description 40 Eridani B Overview
A white dwarf in the triple star system 40 Eridani, historically notable as the first white dwarf whose anomalously high density was recognized and analyzed.
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40 Eridani B ranks #41 of 217 in the Star ranking, behind Hadar, ahead of Mintaka.
Historically crucial white dwarf with early density recognition, strong compact-star reputation.
help 40 Eridani B FAQ
Where is 40 Eridani B within the 40 Eridani system?
40 Eridani B is the white-dwarf member of a nearby triple system containing 40 Eridani A, B, and C. It is paired with the red dwarf 40 Eridani C, while the orange main-sequence star 40 Eridani A lies much farther from that pair.
Why was 40 Eridani B important to the discovery of white dwarfs?
Astronomers recognized that 40 Eridani B was remarkably faint despite having a spectrum associated with a hot star. Its small size and unusually high density helped establish white dwarfs as a distinct class of stellar remnant.
Can 40 Eridani B be seen without a telescope?
The white dwarf itself is too faint for unaided viewing, although the primary star 40 Eridani A is visible under dark skies. A telescope is needed to separate the system's components, which are located about 16 light-years from Earth.
Is 40 Eridani B still producing energy through fusion?
No, it is the exposed remnant of a star that has exhausted its normal nuclear fuel and shed its outer layers. It now shines mainly because its extremely dense core remains hot and is slowly cooling.
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