S-process

From Wikipedia, the free encyclopedia

Nuclear processes

Radioactive decay processes Alpha decay Beta decay Cluster decay Double beta decay Double electron capture Electron capture Gamma radiation Internal conversion Isomeric transition Neutron emission Positron emission Proton emission Spontaneous fission Nucleosynthesis Nuclear fusion Proton-proton chain reaction CNO cycle Triple-alpha process Carbon burning process Neon burning process Oxygen burning process Silicon burning process Neutron capture The R-process The S-process Proton capture: The P-process The Rp-process Spallation

The S-process or slow-neutron-capture-process is a nucleosynthesis process that occurs at relatively low neutron density and intermediate temperature conditions in stars. Under these conditions the rate of neutron capture by atomic nuclei is slow relative to the rate of radioactive beta-decay. A stable isotope captures another neutron; but a radioactive isotope decays to its stable daughter before the next neutron is captured. This process produces stable isotopes by moving along the valley of beta stability in the chart of isotopes. The S-process produces approximately half of the isotopes of the elements heavier than iron, and therefore plays an important role in the galactic chemical evolution. The S-process differs from the more rapid R-process of neutron-capture by its slow rate of neutron captures.

Contents 1 History 2 The S-process in stars 3 The S-process measured in Stardust 4 References

[edit] History

The S-process was seen to be needed from the relative abundances of isotopes of heavy elements and from a newly published table of abundances by Hans Suess and Harold Urey in 1956. A table apportioning the heavy isotopes between S-process and R-process was published in a famous review paper in 1957 ^[1] . There it was also argued that the S-process occurs in red giant stars. But a calculable model for creating the heavy isotopes from iron seed nuclei in a time dependent manner was not provided until 1961 ^[2]. That work showed that the large overabundances of barium observed by astronomers in certain red-giant stars could be created from iron seed nuclei if the total fluence (number of neutrons per unit area) of neutrons was appropriate. It also showed that no one single fluence could account for the observed S-process abundances, but that a wide range of fluences is required. The numbers of iron seed nuclei that were exposed to a given fluence must decrease as the fluence becomes stronger. This work also showed that the curve of the product of neutron-capture cross section times abundance is not a smoothly falling curve, but rather has a ledge-precipice structure. A series of papers in the 1970s by D. Clayton based on the assumption of an exponentially declining neutron fluence as a function of the number of iron seed so exposed became the standard model of the S-process and remained so until the details of AGB-star nucleosynthesis became advanced enough that they became a standard model based on the stellar structure models. Important series of measurements of neutron-capture cross sections were reported from Oak Ridge National Lab in 1965 ^[3] and by Karlsruhe Nuclear Physics Center in 1982 ^[4] and subsequently. These placed the s-process on the firm quantitative basis that it enjoys today.

[edit] The S-process in stars

The S-process is believed to occur mostly in Asymptotic Giant Branch stars. In contrast to the R-process which is believed to occur over time scales of seconds in explosive environments, the S-process is believed to occur over time scales of thousands of years. The extent to which the s-process moves up the elements in the chart of isotopes to higher mass numbers is essentially determined by the degree to which the star in question is able to produce neutrons, and by the amount of iron in the star's initial abundance distribution. Iron is the "starting material" (or seed) for this neutron capture - beta decay sequence of synthesizing new elements.

The main neutron source reactions are:

¹³C + α → ¹⁶O + n

²²Ne + α → ²⁵Mg + n

One distinguishes the main and the weak s-process component. The main component produces heavy elements beyond Sr and Y, and up to Pb in the lowest metallicity stars. The production site of the main component are low-mass Asymptotic Giant Branch stars. An excellent short discussion and illuminating figure of how both neutron sources operate in complicated pulsation cycles within the AGB stars can be found in Science magazine ^[5].The weak component of the S-process, on the other hand, synthesizes S-process isotopes of elements from the iron group up to Sr and Y, and takes place at the end of He- and C-burning in massive stars. These stars will become supernovae at their demise and spew those s isotopes into interstellar space.

The S-process is often mathematically treated using the so-called local approximation, which gives a theoretical model of elemental abundances based on the assumption of constant neutron flux in a star, so that the ratio of abundances is inversely proportional to the ratio of neutron-capture cross-sections for different isotopes. This approximation is - as the name indicates - only valid locally, meaning for isotopes of similar mass number.

Because of the relatively low neutron fluxes expected to occur during the S-process (on the order of 10⁵ to 10¹¹ neutrons per cm² per second), this process does not have the ability to produce any of the heavy radioactive isotopes such as Thorium or Uranium. The cycle that terminates the S-process is:

²⁰⁹Bi + n⁰ → ²¹⁰Bi + γ

²¹⁰Bi → ²¹⁰Po + β^-

²¹⁰Po → ²⁰⁶Pb + α

Pb-206 then captures three neutrons, producing Pb-209, which decays to Bi-209 by beta decay, restarting the cycle.

Nucleosynthesis

Stellar nucleosynthesis Big Bang nucleosynthesis Supernova nucleosynthesis Cosmic ray spallation

Related topics

Astrophysics Nuclear fusion R-process S-process Nuclear fission

edit

[edit] The S-process measured in Stardust

Stardust is one component of cosmic dust. Individual solid grains from various presolar stars are found in meteorites, where they have been preserved as interstellar grains that existed before the solar system. Stardust grains are demonstrated by laboratory measurements of extremely unsual isotopic abundance ratios within the grain. These mark them as solid pieces of dead stars. They give new astronomical information ^[6]. The silicon-carbide (SiC) Stardust grains condensed in the atmospheres of AGB stars and thus trap the isotopes of that star. Because the AGB stars are the main site of the s process in the galaxy, the heavy elements in the SiC grains are virtually pure S-process isotopes of those elements. This fact has been measured repeatedly by sputtering-ion mass spectrometers ^[7] in laboratories that study these presolar grains. Several surprising measurements have shown that the division between s process and r process abundances is somewhat different than previously assumed. It has also shown with trapped isotopes of krypton and xenon that the s process abundances in the stellar atmospheres change in time or from star to star, presumably with the strength of neutron fluence or perhaps the temperature. This is a frontier of S-process studies today.

[edit] References

1. ^ E.M. Burbidge, G.R. Burbidge, W.A. Fowler and F. Hoyle (1957). "Synthesis of Elements in Stars". REVIEWS OF MODERN PHYSICS 29: 547. 
2. ^ D. D. Clayton (1961). "Neutron capture chains in heavy-element sysnthesis". ANNALS OF PHYSICS 12: 331-408. 
3. ^ R. L. Macklin and J. H. Gibbons (1965). "Neutron Cross Sections for the s Process". REVIEWS OF MODERN PHYSICS 37: 166. 
4. ^ F. Kaeppeler, H. Beer, K. Wishak, D. D. Clayton, R.L. Macklin and R. A. Ward (1982). "s Process Studies in Light of New Experimental Cross Sections". ASTROPHYSICAL JOURNAL 257: 821-846. 
5. ^ a. Boothroyd (2006). "Heavy elements in stars". SCIENCE 314: 1690-91. 
6. ^ D. D. Clayton and L. R. Nittler (2004). "Astrohysics with Presolar Stardust". ANNUAL REVIEWS OF ASTRONOMY AND ASTROPHYSICS 42: 39-78. 
7. ^ D. D. Clayton and L. R. Nittler (2004). "Astrohysics with Presolar Stardust". ANNUAL REVIEWS OF ASTRONOMY AND ASTROPHYSICS 42: 39-78.