Tutorials

NMMA will be under continuous development meaning that new astrophysical models such as for kilonovae, supernovae, gamma-ray bursts and so on will be implemented over time. Therefore, it is worthwhile to check out the`model_parameters_dict` in models.py and

These are optical counterparts to binary neutron star mergers generated by r-process material produced (Metzger 2017). In this framework, we use a POSSIS-based grid of kilonova models spanning the plausible binary neutron star parameter space (Dietrich et al. 2020). There are four parameters:

• the dynamical ejecta mass \(M_{ej}^{dyn}\) ,
• the wind ejecta mass \(M_{ej}^{wind}\) ,
• the half opening angle \(\phi\) ,
• the observatoin angle \(\theta_{obs}\)

We use afterglowpy (Ryan et al. 2020), an open-source computational tool modeling forward shock synchrotron emission from relativistic blast waves as a function of jet structure and viewing angle. The model parameters are:

• the isotropic kinetic energy \(E_{K, iso}\) ,
• the jet collimation angle \(\theta_{c}\) ,
• the viewing angle \(\theta_{v}\) ,
• the circumburst constant density \(n\),
• the spectral slope of the electron distribution \(p\) ,
• the fraction of energy imparted to the electrons by the shock \(\epsilon_{e}\) ,
• the fraction of energy imparted to the magnetic field \(\epsilon_{B}\),

We use a model from Piro et al. 2021. Following shock breakout, the radiation of shock heated material expands and cools, known as shock cooling emission. The model has parameters:

• the mass of extended material \(M_{e}\),
• the radius of extended material \(R_{e}\),
• the energy of material as the shock passes through it \(E_{e}\)

We rely on a few different models for supernovae from sncosmo. For example, the nugent-hyper model (Levan et al. 2005) used for SN Ib/c supernovae with the stretch and scale set to match the intrinsic (dereddened, rest frame) -band luminosity of SN 1998bw at maximum light. The main free parameter is the absolute magnitude.