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Sirius B, which is a white dwarf, can be seen as a faint point of light to the lower left of the much brighter Sirius A. A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: in an Earth sized volume, it packs a mass that is comparable to the Sun.
Alvan Graham Clark was born in Fall River, Massachusetts, the son of Alvan Clark, founder of Alvan Clark & Sons. [1]On January 31, 1862, while testing a new 18.5-inch (470 mm) aperture great refractor telescope in Cambridgeport, Massachusetts, Clark made the first ever observation of a white dwarf star.
Sirius B: 1852 Sirius system Sirius B is also the nearest white dwarf (as of 2005) [2] [3] First found in a binary star system First double white dwarf system LDS 275: 1944 L 462-56 system [4] First solitary white dwarf Van Maanen 2: 1917 Van Maanen's star is also the nearest solitary white dwarf [5] First white dwarf with a planet WD B1620− ...
About 6% of white dwarfs show infrared excess due to a disk around a white dwarf. [66] In the past only a relative small sample of white dwarf disks was known. [ 67 ] Due to advances in white dwarf detection (e.g. with Gaia or LAMOST ) and improvement of WISE infrared catalogs with unWISE/CatWISE, the number has increased to hundreds of candidates.
Download as PDF; Printable version; ... White dwarf star stubs (24 P) Pages in category "White dwarfs" ... Sirius; Stein 2051; SU Ursae Majoris;
Sirius is a binary star consisting of a main-sequence star of spectral type A0 or A1, termed Sirius A, and a faint white dwarf companion of spectral type DA2, termed Sirius B. The distance between the two varies between 8.2 and 31.5 astronomical units as they orbit every 50 years.
At a distance of 14.1 light-years it is the third closest of its type of star after Sirius B and Procyon B, in that order. [9] [10] Discovered in 1917 by Dutch–American astronomer Adriaan van Maanen, [11] Van Maanen 2 was the third white dwarf identified, after 40 Eridani B and Sirius B, and the first solitary example. [12]
Iota Canis Majoris, lying between Sirius and Gamma, is another star that has been classified as a Beta Cephei variable, varying from magnitude 4.36 to 4.40 over a period of 1.92 hours. [36] It is a remote blue-white supergiant star of spectral type B3Ib, around 46,000 times as luminous as the sun and, at 2500 light-years distant, 300 times ...