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16 Eylül 2012 Saat : 5:52
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View original: http://arxiv.org/abs/1209.2520
We study the nature of phase transition in classical Heisenberg model on triangular lattice with competing interactions. In frustrated systems, various types of phase transitions occur depending on the lattice and spin symmetries. Recently, a first-order phase transition with threefold symmetry breaking in frustrated Heisenberg model on triangular lattice was discovered [R. Tamura and N. Kawashima, J. Phys. Soc. Jpn. 80, 074008 (2011)]. To change the underlying symmetry, we introduce a uniaxial distortion effect into their model. We find the order of the phase transition changes into the second order when the spontaneous breaking of the twofold symmetry occurs. Moreover, dissociation of Z_2 vortex pairs occurs at the second-order phase transition point.
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View original: http://arxiv.org/abs/1209.1339
Extremely luminous, super-Chandrasekhar (SC) Type Ia Supernovae (SNe Ia) are as yet an unexplained phenomenon. We analyse a well-observed SN of this class, SN 2009dc, by modelling its photospheric spectra with a spectral synthesis code, using the technique of 'Abundance Tomography'. We present spectral models based on different density profiles, corresponding to different explosion scenarios, and discuss their consistency. First, we use a density structure of a simulated explosion of a 2 M_sun rotating C-O white dwarf (WD), which is often proposed as a possibility to explain SC SNe Ia. Then, we test a density profile empirically inferred from the evolution of line velocities (blueshifts). This model may be interpreted as a core-collapse SN with an ejecta mass \sim 3 M_sun. Finally, we calculate spectra assuming an interaction scenario. In such a scenario, SN 2009dc would be a standard WD explosion with a normal intrinsic luminosity, and this luminosity would be augmented by interaction of the ejecta with a H-/He-poor circumstellar medium. We find that no model tested easily explains SN 2009dc. With the 2 M_sun WD model, our abundance analysis predicts small amounts of burning products in the intermediate-/high-velocity ejecta (v > 9000 km/s). However, in the original explosion simulations, where the nuclear energy release per unit mass is large, burned material is present at high v. This contradiction can only be resolved if asymmetries strongly affect the radiative transfer or if C-O WDs with masses significantly above 2 M_sun exist. In a core-collapse scenario, low velocities of Fe-group elements are expected, but the abundance stratification in SN 2009dc seems 'SN Ia-like'. The interaction-based model looks promising, and we have some speculations on possible progenitor configurations. However, radiation-hydro simulations will be needed to judge whether this scenario is realistic at all.
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