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This system consists of a spectral class B3 star being orbited by a less massive class A4 star.
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The mandible under reflected light from above (Fig. 2a, b) or at other angles of incidence (Fig. 2c, d) would suggest a surface bounded by a proximal border, indicating a less massive structure.
When a massive galaxy encounters a less massive galaxy, the effects of the merger are smaller and the massive galaxy can maintain its shape.
Explosions of smaller stars often leave a less massive compact remnant called a neutron star.
A car with a lighter body can use a lighter engine, a less massive suspension, and a less elaborate structure.
Several globular clusters (like M15) have extremely massive cores which may harbor black holes, although simulations suggest that a less massive black hole or central concentration of neutron stars or massive white dwarfs explain observations equally well.
The most likely scenario therefore appears to be the formation of a massive central star or a binary system, surrounded by a number of significantly less massive stars.
Even though a deuteron is less massive by about 2.2 MeV (mega-electron volts) than an individual, free proton or neutron, the photons are energetic enough to more than make up for that mass difference.
A brown dwarf is less massive than a star, so there is less gravity available to pull it together.
Smaller and less massive by far than Triton, and less than half the diameter of Mercury, the Plutonian system is the first one in the Kuiper belt to be imaged from up close.
But when neutrons and protons are bound together into helium, the entire combination of four nucleons winds up being significantly less massive — by about 0.7% — than the individual, unbound constituents.
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