A binary merger model for the formation of the Supernova 1987A triple-ring nebula

Details A binary merger model for the formation of the Supernova 1987A triple-ring nebula A binary merger model for the formation of the Supernova 1987A triple-ring nebula

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009mnras.399..515m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 399, Issue 2, pp. 515-538.

Astronomy and Astrophysics

Astronomy

4

Hydrodynamics, Circumstellar Matter, Supernovae: Individual: Supernova 1987A

Scientific paper

We examine a binary merger model for the formation of the mysterious triple-ring nebula surrounding Supernova 1987A, which still has not been convincingly explained in detailed hydrodynamical calculations. During the merger of 15 and 5Msolar binary systems, mass is ejected primarily at mid-latitudes for a sufficiently evolved primary, as demonstrated by Morris & Podsiadlowski. This material is swept up by the fast wind of the central star during its post-merger blue supergiant phase, leading to a density contrast of ~150 in the outer rings at the time of the supernova. The equatorial ring probably formed later when the star contracted to become a blue supergiant. The asymmetry between the northern and southern outer rings can be explained by a 10 per cent asymmetry during the merger, perhaps due to a pulsational instability in the common envelope.
We present a parameter study from which we determine a mass-loss rate in the blue supergiant wind in the range 1.5-3 × 10-7Msolaryr-1 in agreement with previous estimates. The morphology of the best model is consistent with the well-known Hubble Space Telescope image at better than 5 per cent and is also in broad agreement with light-echo observations. The circumstellar environment on larger scales (up to 3pc) is also investigated. We conclude with a brief discussion of the bipolar nebulae surrounding the Galactic stars, Sheridan 25, HD 168625 and η Carinae.

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