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Turning point might may not depend on recession," 22 Mar. First Known Use of heavy Adjective before the 12th century, in the meaning defined at sense 1a Adverb before the 12th century, in the meaning defined above Noun , in the meaning defined at sense 1.

Learn More about heavy. Time Traveler for heavy The first known use of heavy was before the 12th century See more words from the same century.

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More Definitions for heavy. US , informal : a person or thing that is serious, important, or powerful. Kids Definition of heavy.

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Love words? Fowler and Donald D. Clayton , [8] who found that no single temporal snapshot matched the solar r -process abundances, but, that when superposed, did achieve a successful characterization of the r -process abundance distribution.

Seeger et al. Today, the r -process abundances are determined using their technique of subtracting the more reliable s -process isotopic abundances from the total isotopic abundances and attributing the remainder to r -process nucleosynthesis.

The creation of free neutrons by electron capture during the rapid collapse to high density of a supernova core along with quick assembly of some neutron-rich seed nuclei makes the r -process a primary nucleosynthesis process , meaning a process that can occur even in a star initially of pure H and He, in contrast to the B 2 FH designation as a secondary process building on preexisting iron.

Primary stellar nucleosynthesis begins earlier in the galaxy than does secondary nucleosynthesis. Alternatively the high density of neutrons within neutron stars would be available for rapid assembly into r -process nuclei if a collision were to eject portions of a neutron star, which then rapidly expands freed from confinement.

That sequence could also begin earlier in galactic time than would s -process nucleosynthesis; so each scenario fits the earlier growth of r -process abundances in the galaxy.

Each of these scenarios is the subject of active theoretical research. Observational evidence of the early r -process enrichment of interstellar gas and of subsequent newly formed of stars, as applied to the abundance evolution of the galaxy of stars, was first laid out by James W.

Truran in This was consistent with the hypothesis that the s -process had not yet begun to enrich interstellar gas when these young stars missing the s -process abundances were born from that gas, for it requires about million years of galactic history for the s -process to get started whereas the r -process can begin after two million years.

These s -process—poor, r -process—rich stellar compositions must have been born earlier than any s -process, showing that the r -process emerges from quickly evolving massive stars that become supernovae and leave neutron-star remnants that can merge with another neutron star.

The primary nature of the early r -process thereby derives from observed abundance spectra in old stars [4] that had been born early, when the galactic metallicity was still small, but that nonetheless contain their complement of r -process nuclei.

Either interpretation, though generally supported by supernova experts, has yet to achieve a totally satisfactory calculation of r -process abundances because the overall problem is numerically formidable, but existing results are supportive.

In , new data about the r -process was discovered when the LIGO and Virgo gravitational-wave observatories discovered a merger of two neutron stars ejecting r -process matter.

Noteworthy is that the r -process is responsible for our natural cohort of radioactive elements, such as uranium and thorium, as well as the most neutron-rich isotopes of each heavy element.

There are three candidate sites for r -process nucleosynthesis where the required conditions are thought to exist: low-mass supernovae , Type II supernovae , and neutron star mergers.

Immediately after the severe compression of electrons in a Type II supernova, beta-minus decay is blocked. This is because the high electron density fills all available free electron states up to a Fermi energy which is greater than the energy of nuclear beta decay.

However, nuclear capture of those free electrons still occurs, and causes increasing neutronization of matter. This results in an extremely high density of free neutrons which cannot decay, on the order of 10 24 neutrons per cm 3 , [1] and high temperatures.

As this re-expands and cools, neutron capture by still-existing heavy nuclei occurs much faster than beta-minus decay.

As a consequence, the r -process runs up along the neutron drip line and highly-unstable neutron-rich nuclei are created.

Three processes which affect the climbing of the neutron drip line are a notable decrease in the neutron-capture cross section in nuclei with closed neutron shells , the inhibiting process of photodisintegration , and the degree of nuclear stability in the heavy-isotope region.

Neutron captures in r -process nucleosynthesis leads to the formation of neutron-rich, weakly bound nuclei with neutron separation energies as low as 2 MeV.

These so-called waiting points are characterized by increased binding energy relative to heavier isotopes, leading to low neutron capture cross sections and a buildup of semi-magic nuclei that are more stable toward beta decay.

Decreasing nuclear stability terminates the r -process when its heaviest nuclei become unstable to spontaneous fission, when the total number of nucleons approaches The fission barrier may be low enough before such that neutron capture might induce fission instead of continuing up the neutron drip line.

The r -process also occurs in thermonuclear weapons, and was responsible for the initial discovery of neutron-rich almost stable isotopes of actinides like plutonium and the new elements einsteinium and fermium atomic numbers 99 and in the s.

It has been suggested that multiple nuclear explosions would make it possible to reach the island of stability , as the affected nuclides starting with uranium as seed nuclei would not have time to beta decay all the way to the quickly spontaneously fissioning nuclides at the line of beta stability before absorbing more neutrons in the next explosion, thus providing a chance to reach neutron-rich superheavy nuclides like copernicium and which should have half-lives of centuries or millennia.

The most probable candidate site for the r -process has long been suggested to be core-collapse supernovae spectral types Ib , Ic and II , which may provide the necessary physical conditions for the r -process.

However, the very low abundance of r -process nuclei in the interstellar gas limits the amount each can have ejected. It requires either that only a small fraction of supernovae eject r -process nuclei to the interstellar medium , or that each supernova ejects only a very small amount of r -process material.

The ejected material must be relatively neutron-rich, a condition which has been difficult to achieve in models, [2] so that astrophysicists remain uneasy about their adequacy for successful r -process yields.

In , entirely new astronomical data about the r -process was discovered in data about the merger of two neutron stars.

Using the gravitational wave data captured in GW to identify the location of the merger, several teams [21] [22] [23] observed and studied optical data of the merger, finding spectroscopic evidence of r -process material thrown off by the merging neutron stars.

When released from the huge internal pressure of the neutron star, these ejecta expand and form seed heavy nuclei that rapidly capture free neutrons, and radiate detected optical light for about a week.

Such duration of luminosity would not be possible without heating by internal radioactive decay, which is provided by r -process nuclei near their waiting points.

These results offer a new possibility for clarifying six decades of uncertainty over the site of origin of r -process nuclei. Confirming relevance to the r -process is that it is radiogenic power from radioactive decay of r -process nuclei that maintains the visibility of these spun off r -process fragments.

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