EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

Yamanaka, Masahito; Kawabata, Koji S.; Kinugasa, K.; Tanaka, Masaomi; Imada, Akira; Maeda, Keiichi; Nomoto, Ken’ichi; Arai, Akira; Chiyonobu, Shingo; Fukazawa, Yasushi; Hashimoto, Osamu; Honda, Satoshi; Ikejiri, Y.; Itoh, R.; Kamata, Yukiko; Kawai, N.; Komatsu, T.; Konishi, K.; Kuroda, D.; Miyamoto, Hisakazu; Miyazaki, Satoshi; Nagae, Osamu; Nakaya, Hidehiko; Ohsugi, T.; Omodaká, Toshihiro; Sakai, Nobuyuki; Sasada, Mahito; Suzuki, Mariko; Taguchi, Hikaru; Takahashi, H.; Tanaka, Hiroyuki; Uemura, Makoto; Yamashita, Takuya; Yanagisawa, K.; Yoshida, Michitoshi

doi:10.1088/0004-637x/707/2/l118

Cited by 159 publications

(158 citation statements)

References 37 publications

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“…Rather than the expected Si ii and Ca ii, its early spectrum displayed high-excitation lines of Fe iii but returned to normal a few months after maximum light. But recently other SNe Ia were found which are even more luminous than SN 1991T, with decline rates that put them well above the Phillips relation by almost one magnitude in the B-band, prototypical examples being SN 2006gz and SN 2009dc [61,[90][91][92][93][94]. By now, seven objects that may belong to this subclass have been discovered and they may contribute up to about 9% of all SNe Ia [33].…”

Section: A General Propertiesmentioning

confidence: 99%

Towards an understanding of Type Ia supernovae from a synthesis of theory and observations

et al. 2013

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Motivated by the fact that calibrated light curves of Type Ia supernovae (SNe Ia) have become a major tool to determine the expansion history of the Universe, considerable attention has been given to, both, observations and models of these events over the past 15 years. Here, we summarize new observational constraints, address recent progress in modeling Type Ia supernovae by means of three-dimensional hydrodynamic simulations, and discuss several of the still open questions. It will be be shown that the new models have considerable predictive power which allows us to study observable properties such as light curves and spectra without adjustable non-physical parameters. This is a necessary requisite to improve our understanding of the explosion mechanism and to settle the question of the applicability of SNe Ia as distance indicators for cosmology. We explore the capabilities of the models by comparing them with observations and we show how such models can be applied to study the origin of the diversity of SNe Ia.

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Section: A General Propertiesmentioning

confidence: 99%

Towards an understanding of Type Ia supernovae from a synthesis of theory and observations

et al. 2013

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“…(12), we obtain the corresponding constant magnetic field B of these stars configurations. We compare these values of B with the maximum value (B max ) allowed by the virial theorem (6). For these star configurations, the results are shown in Table 1, where we also calculate the magnetic energy W B given by Eq.…”

Section: Results and Conclusionmentioning

confidence: 99%

“…In this case, the low kinetic energies as well as the high luminosity, both observed in these supernovae could be explained by the higher binding energy of a super-Chandrasekhar object 3 . In this scenario, the such white dwarf would need to have a gravitational mass lying between (2.1 − 2.8)M , depending on the model used to estimate the nickel mass, to be able to successfully explain the observed properties of the superluminous Ia supernovae [3][4][5][6][7][8] . In a recent work, considering the effect of an extremely large uniform magnetic field inside the white dwarf, Das & Banibrata obtained a new mass limit for strongly magnetized white dwarfs of 2.58M , significantly higher than the Chandrasekhar mass limit of 1.44M…”

Section: Introductionmentioning

confidence: 99%

Ultra-magnetized white dwarfs are stable?

Malheiro¹,

Marinho²,

Lobato³

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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Recently the role of huge magnetic fields in white dwarfs (WDs) has been explore. It was proposed the existence of WDs with a magnetic field of 10 18 G with a critical mass Mmax ≈ 2.58M much larger than the Chandrasekhar limit ∼ 1.4M . These Ultra-magnetized super-Chandrasekhar white dwarfs were obtained not considering some physical aspects as virial theorem, breaking of spherical symmetry, inverse β-decay, and pycnonuclear fusion reactions, making them unstable. Taking in account these points, ultra-magnetized, supermassive and stable white dwarfs, with magnetic fields in their interior at maximum of the order of 10 13 − 10 14 G, even difficult to be formed, are possible to exist at least theoretically.

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“…SN 2009dc is one of the overluminous Type Ia supernovae (SNe Ia) and is estimated to have 1.2 M of 56 Ni (e.g., Yamanaka et al 2009). To explain the production of such a large mass of 56 Ni, its progenitor is proposed to be a super-Chandrasekhar-mass (super-Ch-mass) C-O white dwarf (WD).…”

mentioning

confidence: 99%

“…The "bolometric" LCs in the observations are not truly bolometric, but cover uvoir. For SN 2009dc, the observed uvoir luminosity is assumed to be ∼1.6 the integrated BVRI one (Yamanaka et al 2009), which is common for normal SNe Ia (Wang et al 2009). Since it is still unknown whether this assumption is true for overluminous SNe Ia, BVRI LCs are compared in the following.…”

mentioning

confidence: 99%

Light Curve Models for SN 2009dc

Kamiya

2011

Proc. IAU

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Abstract. Simplified explosion models of super-Chandrasekhar-mass C-O white dwarfs (WDs) are constructed with parameters such as WD mass and 56 Ni mass. Their light curves are obtained by solving one-dimensional equations of radiation hydrodynamics, and compared with the observations of SN 2009dc, one of the overluminous Type Ia supernovae, to estimate its properties. As a result, the progenitor of SN 2009dc is suggested to be a 2.2-2.4-M C-O WD with 1.2-1.4 M of 56 Ni, if the extinction by its host galaxy is negligible. To study the properties of SN 2009dc from its light curves (LCs), simplified explosion models of super-Ch-mass C-O WDs are constructed in a manner similar to Maeda & Iwamoto (2009 . Then the density and velocity structures are obtained by scaling those of W7 (Nomoto et al. 1984, Thielemann et al. 1986) with M W D and E kin . For its abundance distribution, the model consists of ECEs, 56 Ni, IMEs, and C-O layers, from the center to the surface. However, mixing is assumed for a certain region due to the observed slow Si ii line velocity (Yamanaka et al. 2009). The parameter ranges in this study areM IM E is hereafter not indicated. Any model whose E kin is not positive is excluded.The STELLA code is used to calculate the LCs, which solves one-dimensional equations of radiation hydrodynamics (e.g., Blinnikov et al. 1998). In this study, multi-band (U -, B-, V -, R-, and I-band) LCs are obtained, as well as bolometric ones. The "bolometric" LCs in the observations are not truly bolometric, but cover uvoir. For SN 2009dc, the observed uvoir luminosity is assumed to be ∼1.6 the integrated BVRI one (Yamanaka et al. 2009), which is common for normal SNe Ia (Wang et al. 2009). Since it is still unknown whether this assumption is true for overluminous SNe Ia, BVRI LCs are compared in the following.The resultant BVRI LCs of the models show a similar tendency to that in Maeda & Iwamoto (2009); a massive WD model has a wider BVRI LC and vice versa. Since SN 314 at https://www.cambridge.org/core/terms. https://doi

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EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

Cited by 159 publications

References 37 publications

Towards an understanding of Type Ia supernovae from a synthesis of theory and observations

Towards an understanding of Type Ia supernovae from a synthesis of theory and observations

Ultra-magnetized white dwarfs are stable?

Light Curve Models for SN 2009dc

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