The hot star group at the LSW mainly studies the mass-loss and variability of hot, massive stars, in the last years mainly with the fiber-linked echelle spectrographs. Infra-red and spectroscopic observations of hot stars in clusters, groups and the field are interpreted. Their circumstellar dust shells are found to have a greater. Wir gehen auf eine Zeitreise, in der wir euch die schönsten Stars der letzten Jahre vorstellen – von bis Fangen wir im Jahr an.
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Namespaces Article Talk. Views Read Edit View history. They are the building blocks of galaxies, of which there are billions in the universe. The life cycle of a star spans billions of years.
As a general rule, the more massive the star, the shorter its life span. Birth takes place inside hydrogen-based dust clouds called nebulae.
Over the course of thousands of years, gravity causes pockets of dense matter inside the nebula to collapse under their own weight.
Because the dust in the nebulae obscures them, protostars can be difficult for astronomers to detect. As a protostar gets smaller, it spins faster because of the conservation of angular momentum—the same principle that causes a spinning ice skater to accelerate when she pulls in her arms.
Increasing pressure creates rising temperatures, and during this time, a star enters what is known as the relatively brief T Tauri phase.
Most of the stars in our galaxy, including the sun, are categorized as main sequence stars. They exist in a stable state of nuclear fusion, converting hydrogen to helium and radiating x-rays.
But figuring out what that heat source could be is proving tricky. We know now, thanks to new research, one thing that it isn't: the sedimentation, or inward sinking, of a neutron-rich stable isotope of neon deep in the stars' interiors.
Most stars in the Milky Way galaxy - those below about eight times the mass of the Sun - are destined to become white dwarf stars. Stars of this mass, having run out of hydrogen and helium to fuse, have insufficient pressure to ignite the carbon that remains.
They eject their outer material, and the core contracts into a sphere about the size of the Earth. This Earth-sized sphere, consisting mainly of carbon and oxygen, is incredibly dense, the most massive up to around 1.
Only something called electron degeneracy pressure, an outward pressure generated by the inability of electrons with the same spin to occupy the same state, prevents the core from complete collapse.