Difference between revisions of "Bubble Chamber"
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| − | [[file:BubbleChamber.jpg|right | + | [[file:BubbleChamber.jpg|right|300px|]] |
| − | + | [[file:FirstBubble.gif|Rotate|degree=-90|right|300px|]] | |
| − | + | The carbon-helium fusion reaction is considered to be the key reaction in the helium | |
| + | burning of stars because it determines not only the carbon and oxygen abundances in stars | ||
| + | and, ultimately, in the universe, but also the nucleosynthesis of all heavier elements. | ||
| − | + | At Jefferson Lab, we plan to obtain the rate for this reaction by measuring the inverse | |
| + | process, i.e., the photo-disintegration of oxygen into helium and carbon. This measurement | ||
| + | would be based on a novel bubble-chamber technique, which makes use of the fact that a | ||
| + | super-heated liquid (Nitrous Oxide) is sensitive to recoiling helium and carbon nuclei produced | ||
| + | by photo-disintegration of the oxygen nuclei in the liquid. | ||
| − | + | This experiment will be staged in the exact place of the completed PEPPo experiment and | |
| + | will re-use the same beamline. The experiment will measure the <sup>16</sup>O(γ,α)<sup>12</sup>C reaction with | ||
| + | bremsstrahlung photons at 7 different electron beam kinetic energies ranging from 7.9 MeV | ||
| + | to 8.5 MeV. These energies are higher than what has been achieved in the Injector, thus the | ||
| + | need to increase the cryo-unit gradient. The uncertainty on the beam energy is the dominant | ||
| + | systematic error. To reduce the absolute energy error, a new dipole with | ||
| + | improved field homogeneity was installed. | ||
| − | |||
| − | * [[ | + | * <span style="font-size:150%"> '''[[Planning Meetings]]''' </span> |
| − | |||
| − | * [[ | + | * <span style="font-size:150%"> '''[[Bubble Chamber Reviews]]''' </span> |
| − | * [[References and Documents]] | + | |
| + | * <span style="font-size:150%"> '''[[Bubble Chamber Beam Tests]]''' </span> | ||
| + | |||
| + | |||
| + | * <span style="font-size:150%"> '''[[Simulations and Backgrounds]]''' </span> | ||
| + | |||
| + | |||
| + | * <span style="font-size:150%"> '''[[Penfold-Leiss Unfolding]]''' </span> | ||
| + | |||
| + | |||
| + | * <span style="font-size:150%"> '''[[Beamline, Radiator and Dump]]''' </span> | ||
| + | |||
| + | |||
| + | * <span style="font-size:150%"> '''[[Absolute Beam Energy]]''' </span> | ||
| + | |||
| + | |||
| + | * <span style="font-size:150%"> '''[[References and Documents]]''' </span> | ||
Latest revision as of 09:13, 15 December 2015
The carbon-helium fusion reaction is considered to be the key reaction in the helium burning of stars because it determines not only the carbon and oxygen abundances in stars and, ultimately, in the universe, but also the nucleosynthesis of all heavier elements.
At Jefferson Lab, we plan to obtain the rate for this reaction by measuring the inverse process, i.e., the photo-disintegration of oxygen into helium and carbon. This measurement would be based on a novel bubble-chamber technique, which makes use of the fact that a super-heated liquid (Nitrous Oxide) is sensitive to recoiling helium and carbon nuclei produced by photo-disintegration of the oxygen nuclei in the liquid.
This experiment will be staged in the exact place of the completed PEPPo experiment and will re-use the same beamline. The experiment will measure the 16O(γ,α)12C reaction with bremsstrahlung photons at 7 different electron beam kinetic energies ranging from 7.9 MeV to 8.5 MeV. These energies are higher than what has been achieved in the Injector, thus the need to increase the cryo-unit gradient. The uncertainty on the beam energy is the dominant systematic error. To reduce the absolute energy error, a new dipole with improved field homogeneity was installed.