Late Spectral Evolution of the Ejecta and Reverse Shock in SN1987A

TL;DR

This study analyzes spectral observations of SN 1987A from 1999 to 2012, revealing the evolution of ejecta and reverse shock emissions, and discusses the effects of X-ray illumination and dust presence.

Contribution

It provides a detailed long-term spectral analysis of SN 1987A's ejecta and reverse shock, highlighting the impact of X-ray illumination on ejecta brightness and morphology.

Findings

Reverse shock flux increased 4-6 times from 2000 to 2007.

Outer ejecta are expected to brighten due to external X-ray illumination.

Evidence of dust inferred from line asymmetries.

Abstract

We present observations with VLT and HST of the broad emission lines from the inner ejecta and reverse shock of SN 1987A from 1999 until 2012 (days 4381 -- 9100 after explosion). We detect broad lines from H-alpha, H-beta, Mg I], Na I, [O I], [Ca II] and a feature at 9220 A. We identify the latter line with Mg II 9218, 9244,most likely pumped by Ly-alpha fluorescence. H-alpha, and H-beta both have a centrally peaked component, extending to 4500 km/s and a very broad component extending to 11,000 km/s, while the other lines have only the central component. The low velocity component comes from unshocked ejecta, heated mainly by X-rays from the circumstellar ring collision, whereas the broad component comes from faster ejecta passing through the reverse shock. The reverse shock flux in H-alpha has increased by a factor of 4-6 from 2000 to 2007. After that there is a tendency of flattening of the light curve, similar to what may be seen in soft X-rays and in the optical lines from the shocked ring. The core component seen in H-alpha, [Ca II] and Mg II has experienced a similar increase, consistent with that found from HST photometry. The ring-like morphology of the ejecta is explained as a result of the X-ray illumination, depositing energy outside of the core of the ejecta. The energy deposition in the ejecta of the external X-rays illumination is calculated using explosion models for SN 1987A and we predict that the outer parts of the unshocked ejecta will continue to brighten because of this. We finally discuss evidence for dust in the ejecta from line asymmetries.