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models_nmma [2022/02/10 14:54]
theoastro 		models_nmma [2023/06/16 10:32] (current)
theoastro
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-===== Models =====+===== Available models ===== 
 + 
 +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 [[https://github.com/nuclear-multimessenger-astronomy/nmma/blob/538326458e1e6101389e9861ff6bf19bc93fa070/nmma/em/model.py#L17|models.py]]  from time to time.
  
 === Kilonovae  === === Kilonovae  ===
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 === Shock Cooling supernovae  === === Shock Cooling supernovae  ===
 We use a model from [[https://arxiv.org/pdf/2007.08543|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: We use a model from [[https://arxiv.org/pdf/2007.08543|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,  +  *  the mass of extended material \(M_{e}\),  
-  *  the radius of extended material, +  *  the radius of extended material \(R_{e}\), 
-  *  the energy of material as the shock passes through it+  *  the energy of material as the shock passes through it \(E_{e}\)
  
 === Supernovae  === === Supernovae  ===
 We rely on a few different models for supernovae from [[https://github.com/sncosmo/sncosmo|sncosmo]]. For example, the nugent-hyper model [[https://arxiv.org/pdf/astro-ph/0403450|(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. We rely on a few different models for supernovae from [[https://github.com/sncosmo/sncosmo|sncosmo]]. For example, the nugent-hyper model [[https://arxiv.org/pdf/astro-ph/0403450|(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.
 +
 +Some models are analytic / semi-analytic that can be sampled, others rely on sampling from a grid of modeled light curves through the use of Principle Component Analysis (PCA) and an interpolation scheme (either Gaussian process modeling or neural networks). Further information on model training can be found [[https://enlil.gw.physik.uni-potsdam.de/dokuwiki/doku.php?id=model_grids|here]]
Last modified: le 2022/02/10 14:54

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