Update Lab1.md

Lab1.md

@@ -25,7 +25,7 @@ In order to smoothly lead into Lab2, we will start running a simulation with bot
 
 Assume that we have a binary star system where the components are close enough to undergo Roche Lobe overflow (RLOF) from the inner L1 Lagrangian point. Additionally, assume that both components do not have the same mass so that the evolution of one star slightly lags the other star. In the lab, we would like to explore how the primary - more massive - star evolves in such a binary.
 
-Since here we are primarily interested in the evolution of the primary, to save some computation time we are going to approximate the secondary as a point mass further. In other words, we are not going to model the evolution of the secondary. Then, later in Lab2, we will switch to treating the primary as a point mass and focus on evolving the secondary mass gainer (accretor).
+Since here we are primarily interested in the evolution of the primary, to save some computation time we are going to approximate the secondary as a point mass. In other words, we are not going to model the evolution of the secondary. Then, later in Lab2, we will switch to treating the primary as a point mass and focus on evolving the secondary mass gainer (accretor).
 
 
 Let's begin by using the downloaded `Lab1_binary` directory from the introduction. We will begin by modeling this system as a star + point mass. To do this, open `inlist_project` and make sure to set `evolve_both_stars = .false.`.
@@ -48,7 +48,7 @@ A range of parameters to adjust the mass transfer efficiency are also available
    mass_transfer_gamma = 0d0    ! radius of the circumbinary coplanar toroid is ``gamma**2 * orbital_separation``
 ```
 
-For non-conservative mass transfer, part of the mass that is transferred to the accretor escapes the system ($\dot{M}_2=-(1-\alpha-\beta-\delta)\dot{M}_1$). The lost mass can take away some angular momentum from the binary, and the amount of angular momentum it takes away depends on the details of the mass transfer flow. Each of the mass transfer parameters corresponds to a different angular momentum loss mode, as described in the comments. Here, we will assume that the non-accreted mass takes away the specific angular momentum of the accretor (Jeans mode mass loss). For example if half of the transferred mass is lost from the system, we set the parameters like this
+For non-conservative mass transfer, part of the mass that is transferred to the accretor escapes the system ($\dot{M}_2=-(1-\alpha-\beta-\delta)\dot{M}_1$). The lost mass can take away some angular momentum from the binary, and the amount of angular momentum it takes away depends on the details of the mass transfer flow. Each of the mass transfer parameters corresponds to a different angular momentum loss mode, as described in the comments. Here, we will assume that the non-accreted mass takes away the specific angular momentum of the accretor (Jeans mode mass loss). For example, if half of the transferred mass is lost from the system, we set the parameters like this
 
 ```
    mass_transfer_beta = 0.5d0     ! fraction of mass lost from the vicinity of accretor as fast wind