and Twenty-Eight Mansions system of traditional Chinese uranography because its stars are too far south for observers in China to know about them prior to the introduction of Western star charts. Based on the work of Xu Guangqi and the German Jesuit missionary Johann Adam Schall von Bell in the late Ming Dynasty, this constellation has been classified as one of the 23 Southern Asterisms (近南極星區, ''Jìnnánjíxīngōu'') under the name Peacock (孔雀, ''Kǒngqiāo''). Possibly Peacock (Alpha Pavonis) is the bright star in this constellation that never seen in Chinese sky. The name of the western constellation in modern Chinese is 孔雀座 (''kǒng què zuò''), which means "the peacock constellation". Stars The map of Chinese constellation in constellation Pavo area consists of : See also * Chinese astronomy * Traditional Chinese star names *Chinese constellations Traditional Chinese astr ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Pavo (constellation)
Pavo is a constellation in the Southern Celestial Hemisphere, southern sky whose name is Latin for "peafowl, peacock". Pavo first appeared on a 35-cm (14 in) diameter celestial globe published in 1598 in Amsterdam by Plancius and Jodocus Hondius and was depicted in Johann Bayer's star atlas ''Uranometria'' of 1603, and was likely conceived by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman. French explorer and astronomer Nicolas-Louis de Lacaille gave its stars Bayer designations in 1756. The constellations Pavo, Grus (constellation), Grus, Phoenix (constellation), Phoenix and Tucana are collectively known as the "Southern Birds". The constellation's brightest member, Alpha Pavonis, is also known as Peacock and appears as a 1.91-Apparent magnitude, magnitude blue-white star, but is actually a spectroscopic binary. Delta Pavonis is a nearby Sun-like star some 19.9 light-years distant. Six of the star systems in Pavo have been found ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kappa Pavonis
Kappa Pavonis (κ Pav) is a variable star in the constellation Pavo. It is the brightest W Virginis variable in the sky. Discovery In 1901, κ Pavonis was reported to be a variable star with a magnitude range of 3.8 to 5.2 with a period of 9.0908 days. Further observations revealed radial velocity variations in time with the brightness variations, but this was assumed to indicate a spectroscopic binary system. The brightness variations were then interpreted as eclipses. Less than 10 years later, was κ Pav was listed as a likely Cepheid variable. In 1937 it was used as part of the effort to calibrate the Cepheid distance scale. Only years later were the separate period luminosity relationships for population I and II Cepheid variables identified, and κ Pav was assigned to the type II group. Variability κ Pavonis ranges between apparent magnitudes 3.91 and 4.78, and spectral types F5 to G5, over a period of 9.1 days. It is a W Virginis variable, a type II ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Brightest Stars
This is a list of stars arranged by their apparent magnitude – their brightness as observed from Earth. It includes all stars brighter than magnitude +2.50 in visible light, measured using a ''V''-band filter in the UBV photometric system. Stars in binary systems (or other multiples) are listed by their ''total'' or ''combined'' brightness if they appear as a single star to the naked eye, or listed separately if they do not. As with all magnitude systems in astronomy, the scale is logarithmic and inverted i.e. lower/more negative numbers are brighter. Most stars on this list appear bright from Earth because they are nearby, not because they are intrinsically luminous. For a list which compensates for the distances, converting the ''apparent'' magnitude to the ''absolute'' magnitude, see the list of most luminous stars. Measurement The Sun is the brightest star as viewed from Earth, at −26.74 mag. The second brightest is Sirius at −1.46 mag. For c ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Chinese Astronomy
Astronomy in China has a long history stretching from the Shang dynasty, being refined over a period of more than 3,000 years. The ancient Chinese people have identified stars from 1300 BCE, as Chinese star names later categorized in the twenty-eight mansions have been found on oracle bones unearthed at Anyang, dating back to the mid-Shang dynasty. The core of the "mansion" (宿 ''xiù'') system also took shape around this period, by the time of King Wu Ding (1250–1192 BCE). Detailed records of astronomical observations began during the Warring States period (fourth century BCE) and flourished from the Han period onward. Chinese astronomy was equatorial, centered on close observation of circumpolar stars, and was based on different principles from those in traditional Western astronomy, where heliacal risings and settings of zodiac constellations formed the basic ecliptic framework. Joseph Needham has described the ancient Chinese as the most persistent and accurate obser ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Omega Pavonis
This is the list of notable stars in the constellation Pavo, sorted by decreasing brightness. See also *List of stars by constellation All stars but one can be associated with an IAU constellation. IAU constellations are areas of the sky. Although there are only 88 IAU constellations, the sky is actually divided into 89 irregularly shaped boxes as the constellation Serpens is spli ... References * * * * * {{Stars of Pavo *List Pavo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Xi Pavonis
ξ Pavonis, Latinised as Xi Pavonis, is a triple star system in the southern constellation of Pavo. It is visible to the naked eye as a faint star with a combined apparent visual magnitude of 4.35 The system is located approximately 440 light-years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. This system forms the double star GLE 2, whose companion's magnitude is 8.6 with a angular separation, which was discovered by Australian amateur astronomer Walter Gale in 1894. The primary component is itself a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.26. The visible member of this inner pair is an aging giant star with a stellar classification In astronomy, stellar classification is the classification of stars based on their stellar spectrum, spectral characteristics. Electromagnetic radiation from the star is analyzed by splitting it with a Prism (optic ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 172555
HD 172555 is a white-hot A7V star located relatively close by, 95 light years from Earth in the direction of the constellation Pavo. Spectrographic evidence indicates a relatively recent collision between two planet-sized bodies that destroyed the smaller of the two, which had been at least the size of Earth's moon, and severely damaged the larger one, which was at least the size of Mercury. Evidence of the collision was detected by NASA's Spitzer Space Telescope. Giant hypervelocity impact debris HD172555 was first recognized in the 1980s as being unusually bright in the mid-infrared by the IRAS sky survey. Follow-up, ground-based observations by Schütz et al. and the Spitzer Space Telescope, also in 2004, confirmed the unusually strong nature of the infrared spectral emission from this system, much brighter than what would be emitted normally from the star's surface. As part of the Beta Pictoris moving group, HD172555 is coeval with that more famous system ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gamma Pavonis
Gamma Pavonis, Romanization of Greek, Latinized from γ Pavonis, is a star in the southern circumpolar constellation of Pavo (constellation), Pavo. With an apparent visual magnitude of 4.22, it is a fourth-magnitude star and thereby Bortle Dark-Sky Scale, visible to the naked eye. From parallax observations with the Hipparcos satellite, the distance to this star has been estimated at . It is drifting closer to the Sun with a radial velocity of −30 km/s. Compared to the Sun, this star has a 21% greater mass and a 15% larger radius. It is a brighter star with 152% of the Sun's luminosity, which is it radiating from the outer envelope at an effective temperature of 6,112 K. The stellar classification of F9 V puts it in the class of F-type main sequence stars that generate energy through the nuclear fusion of hydrogen at the core. It is a metal-poor star, which means it has a low abundance of Chemical element, elements heavier than helium. Age estimates range ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Pavonis
Epsilon Pavonis, Latinisation of names, Latinized from ε Pavonis, is a single, white-hued star in the constellation Pavo (constellation), Pavo. It can be viewed with the naked eye, having an apparent visual magnitude of 3.97. The annual stellar parallax, parallax shift of 31.04 milliarcsecond, mas provides a distance estimate of 105 light years from the Sun. This star is a member of the proposed Argus Association, a young moving group of more than 60 stars associated with the IC 2391 cluster. Epsilon Pavonis is moving closer to the Sun with a radial velocity of −6.7 km/s. With a stellar classification of A0 Va, Epsilon Pavonis is an ordinary A-type main-sequence star that is generating energy through hydrogen fusion at its stellar core, core. It is just 27 million years old with a projected rotational velocity of 85 km/s. The star has 2.2 times the mass of the Sun and 1.74 the Sun's radius. It is radiating 32 times the Sun's luminosity from its ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Pavonis
Zeta Pavonis, Latinisation of names, Latinized from ζ Pavonis, is an orange-hued star in the southern constellation Pavo (constellation), Pavo. Its apparent magnitude is 4.01, which is bright enough to be faintly visible to the naked eye. The annual stellar parallax, parallax shift of this star is 14.93 milliarcsecond, mas as seen from Earth, which provides a distance estimate of approximately away from the Sun. It is moving closer to the Sun with a radial velocity of −16.30. Based upon its motion through space, this star appears to be a member of the Hyades Supercluster. This is an stellar evolution, evolved K-type star, K-type giant star with a stellar classification of K0 III, which indicates it has exhausted the supply of hydrogen at its stellar core, core. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of this star, this yields a physical size of about 19 times the Solar radius, radius of t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Beta Pavonis
Beta Pavonis, Latinised from β Pavonis, is a single, white-hued star in the southern constellation of Pavo. It can be seen with the naked eye, having an apparent visual magnitude of 3.42. Based upon an annual parallax shift of 24.14 mas as seen from Earth, it is located 135 light-years from the Sun. It is moving away from the Sun with a radial velocity of +4 km/s. Beta Pavonis is a member of the Ursa Major Moving Group, a set of stars that share a similar motion through space. Zorec and Royer (2012) list a stellar classification for this star of A5 IV, indicating it is an evolving subgiant star that has consumed the hydrogen at its core and has begun to expand onto the red giant branch. However, Houk (1979) listed a more evolved class of A7 III, suggesting it is already a giant star. It has about 2.3 times the Sun's radius and 2.51 times the mass of the Sun. At the estimated age of 305 million years, the star still has a relatively high rat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Pavonis
Delta Pavonis, Latinized from δ Pavonis, is a single star in the southern constellation of Pavo. It has an apparent visual magnitude of 3.56, making it a fourth-magnitude star that is visible to the naked eye from the southern hemisphere. Parallax measurements yield an estimated distance of from Earth. This makes it one of the nearest bright stars to the Solar System. It is approaching the Sun with a radial velocity of −23.5 km/s, and is predicted to come as close as in around 49,200 years. Observations This object is a subgiant of spectral type G8 IV; it will stop fusing hydrogen at its core relatively soon, starting the process of becoming a red giant. Hence, Delta Pavonis is 24% brighter than the Sun, but the effective temperature of its outer atmosphere is less: 5,571 K. Its mass is 105% of Sol's mass, with a mean radius 120% of Sol's radius. Delta Pavonis's surface convection zone extends downward to about 43.1% of the star's radius, bu ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
