| 27 | | where [[latex($M_i$)]] is the mass of the sink particle at i, [[latex($dm_i$)]] is the total accreted mass for that time-step, [[latex($G$)]] is the gravitational constant in computational units, [[latex($R$)]] is the radius of the star, taken to be 1 solar radius by default, but modifiable by the user at run-time, and [[latex($dt$)]] is the hydro time-step. This luminosity is only computed after the sink particle has grown to have non-zero mass, and then will only be a source of luminosity after surrounding material has been deemed unstable and collapsing inward to the sink particle (i.e. is accreted). |
| | 27 | where [[latex($M_i$)]] is the mass of the sink particle at i, [[latex($dm_i$)]] is the total accreted mass for that time-step, [[latex($G$)]] is the gravitational constant in computational units, [[latex($R$)]] is the radius of the star, taken to be 1 solar radius by default, but modifiable by the user at run-time, and [[latex($dt$)]] is the hydro time-step. |
