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Title: Light and Color Curve Properties of Type Ia Supernovae: Theory Versus Observations

Abstract

We study the optical light curve (LC) relations of Type Ia supernovae (SNe Ia) for their use in cosmology using high-quality photometry published by the Carnegie Supernova Project (CSP-I). We revisit the classical luminosity decline rate (Δ m {sub 15}) relation and the Lira relation, as well as investigate the time evolution of the ( B − V ) color and B ( B − V ), which serves as the basis of the color–stretch relation and Color–MAgnitude Intercept Calibrations (CMAGIC). Our analysis is based on explosion and radiation transport simulations for spherically symmetric delayed-detonation models (DDT) producing normal-bright and subluminous SNe Ia. Empirical LC relations can be understood as having the same physical underpinnings, i.e., opacities, ionization balances in the photosphere, and radioactive energy deposition changing with time from below to above the photosphere. Some three to four weeks past maximum, the photosphere recedes to {sup 56}Ni-rich layers of similar density structure, leading to a similar color evolution. An important secondary parameter is the central density ρ {sub c} of the WD because at higher densities, more electron-capture elements are produced at the expense of {sup 56}Ni production. This results in a Δ m {sub 15} spread of 0.1more » mag in normal-bright and 0.7 mag in subluminous SNe Ia and ≈0.2 mag in the Lira relation. We show why color–magnitude diagrams emphasize the transition between physical regimes and enable the construction of templates that depend mostly on Δ m {sub 15} with little dispersion in both the CSP-I sample and our DDT models. This allows intrinsic SN Ia variations to be separated from the interstellar reddening characterized by E ( B − V ) and R {sub B}. Invoking different scenarios causes a wide spread in empirical relations, which may suggest one dominant scenario.« less

Authors:
;  [1];  [2];  [3];  [4];  [5];  [6];  [7]; ; ;  [8]; ;  [9]
  1. Department of Physics, Florida State University, Tallahassee, FL 32306 (United States)
  2. Astrophysics Research Institute, Liverpool John Moore University, 146 Brownlow Hill, Liverpool L3 5RF (United Kingdom)
  3. Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101 (United States)
  4. NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)
  5. Carnegie Observatories, Las Campanas Observatory, Casilla 601 La Serena (Chile)
  6. Physics and Astronomy Department, Texas Tech University, Box 41051, Lubbock, TX 79409-1051 (United States)
  7. Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000, Aarhus (Denmark)
  8. The G.P. and C. Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A and M University, Department of Physics and Astronomy, 4242 TAMU, College Station, TX 77843 (United States)
  9. Departamento de Física, Universidad Técnica Federico Santa Maria, Ava España 1680, Casilla 110-V, Valparaiso (Chile)
Publication Date:
OSTI Identifier:
22663171
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 846; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COSMOLOGY; DENSITY; DISPERSIONS; ELECTRON CAPTURE; ELECTRONS; ENERGY ABSORPTION; ENERGY LOSSES; IONIZATION; LAYERS; LUMINOSITY; NICKEL 56; OPACITY; PHOTOMETRY; PHOTOSPHERE; RADIANT HEAT TRANSFER; RADIATION TRANSPORT; SIMULATION; SYMMETRY; TYPE I SUPERNOVAE

Citation Formats

Hoeflich, P., Hsiao, E. Y., Ashall, C., Burns, C. R., Diamond, T. R., Phillips, M. M., Sand, D., Stritzinger, M. D., Suntzeff, N., Krisciunas, K., Wang, L., Contreras, C., and Morrell, N., E-mail: phoeflich77@gmail.com. Light and Color Curve Properties of Type Ia Supernovae: Theory Versus Observations. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA84B2.
Hoeflich, P., Hsiao, E. Y., Ashall, C., Burns, C. R., Diamond, T. R., Phillips, M. M., Sand, D., Stritzinger, M. D., Suntzeff, N., Krisciunas, K., Wang, L., Contreras, C., & Morrell, N., E-mail: phoeflich77@gmail.com. Light and Color Curve Properties of Type Ia Supernovae: Theory Versus Observations. United States. doi:10.3847/1538-4357/AA84B2.
Hoeflich, P., Hsiao, E. Y., Ashall, C., Burns, C. R., Diamond, T. R., Phillips, M. M., Sand, D., Stritzinger, M. D., Suntzeff, N., Krisciunas, K., Wang, L., Contreras, C., and Morrell, N., E-mail: phoeflich77@gmail.com. Fri . "Light and Color Curve Properties of Type Ia Supernovae: Theory Versus Observations". United States. doi:10.3847/1538-4357/AA84B2.
@article{osti_22663171,
title = {Light and Color Curve Properties of Type Ia Supernovae: Theory Versus Observations},
author = {Hoeflich, P. and Hsiao, E. Y. and Ashall, C. and Burns, C. R. and Diamond, T. R. and Phillips, M. M. and Sand, D. and Stritzinger, M. D. and Suntzeff, N. and Krisciunas, K. and Wang, L. and Contreras, C. and Morrell, N., E-mail: phoeflich77@gmail.com},
abstractNote = {We study the optical light curve (LC) relations of Type Ia supernovae (SNe Ia) for their use in cosmology using high-quality photometry published by the Carnegie Supernova Project (CSP-I). We revisit the classical luminosity decline rate (Δ m {sub 15}) relation and the Lira relation, as well as investigate the time evolution of the ( B − V ) color and B ( B − V ), which serves as the basis of the color–stretch relation and Color–MAgnitude Intercept Calibrations (CMAGIC). Our analysis is based on explosion and radiation transport simulations for spherically symmetric delayed-detonation models (DDT) producing normal-bright and subluminous SNe Ia. Empirical LC relations can be understood as having the same physical underpinnings, i.e., opacities, ionization balances in the photosphere, and radioactive energy deposition changing with time from below to above the photosphere. Some three to four weeks past maximum, the photosphere recedes to {sup 56}Ni-rich layers of similar density structure, leading to a similar color evolution. An important secondary parameter is the central density ρ {sub c} of the WD because at higher densities, more electron-capture elements are produced at the expense of {sup 56}Ni production. This results in a Δ m {sub 15} spread of 0.1 mag in normal-bright and 0.7 mag in subluminous SNe Ia and ≈0.2 mag in the Lira relation. We show why color–magnitude diagrams emphasize the transition between physical regimes and enable the construction of templates that depend mostly on Δ m {sub 15} with little dispersion in both the CSP-I sample and our DDT models. This allows intrinsic SN Ia variations to be separated from the interstellar reddening characterized by E ( B − V ) and R {sub B}. Invoking different scenarios causes a wide spread in empirical relations, which may suggest one dominant scenario.},
doi = {10.3847/1538-4357/AA84B2},
journal = {Astrophysical Journal},
number = 1,
volume = 846,
place = {United States},
year = {Fri Sep 01 00:00:00 EDT 2017},
month = {Fri Sep 01 00:00:00 EDT 2017}
}