Remove a few more extra $'s

doc/models.md

@@ -13,9 +13,9 @@ These are optical counterparts to binary neutron star mergers generated by r-pro
 
 We use a model from [Kasen et al. 2017](https://arxiv.org/abs/1710.05463). The model is named Ka2017 in the code. The parameters are:
 
-* ejecta mass $$M_{\rm ej}$$
-* ejecta velocity $$v_{\rm ej}$$
-* lathanide fraction $$X_{\rm lan}$$
+* ejecta mass $M_{\rm ej}$
+* ejecta velocity $v_{\rm ej}$
+* lathanide fraction $X_{\rm lan}$
 
 The original light curves are available on GitHub [here](https://github.com/dnkasen/Kasen_Kilonova_Models_2017).
 
@@ -46,10 +46,10 @@ The half opening angle $\Phi$ is fixed to 30 deg. The original light curves are
 We use a model from [Anand et al. 2023](https://arxiv.org/abs/2307.11080), which is derived from [POSSIS](https://arxiv.org/abs/1906.04205), spanning the plausible binary neutron star parameter space. The model is named Bu2022mv in the code. The model parameters are:
 
 * dynamical ejecta mass $M^{\rm dyn}_{\rm ej}$
-* dynamical ejecta velocity $$v^{\rm dyn}_{\rm ej}$
+* dynamical ejecta velocity $v^{\rm dyn}_{\rm ej}$
 * disk wind ejecta mass $M^{\rm wind}_{\rm ej}$$
 * disk wind ejecta velocity $$v^{\rm wind}_{\rm ej}$
-* observation angle $\Theta_{\rm{obs}}$$
+* observation angle $\Theta_{\rm{obs}}$
 
 The original light curves are available on GitHub [here](https://github.com/mbulla/kilonova_models).