Constraints on the progenitor systems of type Ia supernovae

By M. Stritzinger, B. Leibundgut, Stefanie Walch, G. Contardo. 2005

133 citations recorded by the source corpus.

Bolometric light curves provide a valuable insight into the nature of type Ia supernovae. We present an analysis of sixteen well-observed type Ia supernovae. Constraints are placed on several global parameters concerning the progenitor system, explosion mechanism, and subsequent radiation transport. By fitting a radioactive decay energy deposition function to the quasi-exponential phase (50 to 100 days after maximum light), it is found that the ejected mass varies by at least a factor of two. This result suggests that a sub Chandrasekhar mass white dwarf could be the progenitor system of some type Ia supernovae. We find that the range in the amount of synthesized $\rm ^{56}Ni$ indicates a significant variation in the burning mechanism. In order to explain a factor of ten range in the observed bolometric luminosity, more detailed modeling of the explosion mechanism is required.

View Paper: https://www.semanticscholar.org/paper/75b354ee3bd5a72be57b4766ebacf9ff646fce52

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Citations in the corpus

• Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae (2013, background): “The maximum 56Ni mass of 0.38 M , which is produced in model N150def, is marginally compatible with the lower end of the distribution of 56Ni masses reported for normal SNe Ia (cf. e.g. Stritzinger et al. 2006).”
• Double-detonation supernovae of sub-Chandrasekhar mass white dwarfs (2007, background): “…the unknown nature of the progenitor systems because neither observations nor theoretical models are yet conclusive (Branch et al. 1995; Ruiz-Lapuente et al. 2000; Livio 2000; Nomoto et al. 2003; Han & Podsiadlowski 2004; Napiwotzki et al. 2005; Stritzinger et al. 2006; Parthasarathy et al. 2007).”
• Double-detonation sub-Chandrasekhar supernovae: can minimum helium shell masses detonate the core? (2010, background): “In principle, this range is sufficiently broad to encompass all major classes of type Ia supernovae (cf., e.g., Stritzinger et al. 2006, for a sample of 56Ni masses determined for 16 well-observed SNe Ia): the high mass end of subluminous SN 1991bg7-like events (∼0.07−0.17 M : Model 1), normal type…”
• SUB-CHANDRASEKHAR WHITE DWARF MERGERS AS THE PROGENITORS OF TYPE Ia SUPERNOVAE (2010, background): “Stritzinger et al. (2006) use peak luminosities to infer similar56Ni masses, but their total masses, inferred from the times that the ejecta become optically thin, do not cluster, but range from 0.5 to 1.3M⊙.”
• The Peculiar SN 2005hk: Do Some Type Ia Supernovae Explode as Deflagrations? (2006, background): “3 # 10 1982; Arnett et al. 1985) as per the prescription given by Stritzinger et al. (2006), we estimate that a 56Ni mass of ∼0.2 M, was produced during the explosion of SN 2005hk (see § 5).”
• Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries (2007, background): “These events come close to matching the peak brightnesses of sub-luminous Type Ia supernovae like 1991bg, though the observed long decay time requires an ejected mass> 0.1M⊙ (Stritzinger et al. 2006).”
• DETONATIONS IN SUB-CHANDRASEKHAR-MASS C+O WHITE DWARFS (2010, background): “First, it has already been suggested by empirical modelling of bolometric SNe Ia light curves (Stritzinger et al. 2006) that differing ejecta masses may be required for different SNe Ia, a property which the sub-MCh model may explain.”
• TYPE Iax SUPERNOVAE: A NEW CLASS OF STELLAR EXPLOSION (2012, methodology): “To determine the amount of 56Ni produced by SNe Ia, we use the Stritzinger et al. (2006) sample of SNe Ia.”
• Secondary Maximum in the Near-Infrared Light Curves of Type Ia Supernovae (2006, result): “This conclusion coincides with several other inferences to the same (Contardo et al. 2000; Mazzali et al. 1998; Stritzinger et al. 2006).”
• The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry (2007, methodology): “We obtain the values k RR I ¼ 0:030 and k IR I ¼ 0:030 by combining our own work with the information reported on the CTIO 4mWeb site25 and with synthetic photometry using 4 mMOSAIC passbands and the Stritzinger et al. (2006) spectrophotometric standards.”
• CONSTRAINING TYPE Ia SUPERNOVA MODELS: SN 2011fe AS A TEST CASE (2012, background): “Assuming a distance to M101 of 6.4Mpc (Shappee & Stanek 2011), SN 2011fe is a normal SN Ia with MB,max = −19.13, having produced ∼0.6M⊙ of 56Ni (Stritzinger et al. 2006).”