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Parts-per-million chart of the relative mass distribution of the Solar System, each cubelet denoting 2 × 10 24 kg. This article includes a list of the most massive known objects of the Solar System and partial lists of smaller objects by observed mean radius.
An analysis of the lightcurve of the microlensing event PA-99-N2 suggests the presence of a planet orbiting a star in the Andromeda Galaxy. [ 97 ] A controversial microlensing event of lobe A of the double gravitationally lensed Q0957+561 suggests that there is a planet in the lensing galaxy lying at redshift 0.355 (3.7 Gly).
This is a list of the most massive stars that have been ... [40] [21] R99: N44: 103 164,000 Ofpe/WN9 ... Intermediate-mass black holes range from 100 to 10 000 M ...
Closest star to the Sun with exactly six [29] exoplanets, and closest K-type main sequence star to the Sun with a multiplanetary system. One of the oldest stars with a multiplanetary system, although it is still more metal-rich than the Sun. None of the known planets is in the habitable zone. [30] 61 Virginis: Virgo: 13 h 18 m 24.31 s: −18 ...
From top to bottom are an F-type main-sequence star, a yellow dwarf (G-type main-sequence star), an orange dwarf (K-type main-sequence star), a typical red dwarf, and an ultra-cool dwarf. Besides solar energy, the primary characteristic of the Solar System enabling the presence of life is the heliosphere and planetary magnetic fields (for those ...
Main-sequence stars vary in surface temperature from approximately 2,000 to 50,000 K, whereas more-evolved stars – in particular, newly-formed white dwarfs – can have surface temperatures above 100,000 K. [3] Physically, the classes indicate the temperature of the star's atmosphere and are normally listed from hottest to coldest.
e.g. for temperature 2.7 K it is 40 fJ/m 3 ... 4.5×10 −31 kg/m 3 and for visible temperature 6000 K we get 1 J/m 3 ... 1.1×10 −17 kg/m 3. But the total radiation emitted by a star (or other cosmic object) is at most equal to the total nuclear binding energy of isotopes in the star.
It would arise when a star "in the transitional range (~8 to 10 solar masses) between white dwarf formation and iron core-collapse supernovae", and with a degenerate O+Ne+Mg core, [139] imploded after its core ran out of nuclear fuel, causing gravity to compress the electrons in the star's core into their atomic nuclei, [140] [141] leading to a ...