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χ Piscium
Chi Piscium (χ Piscium) is a solitary, orange-hued star in the zodiac constellation of Pisces. It can be seen with the naked eye, having an apparent visual magnitude of +4.64. Based upon an annual parallax shift of 8.50 mas as seen from Earth, it is located about 384 light years from the Sun. This is an evolved G-type giant star with a stellar classification of G8.5 III. There is a 94% chance that it is on the horizontal branch and is a red clump star, which means it is generating energy through helium fusion at its core. Chi Piscium is estimated to have 3.17 times the mass of the Sun, nearly 21 times the solar radius, and shines with 209 times the Sun's luminosity. It is around 380 million years old. Naming In Chinese, (), meaning ''Legs (asterism)'', refers to an asterism consisting of χ Piscium, η Andromedae, 65 Piscium, ζ Andromedae, ε Andromedae, δ Andromedae, π Andromedae, ν Andromedae, μ Andromedae, β Andromedae, σ Piscium, τ ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
J2000
In astronomy, an epoch or reference epoch is a moment in time used as a reference point for some time-varying astronomical quantity. It is useful for the celestial coordinates or orbital elements of a celestial body, as they are subject to perturbations and vary with time. These time-varying astronomical quantities might include, for example, the mean longitude or mean anomaly of a body, the node of its orbit relative to a reference plane, the direction of the apogee or aphelion of its orbit, or the size of the major axis of its orbit. The main use of astronomical quantities specified in this way is to calculate other relevant parameters of motion, in order to predict future positions and velocities. The applied tools of the disciplines of celestial mechanics or its subfield orbital mechanics (for predicting orbital paths and positions for bodies in motion under the gravitational effects of other bodies) can be used to generate an ephemeris, a table of values giving ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Solar Mass
The solar mass () is a frequently used unit of mass in astronomy, equal to approximately . It is approximately equal to the mass of the Sun. It is often used to indicate the masses of other stars, as well as stellar clusters, nebulae, galaxies and black holes. More precisely, the mass of the Sun is The solar mass is about times the mass of Earth (), or times the mass of Jupiter (). History of measurement The value of the gravitational constant was first derived from measurements that were made by Henry Cavendish in 1798 with a torsion balance. The value he obtained differs by only 1% from the modern value, but was not as precise. The diurnal parallax of the Sun was accurately measured during the transits of Venus in 1761 and 1769, yielding a value of (9 arcseconds, compared to the present value of ). From the value of the diurnal parallax, one can determine the distance to the Sun from the geometry of Earth. The first known estimate of the solar mass was by ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Sigma Piscium
Sigma Piscium (Sigma Psc, σ Piscium, σ Psc) is a binary star in the zodiac constellation of Pisces. It has an apparent magnitude of +5.50, meaning it is barely visible to the naked eye, according to the Bortle scale. While parallax measurements by the Hipparcos spacecraft give a distance of approximately 430 light years (133 parsecs), dynamical parallax measurements put it slightly closer, at 368 light-years (113 parsecs) from Earth. Sigma Piscium is a spectroscopic binary system, meaning the components of the system have been detected from periodic Doppler shifts in their spectra. In this case, light from both stars can be detected and it is double-lined. It has an orbital period of 81 days, and the orbit is relatively eccentric, at about 0.9. Both components are B-type main-sequence stars. Sigma Piscium is moving through the Milky Way at a speed of 23.5 km/s relative to the Sun. Its projected galactic orbit carries it between 24,300 and 29,40 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Beta Andromedae
Mirach is a prominent star in the northern constellation of Andromeda. It is pronounced and has the Bayer designation Beta Andromedae, which is Latinized from β Andromedae. This star is positioned northeast of the ''Great Square'' of Pegasus and is potentially visible to all observers north of latitude 54° S. It is commonly used by stargazers to find the Andromeda Galaxy. The galaxy NGC 404, also known as Mirach's Ghost, is seven arcminutes away from Mirach. This star has an apparent visual magnitude of around 2.07, varying between 2.01 and 2.10, which at times makes it the brightest star in the constellation. Based upon parallax measurements, it is roughly from the Solar System. Its apparent magnitude is reduced by 0.06 by extinction due to gas and dust along the line of sight. The star has a negligible radial velocity of 0.1 km/s, but with a relatively large proper motion, traversing the celestial sphere at an angular rate of ·yr−1. Properties Mirach ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mu Andromedae
Mu Andromedae is a binary star system in the northern constellation of Andromeda. Its Bayer designation is Latinized from μ Andromedae, and abbreviated Mu And or μ And, respectively. The system has an apparent visual magnitude of 3.87, making it readily visible to the naked eye. Based upon parallax measurements, it is located at a distance of approximately from Earth. In the constellation, the star is situated about halfway between the bright star Mirach to the southwest and the Andromeda Galaxy (M31) to the northeast. The spectrum of this star matches a stellar classification of A5 V, indicating that it is an A-type main sequence star. It has 2.2 times the mass of the Sun and three times the Sun's radius. The star is radiating about 40 times the luminosity of the Sun from its outer envelope at an effective temperature of 8,320 K, giving it the characteristic white glow of an A-type star. It is estimated to be about 724 million years o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Nu Andromedae
Nu Andromedae is a binary star system in the constellation Andromeda. Its Bayer designation is Latinized from ν Andromedae, and abbreviated Nu And or ν And, respectively. The system has an apparent visual magnitude of 4.5, which is bright enough to be seen with the naked eye. Based on parallax measurements, it is located at a distance of approximately from Earth. The pair are drifting closer with a heliocentric radial velocity of –24 km/s. Situated just over a degree to the west of this star is the Andromeda Galaxy. Nu Andromedae is close spectroscopic binary 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 us ... system with a period of 4.2828 days and a nearly circular orbit. The primary component is a B-type main sequence star with a stellar class ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Pi Andromedae
Pi Andromedae is a binary star 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 us ... system in the northern constellation of Andromeda (constellation), Andromeda. Its Bayer designation is Romanization of Greek, latinized from π Andromedae, and abbreviated Pi And or π And, respectively. With an apparent visual magnitude of 4.4, it is Bortle Dark-Sky Scale, visible to the naked eye. Based on stellar parallax, parallax measurements, it is located at a distance of approximately from Earth. The pair is classified as a blue-white stellar classification, B-type main sequence, main sequence dwarf, with an apparent magnitude of +4.34. It is a spectroscopic binary with an orbital period of 143.5 days and an orbital eccentricity, eccentricity of 0.54. The spectroscopi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Andromedae
Delta Andromedae is a triple star system in the northern constellation of Andromeda. Its identifier is a Bayer designation that is Romanization of Greek, Latinized from δ Andromedae, and abbreviated Delta And or δ And, respectively. The system is visible to the naked eye as a point of light with a combined apparent visual magnitude of 3.28. Based upon stellar parallax, parallax measurements, it is located at a distance of approximately from the Sun. The system is drifting closer with a radial velocity of −10 km/s. In Chinese astronomy, Chinese, (), meaning ''Legs (Chinese constellation), Legs (asterism)'', refers to an asterism consisting of δ Andromedae, Eta Andromedae, η Andromedae, 65 Piscium, Zeta Andromedae, ζ Andromedae, Iota Piscium, ι Piscium, Epsilon Andromedae, ε Andromedae, Pi Andromedae, π Andromedae, Nu Andromedae, ν Andromedae, Mu Andromedae, μ Andromedae, Beta Andromedae, β Andromedae, Sigma Piscium, σ Piscium, Tau Piscium ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Andromedae
Epsilon Andromedae is a star in the constellation of Andromeda. Its identifier is a Bayer designation that is Latinized from ε Andromedae, and abbreviated eps And or ε And, respectively. This star can be seen with the naked eye, having an apparent visual magnitude of 4.4. Based upon an annual parallax shift of 19.2 mas as seen from Earth, it is located approximately 169 light years from the Sun. The system is moving closer to the Sun with a radial velocity of −84 km/s. Its orbit in the Milky Way is highly eccentric, causing it to move rapidly relative to the Sun and its neighboring stars. This is an evolved G-type giant star with a stellar classification of . The suffix notation indicates there is a strong underabundance of iron in the spectrum, and an overabundance of cyanogen (CN). ε Andromedae is believed to be a red clump star which is fusing helium in its core. It has about the same mass as the Sun, but has expanded ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Andromedae
Zeta Andromedae, also named Shimu, is a binary star system in the northern constellation Andromeda (constellation), Andromeda. It is visible to the naked eye with an apparent visual magnitude that varies from over the course of its 17.7 day orbit. Based on stellar parallax, parallax measurements, it is located at a distance of approximately 181 light-years from the Sun. The system is drifting closer with a heliocentric radial velocity of −24.4 km/s. Naming The star's location is in the northern constellation Andromeda, in which it is the second-most southerly of the stars in this often drawn characteristic shape representing the mythical princess asterism (astronomy), asterism, after η Andromedae. Zeta Andromedae (Zeta And, ζ Andromedae, ζ And) is the star's Bayer designation. It also has the Flamsteed designation 34 Andromedae and multiple other designations in stellar catalogues. In Chinese astronomy, Chinese, (), meaning ''L ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
65 Piscium
This is the list of notable stars in the constellation A constellation is an area on the celestial sphere in which a group of visible stars forms Asterism (astronomy), a perceived pattern or outline, typically representing an animal, mythological subject, or inanimate object. The first constellati ... Pisces, sorted by decreasing brightness. See also * List of stars by constellation References * * * * * {{Stars of Pisces *List Pisces ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Andromedae
Eta Andromedae, also named Kui, is a spectroscopic binary star system in the northern constellation of Andromeda. It consists of two G-type evolved stars orbiting each other with a period of 115.7 days and has an overall apparent visual magnitude of approximately 4.403. Based on parallax measurements, this system is located at a distance of approximately 260 light years from the Sun. But it is drawing closer with a heliocentric radial velocity of −10.30 km/s. This star was discovered to be a double-lined spectroscopic binary in a series of spectra taken in 1899 and 1900. Its orbit was computed in 1946 from spectroscopic observations. Because spectroscopy only reveals the radial velocity of a star towards or away from the viewer, such a computation does not determine all orbital elements. In observations made from 1990 to 1992, Eta Andromedae was resolved interferometrically by the Mark III Stellar Interferometer at Mount Wilson Observatory, Califor ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
