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Figure_list.md

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1. Introduction

2. Methods

2.1 Breif overview of SNEC

2.2 Opacities

  • opacity as a function of Ye, compare kNEC and Tanaka et al.

2.3 Heating rates

  • Heating rate trajectories as obtained by SkyNet
  • Heating rate fitted trajectories
  • SkyNet and fitted, 5 different representative sets of thermodynamic variables

2.4 Initial and boundary conditions

Initial ejecta profile

  • SFHo/BLh/DD2: Ye, density, velocity as a function of enclosed mass (2+ figures)
  • uniform/wind3/wind310/wind310T6(optimal wind): density, velocity, temperature as a function of radius (2+ figures)
  • Question
    1. ignore wind-ex profiles?
    2. compare hydro and homologous expansion here to explain why we use wind310, or leave this in code validation?

Boundary condition p(imax) = 0 and its problem

  • final velocity as a function of enclosed mass, wind310Tx profiles, no heating

  • final velocity as a function of enclosed mass, wind310Tx profiles, with heating (thermalization efficiency 0.5)

  • final velocity as a function of enclosed mass, blh profile, no heating

  • Question

    1. Do we need to mention that blh (with heating) boundary velocity exceeds speed of light?

      (Comparison with blh-with-modified-vel profile shows that this makes little difference to light curves. For the part of ejecta whose vel > 0.6c, mass and kinetic energy are negligible compared to the whole ejecta.)

2.5 Other difference with SNEC

  • Lbol: effects of mean molecular weight $\mu$, mean degree of ionization $\bar{y}$

2.6 Bolometric luminosities and multicolor luminosities

3. Code Validation

3.1 Hydrodynamics

  • Lbol: compare hydro and homologous expansion, using wind/optimal wind profiles
  • Lbol: compare hydro and homologous expansion (v = kr ?) , using blh-with-modified-vel profile
  • velocity fit: blh and blh-with-modified-vel
  • AB Mags: compare hydro and homologous expansion (?) , using blh-with-modified-vel profile
  • density of ejecta: compare hydro and homologous expansion

3.2 Energy conservation

  • E1 = Eejecta = Ekin + Egrav + Eint; E2 = Einitial + Eheating - Eradiation + boundary pdV work

    E1, E2 as a function of time; optimal wind/blh profiles

3.3 Comparison with analytic models

  • Lbol: kNEC VS Ricigliano's model, uniform/optimal wind, Ye = 0.1 ~ 0.4
  • Photospheric radius Rph, AB mags, Teff
  • kNEC VS Rahul's model

4. Ab-initio simulations: from mergers to kilonovae

4.1 General Features

  • ? Lbol, AB Mags, Energy, Rph, Teff

4.2 Impact of uncertainties in heating rates

  • Lbol/heating rate: wind/optimal wind, heating x3, x3 (0-10 sec), x0.3, x0.3 (0-10 sec), high Ye 0.4, low Ye0.1

  • Lbol/AB Mags: blh profile, heating x3, x3 (0-10 sec), x0.3, x0.3 (0-10 sec)

    ? combine this with piston shock results

5. A first application to AT2017GFO (Combine this with 4?)

5.2 Comparison between NR informed models and observations

  • blh/sfho extrapolation method: density/mass as a function of time
  • AB Mags: blh and extrapolated blh

5.3 Impact of shock injection