Beam analysis system for Texas A&M K500 cyclotron

Stellar reaction rate forMg22+p→Al-Abdullah1, Cârstoiu2, Chen3 et al. 2010Phys. Rev. C263160View full textAdd to dashboardCite

“…Taken all together, the above observations support the theory that the H-burning sequence of reactions can yield substantial concentrations of 22 Na in ONe novae, which is produced in the thermonuclear runaway during the high-temperature stage of the burning region mainly through the reaction chain 20 Ne(p,γ ) 21 Na(p,γ ) 22 Mg(β + ν) 22 Na. Then the radioactive 22 Na becomes a stalling point because of its slow decay rate to 22 Ne via the reaction 22 Na → 22 Ne + β + + ν. The half-life of 22 Na is t 1/2 = 2.603 yr. Its β + decay populates the short-lived first excited state in 22 Ne and leads to the emission of an identifying 1.275-MeV γ ray.…”

“…Moreover, the enrichment of 22 Ne in the so-called "Ne-E meteorites," which contain grains that might be partially condensed in nova outbursts, provides evidence of the pre-existence of sodium isotopes, namely 22 Na [5,6]. Taken all together, the above observations support the theory that the H-burning sequence of reactions can yield substantial concentrations of 22 Na in ONe novae, which is produced in the thermonuclear runaway during the high-temperature stage of the burning region mainly through the reaction chain 20 Ne(p,γ ) 21 Na(p,γ ) 22 Mg(β + ν) 22 Na. Then the radioactive 22 Na becomes a stalling point because of its slow decay rate to 22 Ne via the reaction 22 Na → 22 Ne + β + + ν.…”

“…The half-life of 22 Na is t 1/2 = 2.603 yr. Its β + decay populates the short-lived first excited state in 22 Ne and leads to the emission of an identifying 1.275-MeV γ ray. If the material is ejected before competing reactions deplete 22 Na, then it can be recognized by γ -ray telescopes. Moreover, because of its relatively short lifetime, 22 Na can give information about the distribution of matter produced in novae shortly after the outburst, complementary to that given by longer-lived isotopes like 26 Al.…”

“…If the material is ejected before competing reactions deplete 22 Na, then it can be recognized by γ -ray telescopes. Moreover, because of its relatively short lifetime, 22 Na can give information about the distribution of matter produced in novae shortly after the outburst, complementary to that given by longer-lived isotopes like 26 Al.…”

“…Then the radioactive 22 Na becomes a stalling point because of its slow decay rate to 22 Ne via the reaction 22 Na → 22 Ne + β + + ν. The half-life of 22 Na is t 1/2 = 2.603 yr. Its β + decay populates the short-lived first excited state in 22 Ne and leads to the emission of an identifying 1.275-MeV γ ray. If the material is ejected before competing reactions deplete 22 Na, then it can be recognized by γ -ray telescopes.…”