Pisces (Constellation): 101 Piscium, 107 Piscium, 109 Piscium, 109 Piscium B, 19 Piscium, 2mass 0036+1821, 35 Piscium, 3c 47, 3c 9, 3 Arietis,

Please note that the content of this book primarily consists of articles available from Wikipedia or other free sources online. Pages: 59. Chapters: 101 Piscium, 107 Piscium, 109 Piscium, 109 Piscium b, 19 Piscium, 2MASS 0036+1821, 35 Piscium, 3C 47, 3C 9, 3 Arietis, 54 Piscium, 54 Piscium b, Alpha Piscium, Andromeda XXII, Beta Piscium, CFHQS J2329-0301, Chi Piscium, CL0024+17, Delta Piscium, Epsilon Piscium, G29-38, Gamma Piscium, GRB 050904, HD 217107, HD 217107 b, HD 217107 c, HD 219447, HD 219548, HD 222210, HD 222278, HD 222410, HD 222463, HD 222502, HD 222520, HD 222559, HD 4203, HD 4203 b, HD 4313 b, HD 4628, HD 6, HD 8574, HD 8574 b, Iota Piscium, Kappa Piscium, Lambda Piscium, List of stars in Pisces, List of star names in Pisces, M74 Group, Messier 74, Mu Piscium, NGC 12, NGC 296, NGC 3, NGC 33, NGC 36, NGC 38, NGC 383, NGC 4, NGC 45, NGC 474, NGC 514, NGC 520, NGC 57, NGC 60, NGC 7499, NGC 7537, NGC 7714, NGC 7840, NGC 99, Nu Piscium, Omega Piscium, Omicron Piscium, Phi Piscium, Pisces Dwarf, Pisces II (dwarf galaxy), Pisces I (dwarf galaxy), Pi Piscium, Psi1 Piscium, Psi2 Piscium, Psi3 Piscium, Psi Piscium, Rho Piscium, Sigma Piscium, SIMP J013656.5+093347, SN 2003gd, Tau Piscium, Theta Piscium, Upsilon Piscium, USNOA2 0975-00026946, Van Maanen's star, WISEPC J004928.48+044100.1, WISE 0106+1518, WISE J004024.88+090054.8, WISE J013525.64+171503.4, WISE J230133.32+021635.1, Xi Piscium, Zeta Piscium. Excerpt: This is the list of notable stars in the constellation Pisces, sorted by decreasing brightness. Van Maanen's star (van Maanen 2) is a white dwarf. Out of the white dwarfs known, it is the third closest to the Sun, after Sirius B and Procyon B, in that order, and the closest known solitary white dwarf. Discovered in 1917 by Adriaan van Maanen, Van Maanen's star was the third white dwarf identified, after 40 Eridani B and Sirius B, and the first that was not a member of a multi-star system. While searching for a companion to the large-proper-motion star Lalande 1299, in 1917 Dutch American astronomer Adriaan van Maanen discovered a star with an even larger proper motion located a few arcminutes to the northeast. He estimated the annual proper motion of the latter as 3 arcseconds. This star had been previously recorded on a plate taken November 11, 1896 for the Carte du Ciel Catalog of Toulouse, and it showed an apparent magnitude of 12.3. The initial spectral classification was type F0. In 1918, American astronomer Frederick Seares obtained a refined visual magnitude of 12.34, but the distance to the star remained unknown. Two years later, van Maanen published a parallax estimate of 0.246, giving it an absolute magnitude of +14.8. This made it the faintest F-type star known at that time. In 1923, Dutch-American astronomer Willem Luyten published a study of stars with large proper motions in which he identified what he called "van Maanen's star" as one of only three known white dwarfs, a term he coined. These are stars that have an unusually low absolute magnitude for their spectral class, lying well below the main sequence on the Hertzsprung Russell diagram of stellar temperature vs. luminosity. The high mass density of white dwarfs was demonstrated in 1925 by American astronomer Walter Adams when he measured the gravitational redshift of Sirius B as 21 km/s. In 1926, British astrophysicist Ralph Fowler used the new theory of quantum mechanics to show that these sta