diff --git a/doc/models.md b/doc/models.md index cd9f410a..2c96c3c4 100644 --- a/doc/models.md +++ b/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).