| | 69 | '''Prediction''': Initially, |
| | 70 | |
| | 71 | [[latex($\frac{E_{rad}}{E_{gas}}=\frac{aT^4}{nKT}=4e-4$)]] |
| | 72 | |
| | 73 | So the radiation will not induce appreciable changes in the temperature. |
| | 74 | |
| | 75 | However, given the luminosity is, |
| | 76 | |
| | 77 | [[latex($L=3.9~e+29 ~erg~s^{-1}$)]], |
| | 78 | |
| | 79 | I expect a swift increase in the radiative energy of the core such that, Erad >> Egas. More precisely, given the diffusion time from sink to boundary is 24 days, we can get a 'diffusion speed' and use it to calculate the time for the diffusion wave to hit any part of the core. At that point, the Erad >> Egas, and thus, we can expect significant heating of the gas (so long as the coupling time is short). |
| | 80 | |
| | 81 | Consider this is the case for small pre-stellar cores, and perhaps why radiative feedback is so important. With high mass star formation it will inevitably take longer to heat the gas. |
| | 82 | |
| | 83 | Here are my initial energy budgets: |
| | 84 | |
| | 85 | || Erad || aT^4^=7.565e-11 erg/cm^3^ || |
| | 86 | || Egas || nKT=1.656e-7 erg/cm^3^ || |
| | 87 | || Estar || || |
| | 88 | |
