Many different periods have been reported, but they are consistently near 860 days or 4,400 days. Properties (July 2008, outdated).
It is also one of the largest known stars with a radius around 1,000 times that of the sun, and were it placed in the Sun's position it … Based on the spectral type (M2Ia) of the star, the star's colour is red . Its brightness changes are tied to its absolute brightness. Based on the spectral type (M2.5 Iab) of the star, the star's colour is red . Mu Cephei Star. Mu Cephei, a type M2 Ia star (probably, but classed as M1 or other kind of M2, also), is known for its red color, and the spectrum bears that out. V354 Cephei is not part of the constellation outline but is within the borders of the constellation. Mu Cephei (μ Cep, μ Cephei), also known as Herschel's Garnet Star, is a red hypergiant star in the constellation Cepheus.It appears garnet red, which was fired observed by William Herschel (hence the star's name). Its apparent brightness varies erratically between magnitude 3.4 and 5.1. Delta Cephei doubles in brightness on a precise schedule, every 5.36 days. Herchel's Garnet Star is a Binary or Multiple star system. Mu Cephei is classified as a semiregular variable star of type SRc (supergiant star of a late spectral class exhibiting semiregular variations in brightness due to pulsations). It is now considered to be a semiregular variable of type SRc.
Alpha Cephei (α Cephei, abbreviated Alpha Cep, α Cep), officially named Alderamin / æ l ˈ d ɛr ə m ɪ n /, is a second magnitude star in the constellation of Cepheus near the northern pole.The star is relatively close to Earth at 49 light years (ly Mu Cephei is a variable star and the prototype of the obsolete class of the Mu Cephei variables. Its apparent brightness varies erratically between magnitude 3.4 and 5.1. Learn how this star helped establish the … It is now considered to be a semiregular variable of type SRc. Titanium oxide lines dominate. The images were recorded on 2 types of photographic plates, one sensitive to red light and the other to blue, and then digitized. Mu Cephei, the Garnet Star, and IC 1396. Desc: Mu Cephei is visually nearly 100,000 times brighter than the Sun, with an absolute visual magnitude of −7.6. Delta Cephei (δ Cep, δ Cephei) is the Bayer designation for a quadruple star system located approximately 887 light-years away in the northern circumpolar constellation of Cepheus, the King.At this distance, the visual magnitude of the star is diminished by 0.23 as a result of extinction caused by gas and dust along the line of sight.
Mu Cephei is a variable star and the prototype of the obsolete class of the Mu Cephei variables. The Garnet Star (Mu Cephei) is a very luminous red supergiant, one of the largest and brightest stars visible not only to the naked eye but in the entire Galaxy.It lies in the constellation Cepheus and is associated with a large region of nebulosity known as IC 1396 or the Garnet Star Nebula (see below). Based on the star's spectral, the stars temperature is between 2,400.00 and 3,700.00 degrees kelvin. Its apparent brightness varies erratically between magnitude 3.4 and 5.1. V354 Cephei has a radius that is 1,520.00 times bigger than the Suns. Credit: Davide De Martin. This image is a composite from B&W images taken with the Palomar Observatory's 48-inch Samuel Oschin Telescope as a part of the 2nd National Geographic Palomar Observatory Sky Survey. The Parallax of the star is given as 0.92840 which gives a calculated distance to MY Cephei of 3513.18 light years from the Earth or 1077.12 parsecs. It is now considered to be a semiregular variable of type SRc. It is visually close to IC 1396, and is much closer than Betelgeuse, so the Earth, visualizing the size of the Betelgeuse, was able to discover its distance and size. The class is now obsolete. Many different periods have been reported, but they are consistently near to either 860 days or 4,400 days. Many different periods have been reported, but they are consistently near 860 days or 4,400 days. Based on the star's spectral type of M7.5I C , MY Cephei's colour and type is red supergiant star. These stars are very different, and the difference is obvious in their low-resolution spectra. It once served as the prototype for a class of stars known as the Mu Cephei variables. The star can be seen with the naked eye, that is, you don't need a telescope/binoculars to see it. The star can not be seen by the naked eye, you need a telescope to see it. Other articles where VV Cephei is discussed: star: Eclipsing binaries: , VV Cephei), which would engulf Jupiter and all the inner planets of the solar system if placed at the position of the Sun.