Abundance stratification in Type Ia supernovae - I. The case of SN 2002bo

By M.Stehle, P. Mazzali, S. Benetti, W. H. M. F. Astrophysik, Garching, Heidelberg · Germany, U. Muenchen, -INAF, Osservatorio astronomico di Trieste, Italy. and 1 more. 2004

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The abundance stratification in the ejecta of the normal Type Ia supernova 2002bo is derived by fitting a series of spectra obtained at close time intervals. A Monte Carlo code, modified to include abundance stratification, is used to compute synthetic spectra at 13 epochs in the photospheric phase, starting 13 d before B maximum. A description of the abundance distribution above 7600 km s −1 is thus obtained. Abundances in deeper layers, down to zero velocity, are derived from models of two nebular-phase spectra. Elements synthesized in different stages of burning are significantly, but not completely, mixed in the ejecta. A total 56 Ni mass of 0.52 M� is derived. Evidence for intermediate-mass elements at high velocities (18 000 km s −1 )i s found, most clearly in Si II 6355 A, in Ca II H&K ,and in the Ca II infrared triplet. Carbon lines are not seen at any velocity, with possible implications for the progenitor/explosion scenario. A synthetic bolometric light curve computed using the inferred abundance distribution is in very good agreement with the observed one, providing an independent check. In particular, the fast rise of the light curve is reproduced very well. This is due to outward mixing of 56 Ni, which is clearly well determined by the spectroscopic modelling. Ke yw ords: supernovae: general ‐ supernovae: individual: SN 2002bo.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3e17c60f2c2a50e5d061c4b244860546b9df565c

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In Astronomy and Astrophysics

1. M. Kromer
2. W. Hillebrandt
3. Rüdiger Pakmor
4. D. Maoz
5. F. Mannucci
6. D. Kasen
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In Instrumentation

1. D. Maoz
2. F. Mannucci
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4. A. Gal-yam
5. P. Mazzali
6. D. Howell
7. Garching
8. J. Sollerman

Citations in the corpus

• How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects (2012, methodology): “Our code has been presented by Lucy (1999) and Mazzali (2000) [see also Abbott & Lucy (1985), Mazzali & Lucy (1993)], and includes the possibility to specify a multi-zone chemical composition (Stehle et al. 2005).”
• Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae (2013, background): “…with normal SNe Ia, the explosion likely has to turn into a detonation at later burning stages (so-called delayed detonation models) to reproduce the abundance stratification inferred from spectral evolution (e.g. Stehle et al. 2005) and also to reach observed brightnesses/explosion energies.”
• Theoretical light curves for deflagration models of Type Ia supernova (2006, background): “Recent papers by Branch et al. (2005); Stehle et al. (2005) used spectroscopic analysis in different approximations and found that the composition structure in SNe Ia is stratified but has some degree of mixing.”
• Observational Clues to the Progenitors of Type Ia Supernovae (2013, methodology): “In one such modeling approach (e.g. Hachinger et al. 2013, Mazzali et al. 2007, Stehle et al. 2005, Tanaka et al. 2011), an ejecta density profile is assumed, based on a hydrodynamical explosion model.”
• NUCLEOSYNTHESIS IN TWO-DIMENSIONAL DELAYED DETONATION MODELS OF TYPE Ia SUPERNOVA EXPLOSIONS (2010, result): “• Abundance Stratification and carbon near the surface: Overall, the stratified composition structure obtained in our 2D models is consistent with the result of the ”abundance tomography” (Stehle et al. 2005; Mazzali et al. 2008).”
• 3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae (2012, result): “This is in clear contrast to normal SNe Ia, which are characterised by strongly layered ejecta (Stehle et al. 2005; Mazzali et al. 2007).”
• RADIATIVE TRANSFER SIMULATIONS OF NEUTRON STAR MERGER EJECTA (2013, unknown): “(A color version of this figure is available in the online journal.) supported by observations (see, e.g., Stehle et al. 2005; Mazzali et al. 2007, 2008; Tanaka et al. 2011).”
• NEUTRON-RICH CHROMIUM ISOTOPE ANOMALIES IN SUPERNOVA NANOPARTICLES (2010, background): “Yet, study of multi-epoch spectra of SNIa shows that mixing can take place (Stehle et al. 2005; Mazzali et al. 2008) and one cannot exclude the possibility that Cr-bearing oxides could condense in the outflows of those stars (either as new grains or as coatings on grains already present in the…”
• On the Progenitors of Type Ia Supernovae (2018, unknown): “This inferred stratification becomes even more convincing in detailed spectral models (e.g., Stehle et al. 2005; Tanaka et al. 2011).”
• SN 2003du: 480 days in the life of a normal type Ia supernova (2007, methodology): “For example, for SN 2002bo, using the abundance distribution and the amount of56Ni mixed out as derived from an abundance tomography experiment (Stehle et al., 2005) gavea much better reproduction of the bolometric light curve.”
• CONSTRAINING TYPE Ia SUPERNOVA MODELS: SN 2011fe AS A TEST CASE (2012, background): “However, they are reported in abundance tomographies of the normal SNe 2002bo (Stehle et al. 2005) and 2004eo (Mazzali et al. 2008) and Nugent et al. (2011b) identify iron in the earliest spectra of SN 2011fe at velocities of 16, 000 kms−1.”
• Three-dimensional delayed-detonation models with nucleosynthesis for Type Ia supernovae (2012, background): “We note that Stehle et al. (2005) find substantial amounts of stable iron out to velocities of about 9,000 analyzing spectra of SN 2002bo.”
• Hubble Space Telescope spectra of the type Ia supernova SN 2011fe: a tail of low-density, high-velocity material with Z < Z⊙ (2013, methodology): “Although it may be considered unphysical because of its parametrisations, W7 represnts a useful benchmark, and its density distribution has been successfully used to reproduce light curves and spectra of normal SNe Ia (e.g. Stehle et al. 2005; Mazzali et al. 2008).”