Delayed detonation models for normal and subluminous type IA sueprnovae: Absolute brightness, light curves, and molecule formation

Höflich, Peter; Khokhlov, A. M.; Wheeler, J. C.

doi:10.1086/175656

Cited by 251 publications

(308 citation statements)

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“…Similar trends appear in the J, H, and K-band LC (Krisciunas et al 2004b), although interesting exceptions have been sought out (e.g., SN 2000cx Candia et al 2003). Despite the theoretical insights (e.g., Hoflich et al 1995;Wheeler et al 1998;Pinto & Eastman 2000a,b;Kasen 2006), the origin of the NIR secondary maximum and its dependence on the SN ejecta properties remain unclear. These NIR LCs therefore provide promising means of investigating a possible empirical secondary parameter, which may explain the deviations from the standard width-luminosity relation (Kasen 2006), and thus help us to understand the intrinsic differences among SNe Ia.…”

Section: Introductionmentioning

confidence: 80%

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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Aims. We present optical and near-infrared (NIR) photometry of supernova (SN) 2008fv and a brief investigation of SN type Ia to search for possible correlations between the properties of NIR light curves and the optical decline rate. Methods. We analyse our BVRI and JHK observations to derive light curves (LCs), colour curves, and the bolometric behaviour of SN 2008fv. Data range from about five days before to two months after maximum. We also collect a database of the main characteristics of NIR LCs of SNe Ia available in literature. Results. We find close similarities between the observed LCs of the SN event studied here and SN 2000E. SN 2008fv is a slow-declining SNe Ia with a post-maximum decline of Δm 15,B = 0.96 ± 0.08 mag and a B-band maximum luminosity of M B,0 = −19.40 ± 0.1 mag, close to the value of normal SNe Ia. The optical and NIR data allow us to constrain the host galaxy reddening of NGC 3147, E(B−V) = 0.22 ± 0.05 mag and its distance μ = 33.2 ± 0.1 mag. Furthermore, we derive a synthesized 56 Ni mass of about 0.7 M , by using the well-known relation between the maximum luminosity of the uvoir bolometric light curve and the initial content of 56 Ni. We investigate the correlation between the NIR characteristics of LCs and optical properties by collecting data of a sample of 40 SNe. We derive quantitative relationships involving the epoch of the secondary maximum in the JHK bands and the decline rate Δm 15 (B). Further, we find no correlations between Δm 15 measured in the JHK bands and the optical Δm 15 (B). In contrast, quite evident correlations with the Δm 15 (B) and Δm 40 (J)/Δm 15 (H).

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Section: Introductionmentioning

confidence: 80%

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

Biscardi

Brocato

Arkharov

et al. 2012

A&A

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“…At the time of the explosion of the WD, its central density ρ c is 2.0 × 10 9 g cm −3 and its mass is close to 1.37 M . The transition density ρ tr has been identified as the main factor that determines the 56 Ni production, and thus the brightness of a SNe Ia (Höflich 1995;Höflich et al 1995;Iwamoto et al 1999). The deflagration-to-detonation transition density is ρ tr = 8 × 10 6 g cm −3 .…”

Section: Delayed-detonation Modelmentioning

confidence: 99%

“…The ratio depends strongly on wavelength. P as a function of the inclination for a source located off-center, at a distance D = R ph /R of 3 (solid blue) and 1.5 (dotted red) (adopted from Höflich et al 1995). Note that D = 3 corresponds to SN 2005ke at day −8, when the photosphere R ph is formed at about 10 000 km s −1 , and assuming the maximum off-center 56 Ni distribution suggested by Maeda et al (2011) for core-normal SNe Ia.…”

Section: Continuum Polarizationmentioning

confidence: 99%

VLT Spectropolarimetry of the Type Ia SN 2005ke

Patat¹,

Hoêflich²,

Baade³

et al. 2012

A&A

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Aims. In this study we try to answer the question whether or not subluminous Type Ia supernovae have additional distinctive properties when examined from the point of view of the explosion geometry. Methods. We have performed optical spectropolarimetric observations of the Type Ia SN 2005ke at 3 epochs (days −8, −7, and +76). The explosion properties are derived by comparing the data to explosion and radiation transfer models. Results. The supernova shows polarimetric properties that are very similar to the only other subluminous event for which spectropolarimetry is available, i.e. SN 1999by. The data present a very marked dominant axis, which is shared by both the continuum and lines such as Si ii λ6355, suggesting that the relatively large, global asymmetry is common to the photosphere and the line-forming region. The maximum polarization degree observed in the Si ii λ6355 absorption reaches 0.39 ± 0.08%. At variance with what is seen in core-normal Type Ia, SN 2005ke displays significant continuum polarization, which grows from the blue to the red and peaks at about 7000 Å, reaching ∼0.7%. The properties of the polarization and flux spectra can be understood within the framework of a subluminous delayed-detonation (DD), or pulsating DD scenario, or white dwarf (WD) mergers. The difference in appearance with respect to core-normal SNe Ia is caused by low photospheric temperatures in combination with layers of unburned C, and more massive layers of the products of explosive C and O burning. The comparatively high level of continuum polarization is explained in terms of a significant global asymmetry (∼15%), which is well reproduced by an oblate ellipsoidal geometry within the general context of a DD explosion. Conclusions. Our results suggest that SN 2005ke arose either from a single-degenerate system in which the WD is especially rapidly rotating, close to the break-up velocity, or from a double-degenerate merger. Based on the current polarization data, we cannot distinguish between these two possibilities. Possible tests are discussed.

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“…The secondary maximum was first noted by Elias et al (1981). Höflich et al (1995) explained the secondary maximum as due to the expansion of the IR pseudophotosphere, whereas Suntzeff (1996) suggested that it was due to a global shift of radiation from blue to red. Pinto & Eastman (2000) suggested that the transition from Fe III to Fe II as the dominant ionization stage was important although they implied that the secondary maximum occurs when the photosphere has receded into the non-radioactive center.…”

Section: Introductionmentioning

confidence: 99%

Near-infrared light curves of type Ia supernovae

Jack

Hauschildt

Baron

2012

A&A

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Aims. With our time-dependent model atmosphere code PHOENIX, our goal is to simulate light curves and spectra of hydrodynamical models of all types of supernovae. In this work, we simulate near-infrared light curves of SNe Ia and confirm the cause of the secondary maximum. Methods. We apply a simple energy solver to compute the evolution of an SN Ia envelope during the free expansion phase. Included in the solver are energy changes due to expansion, the energy deposition of γ-rays and interaction of radiation with the material. Results. We computed theoretical light curves of several SN Ia hydrodynamical models in the I, J, H, and K bands and compared them to the observed SN Ia light curves of SN 1999ee and SN 2002bo. By changing a line scattering parameter in time, we obtained quite reasonable fits to the observed near-infrared light curves. This is a strong hint that detailed NLTE effects in IR lines have to be modeled, which will be a future focus of our work. Conclusions. We found that IR line scattering is very important for the near-infrared SN Ia light curve modeling. In addition, the recombination of Fe III to Fe II and of Co III to Co II is responsible for the secondary maximum in the near-infrared bands. For future work the consideration of NLTE for all lines (including the IR subordinate lines) will be crucial.

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Delayed detonation models for normal and subluminous type IA sueprnovae: Absolute brightness, light curves, and molecule formation

Cited by 251 publications

References 0 publications

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

The slowly declining type Ia supernova 2008fv and the near-infrared second maximum

VLT Spectropolarimetry of the Type Ia SN 2005ke

Near-infrared light curves of type Ia supernovae

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