Detection of asymmetry of the photosphere of SN 1987A from scattering-line profiles

Astronomy and Astrophysics – Astronomy

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Scientific paper

Computations of the profiles of the NaI 5892A and Ba II6142 A resonance scattering lines in SN II 1987A in the photospheric stage show that a spherically symmetric model of the photosphere faithfully reproduces the observed profiles prior to the phase of the Bochum event (t ~ 20 days), which is characterized by the appearance of asymmetry in the hydrogen-line profiles. However, this model comes into serious conflict with the observed profiles of these lines at the peak of the Bochum event (t ~ 38 days). To a first approximation, the difference between the computed and observed profiles can be eliminated by displacing the spherically symmetric photosphere along the radial- velocity axis by +600 km s^-1^. The same result can be obtained with an eccentricity of the photosphere equal to 0.3, as confirmed by the appropriate computations of the scattering-line profiles. This asymmetry of the photosphere is due to an asymmetric distribution of the bulk of radioactive ^56^Ni in the envelope of SN 1987A. Qualitatively, the evolution of the photosphere of SN 1987A fits into the following scheme. At an early photospheric epoch (t < 30 days), the cooling wave is powered by the internal energy with a spherically symmetric distribution stored up after the passage of the shock wave through the envelope. After the bulk of the internal energy radiates away, the cooling wave ends up near the region of energy release via radioactive decay (v <= 2500 km s^-1^) which is markedly asymmetric due to the highly asymmetric distribution of the ejected ^56^Ni.

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