Details

Autor(en) / Beteiligte

• Larsson, J.
• Fransson, C.
• Spyromilio, J.
• Leibundgut, B.
• Challis, P.
• Chevalier, R. A.
• France, K.
• Jerkstrand, A.
• Kirshner, R. P.
• Lundqvist, P.
• Matsuura, M.
• McCray, R.
• Smith, N.
• Sollerman, J.
• Garnavich, P.
• Heng, K.
• Lawrence, S.
• Mattila, S.
• Migotto, K.
• Sonneborn, G.
• Taddia, F.
• Wheeler, J. C.

Titel

THREE-DIMENSIONAL DISTRIBUTION OF EJECTA IN SUPERNOVA 1987A AT 10,000 DAYS

Ist Teil von

• The Astrophysical journal, 2016-12, Vol.833 (2), p.147

Ort / Verlag

Goddard Space Flight Center: The American Astronomical Society

Erscheinungsjahr

2016

Link zum Volltext

Quelle

Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals

Beschreibungen/Notizen

• ABSTRACT Due to its proximity, SN 1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN 1987A obtained ∼10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of H to date, the first 3D maps for [Ca ii] , [O i] , and Mg ii , as well as new maps for [Si i]+[Fe ii] and He i 2.058 m. A comparison with previous observations shows that the [Si i]+[Fe ii] flux and morphology have not changed significantly during the past ten years, providing evidence that this line is powered by 44Ti. The time evolution of H shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, H and [Si i]+[Fe ii] 1.644 m, show substructures at the level of ∼200-1000 km s-1and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.