E2/M1 mixing in the Jπ= 5/2+ to 3/2+ transition in 21Na and its relation to the 20Ne(p,y ) stellar reaction rate
| dc.contributor.advisor | Triambak, Smarajit | |
| dc.contributor.author | Gopal, Sumeera | |
| dc.date.accessioned | 2023-02-03T08:09:11Z | |
| dc.date.accessioned | 2024-10-30T10:23:59Z | |
| dc.date.available | 2023-02-03T08:09:11Z | |
| dc.date.available | 2024-10-30T10:23:59Z | |
| dc.date.issued | 2022 | |
| dc.description | >Magister Scientiae - MSc | en_US |
| dc.description.abstract | In the above, M is the total mass of the molecular cloud, R is its radius, k is Boltzmann's constant, G is the gravitational constant, T is the cloud temperature, m is the mean molecular weight, and is the cloud molecular density. Interstellar clouds typically have densities of about 100 atoms cm3 and T ' 100 K. The Jeans criterion is only met when the mass of the cloud is greater than 2 104 M [5] (where M denotes one solar mass). The genesis of stars is initiated through such condensation of gas clouds in interstellar space. The gravitational collapse to a high central density results in the formation of a protostar. The internal heat that is generated is radiated away from the center, which is relatively hotter than the surface. | en_US |
| dc.identifier.uri | https://hdl.handle.net/10566/16702 | |
| dc.language.iso | en | en_US |
| dc.publisher | University of the Western Cape | en_US |
| dc.rights.holder | University of the Western Cape | en_US |
| dc.subject | Physics | en_US |
| dc.subject | Astronomy | en_US |
| dc.subject | Energy | en_US |
| dc.subject | Thermal energy | en_US |
| dc.title | E2/M1 mixing in the Jπ= 5/2+ to 3/2+ transition in 21Na and its relation to the 20Ne(p,y ) stellar reaction rate | en_US |