Alpha process

The alpha process, also known as the alpha ladder, is one of two classes of nuclear fusion reactions by which stars convert helium into heavier elements, the other being the triple-alpha process. While the triple-alpha process only requires helium, once some carbon is present, these other reactions that consume helium are possible:

$\mathrm{_6^{12}C} + \mathrm{_2^4He} \rightarrow \mathrm{_{8}^{16}O} + \gamma$, Q = 7,16 МeV

$\mathrm{_8^{16}O} + \mathrm{_2^4He} \rightarrow \mathrm{_{10}^{20}Ne} + \gamma$, Q = 4,73 МeV

$\mathrm{_{10}^{20}Ne} + \mathrm{_2^4He} \rightarrow \mathrm{_{12}^{24}Mg} + \gamma$, Q = 9,32 МeV

$\mathrm{_{12}^{24}Mg} + \mathrm{_2^4He} \rightarrow \mathrm{_{14}^{28}Si} + \gamma$, Q = 9,98 МeV

$\mathrm{_{14}^{28}Si} + \mathrm{_2^4He} \rightarrow \mathrm{_{16}^{32}S} + \gamma$, Q = 6,95 МeV

$\mathrm{_{16}^{32}S} + \mathrm{_2^4He} \rightarrow \mathrm{_{18}^{36}Ar} + \gamma$, Q = 6,64 МeV

$\mathrm{_{18}^{36}Ar} + \mathrm{_2^4He} \rightarrow \mathrm{_{20}^{40}Ca} + \gamma$, Q = 7,04 МeV

$\mathrm{_{20}^{40}Ca} + \mathrm{_2^4He} \rightarrow \mathrm{_{22}^{44}Ti} + \gamma$, Q = 5,13 МeV

$\mathrm{_{22}^{44}Ti} + \mathrm{_2^4He} \rightarrow \mathrm{_{24}^{48}Cr} + \gamma$, Q = 7,70 МeV

$\mathrm{_{24}^{48}Cr} + \mathrm{_2^4He} \rightarrow \mathrm{_{26}^{52}Fe} + \gamma$, Q = 7,94 МeV

$\mathrm{_{26}^{52}Fe} + \mathrm{_2^4He} \rightarrow \mathrm{_{28}^{56}Ni} + \gamma$, Q = 8,00 МeV

Energy Q  is produced principally in gamma ray ($\gamma$)

In the center of large and old stars, alpha ($\mathrm{_2^4He}$) particles are needed for those alpha reactions and by inverses reactions, like photodisintegration of nuclei available in the center. $\mathrm{_{26}^{56}Ni}$ is the lighter per nucléons alpha nuclei. Production of heavier nuclei requires energy.

Ex: $\mathrm{_{26}^{56}Ni} + \mathrm{_2^4He} \rightarrow \mathrm{_{28}^{60}Zn} + \gamma$, Q = 2,71 МeV

Energy is produced in the isolated fusion reaction of nickel-56 with helium-4, but less than consumed to product of helium-4 by photodisintegration of heavier nuclei, causing alpha buildup of nickel-56 to be shut off due to the essential fact that nickel-56 has nucleon binding energy less zinc-60.

All these reactions have a very low rate at the temperatures and densities in stars and therefore do not contribute significantly to a star's energy production; with elements heavier than neon (atomic number > 10), they occur even less easily due to the increasing Coulomb barrier.

Alpha process elements (or alpha elements) are so-called since their most abundant isotopes are integer multiples of four, the mass of the helium nucleus (the alpha particle). Stable alpha elements are: C, O, Ne, Mg, Si, S, Ar, Ca. They are synthesized by alpha capture prior to the silicon fusing process, a precursor to Type II supernovae. Silicon and calcium are purely alpha process elements. Magnesium can be burned by proton capture reactions. As for oxygen, some authors consider it an alpha element, while others do not. Oxygen is surely an alpha element in low-metallicity population II stars. It is produced in Type II supernovae and its enhancement is well correlated with an enhancement of other alpha process elements. Sometimes carbon and nitrogen are considered alpha process elements, since they are synthesized in nuclear alpha-capture reactions.

The abundance of alpha elements in stars is usually expressed in a logarithmic manner:

$[\alpha/Fe] = \log_{10}{\left(\frac{N_{\alpha}}{N_{Fe}}\right)_{Star}} - \log_{10}{\left(\frac{N_{\alpha}}{N_{Fe}}\right)_{Sun}}$,

Here $N_{\alpha}$ and $N_{Fe}$ are the number of alpha elements and iron nuclei per unit volume. Theoretical galactic evolution models predict that early in the universe there were more alpha elements relative to iron. Type II supernovae mainly synthesize oxygen and the alpha-elements (Ne, Mg, Si, S, Ar, Ca and Ti) while Type Ia supernovae mainly produce elements of the iron peak (Ti, V, Cr, Mn, Fe, Co and Ni) but also alpha-elements.

External links

• The Age, Metallicity and Alpha-Element Abundance of Galactic Globular Clusters from Single Stellar Population Models