Spectral analysis of the 91bg-like Type Ia SN 2005bl: low luminosity, low velocities, incomplete burning

The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between −6 d...

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Published inMonthly notices of the Royal Astronomical Society Vol. 399; no. 3; pp. 1238 - 1254
Main Authors Hachinger, Stephan, Mazzali, Paolo A., Taubenberger, Stefan, Pakmor, Rüdiger, Hillebrandt, Wolfgang
Format Journal Article
LanguageEnglish
Published Oxford, UK Blackwell Publishing Ltd 01.11.2009
Wiley-Blackwell
Oxford University Press
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Abstract The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between −6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v≳ 15 000 km s−1). The zone between ∼8500 and 15 000 km s−1 is dominated by oxygen and includes some amount of intermediate-mass elements. At lower velocities, intermediate-mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible-to-moderate abundances of Fe-group elements, indicates large-scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at ≳13 000 km s−1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M⊙), but a kinetic energy reduced by ∼30 per cent (i.e. from 1.33 × 1051 to 0.93 × 1051 erg).
AbstractList The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between −6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v≳ 15 000 km s−1). The zone between ∼8500 and 15 000 km s−1 is dominated by oxygen and includes some amount of intermediate-mass elements. At lower velocities, intermediate-mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible-to-moderate abundances of Fe-group elements, indicates large-scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at ≳13 000 km s−1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M⊙), but a kinetic energy reduced by ∼30 per cent (i.e. from 1.33 × 1051 to 0.93 × 1051 erg).
The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between -6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v [gsim] 15 000 km s-1). The zone between similar to 8500 and 15 000 km s-1 is dominated by oxygen and includes some amount of intermediate-mass elements. At lower velocities, intermediate-mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible-to-moderate abundances of Fe-group elements, indicates large-scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at [gsim]13 000 km s-1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M[odot]), but a kinetic energy reduced by similar to 30 per cent (i.e. from 1.33 x 1051 to 0.93 x 1051 erg).
The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between -6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v [gsim] 15 000 km s-1). The zone between 68500 and 15 000 km s-1 is dominated by oxygen and includes some amount of intermediate-mass elements. At lower velocities, intermediate-mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible-to-moderate abundances of Fe-group elements, indicates large-scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at [gsim]13 000 km s-1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M[odot]), but a kinetic energy reduced by 630 per cent (i.e. from 1.33 x 1051 to 0.93 x 1051 erg).
ABSTRACT The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between −6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v≳ 15 000 km s−1). The zone between ∼8500 and 15 000 km s−1 is dominated by oxygen and includes some amount of intermediate‐mass elements. At lower velocities, intermediate‐mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible‐to‐moderate abundances of Fe‐group elements, indicates large‐scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at ≳13 000 km s−1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M⊙), but a kinetic energy reduced by ∼30 per cent (i.e. from 1.33 × 1051 to 0.93 × 1051 erg).
The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the structure of the dim SN Ia 2005bl. We infer the abundance and density profiles needed to reproduce the observed spectral evolution between -6 d and +12.9 d with respect to B maximum. Initially, we assume the density structure of the standard explosion model W7; then we test whether better fits to the observed spectra can be obtained using modified density profiles with different total masses and kinetic energies. Compared to normal SNe Ia, we find a lack of burning products especially in the rapidly expanding outer layers (v [~>] 15,000 km s-1). The zone between ~8500 and 15,000 km s-1 is dominated by oxygen and includes some amount of intermediate-mass elements. At lower velocities, intermediate-mass elements dominate. This holds down to the lowest zones investigated in this work. This fact, together with negligible-to-moderate abundances of Fe-group elements, indicates large-scale incomplete Si burning or explosive O burning, possibly in a detonation at low densities. Consistently with the reduced nucleosynthesis, we find hints of a kinetic energy lower than that of a canonical SN Ia: the spectra strongly favour reduced densities at [~>]13,000 km s-1 compared to W7, and are very well fitted using a rescaled W7 model with original mass (1.38 M[dotcircle]), but a kinetic energy reduced by ~30 per cent (i.e. from 1.33 x 1051 to 0.93 x 1051 erg). [PUBLICATION ABSTRACT]
Author Mazzali, Paolo A.
Taubenberger, Stefan
Hachinger, Stephan
Pakmor, Rüdiger
Hillebrandt, Wolfgang
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  givenname: Rüdiger
  surname: Pakmor
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  organization: Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
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  givenname: Wolfgang
  surname: Hillebrandt
  fullname: Hillebrandt, Wolfgang
  organization: Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
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Issue 3
Keywords supernovae: general
radiative transfer
techniques: spectroscopic
Type I supernova
Detonations
Nucleosynthesis
Luminosity
Standard model
Abundance
Radiative transfer
Kinetic energy
Spectral analysis
Language English
License CC BY 4.0
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SSID ssj0004326
Score 2.2280807
Snippet The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look at the...
ABSTRACT The properties of underluminous Type Ia supernovae (SNe Ia) of the 91bg subclass have yet to be theoretically understood. Here, we take a closer look...
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SubjectTerms Astronomy
Astrophysics
Earth, ocean, space
Exact sciences and technology
radiative transfer
Spectrum analysis
Supernovae
supernovae: general
techniques: spectroscopic
Theory
Title Spectral analysis of the 91bg-like Type Ia SN 2005bl: low luminosity, low velocities, incomplete burning
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