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Nuclear physics experiments address stability (i.e., lifetimes and masses) for atomic nuclei well beyond the regime of stable nuclides into the realm of radioactive/unstable nuclei, almost to the limits of bound nuclei (the drip lines), and under high density (up to neutron star matter) and high temperature (plasma temperatures up to 10 9 K ...
Old high-precision frequency standards, i.e. hyperfine structure transition-based atomic clocks, may require periodic fine-tuning due to exposure to magnetic fields. This is carried out by measuring the Zeeman effect on specific hyperfine structure transition levels of the source element (cesium) and applying a uniformly precise, low-strength ...
Atomic astrophysics is concerned with performing atomic physics calculations that will be useful to astronomers and using atomic data to interpret astronomical observations. Atomic physics plays a key role in astrophysics as astronomers' only information about a particular object comes through the light that it emits, and this light arises ...
In atomic physics, spin–orbit coupling, also known as spin-pairing, describes a weak magnetic interaction, or coupling, of the particle spin and the orbital motion of this particle, e.g. the electron spin and its motion around an atomic nucleus. One of its effects is to separate the energy of internal states of the atom, e.g. spin-aligned and ...
Jahn–Teller effect (condensed matter physics) (inorganic chemistry) (organometallic chemistry) (quantum chemistry) January effect (behavioral finance) (economics and finance) (market trends) (stock market) Janus effect (effects) (sociology) Johnsen–Rahbek effect (classical mechanics) (electrical engineering) Joule–Thomson effect ...
How major US stock indexes fared Thursday, 12/26/2024. Food. Food. Allrecipes. The 1 ingredient that makes roast chicken taste better every time. Food. Allrecipes. The top 10 food trends of 2024.
For a star with the mass of the Sun, this period is around ten billion years. At 5 M ☉ the lifetime is 65 million years while at 25 M ☉ the core hydrogen–fusing period is only six million years. [7] The longest-lived stars are fully convective red dwarfs, which can stay on the main sequence for hundreds of billions of years or more. [8]
Astrochemistry overlaps with astrophysics and nuclear physics in characterizing the nuclear reactions which occur in stars, as well as the structure of stellar interiors. If a star develops a largely convective envelope, dredge-up events can occur, bringing the products of nuclear burning to the surface.