Free Access

Fig. A.2


Bolometric light curves from HERACLES simulations for the RSG progenitor. At ~125 d, the shock between ejecta and progenitor wind leaves the grid and causes a slight glitch in the luminosity. In some models (e.g., RE3B7), the light curve shows a small bump at late times in the photospheric phase. This feature is associated with the dense shell that results from the dynamical influence of the magnetar power (even though we adopt a broad energy deposition profile; see Sect. 3). Models with a higher initial magnetar energy and/or a higher magnetar field tend to produce a more massive dense shell and show this late light curve bump.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.