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11–15 Jun 2018
Geological Museum, University of Copenhagen
Europe/Copenhagen timezone

Old and new dust associated with Supernova 1995N

12 Jun 2018, 12:05
25m
Main Auditorium (Geological Museum, University of Copenhagen)

Main Auditorium

Geological Museum, University of Copenhagen

Øster Voldgade 5 - 7, 1350 København K, Denmark
Contributed talk The creation and evolution of dust Dust production by supernovae and massive stars

Speaker

Roger Wesson (University College London)

Description

The discovery of 0.4-0.7M$_\odot$ of dust in the remnant of SN1987A 23 years
after its explosion (Matsuura et al. 2011) demonstrated that supernovae can be
efficient dust factories, but raised many questions. Among them, when did this
dust form? Was it there at early times but previously undiagnosed by
techniques for estimating dust masses, or did it form at later times? In
Wesson et al. (2015) we created radiative transfer models to investigate this
question, fitting the optical-far IR SED of SN1987A to calculate the dust mass
at epochs from 600-9000 days after the explosion. We found that the rate of
dust formation could be represented by a sigmoid curve with peak dust
formation occurring many years after the explosion.

The far infrared observations necessary to constrain the emission from cold
dust are lacking in most supernovae. An alternative method of estimating the
dust mass exploits the blue-shifting of emission lines in the presence of dust
to diagnose the dust mass (Bevan and Barlow, 2016). This has the additional
advantage that only dust within the expanding remnant will affect the line
profiles - pre-existing dust that is thermally echoing will not.

I will present SED and emission line profile models of SN 1995N, observed as
part of a programme to determine dust masses in supernova remnants years to
decades old. Van Dyk (2013) found that mid-IR observations implied the
presence of 0.05-0.2Mo of pre-existing circumstellar dust which has been
flash-heated by the supernova outburst. I confirm this with three-dimensional
radiative transfer models to fit the SED. Additionally, emission line profile
modelling reveals that a further 0.1-0.4Mo of dust has formed in the expanding
supernova ejecta. This shows that pre-existing and newly formed dust can be
clearly distinguished in supernova remnants, and that both may contribute
significantly to the total dust mass formed by a massive star.

Consider for a poster? Yes

Primary author

Roger Wesson (University College London)

Presentation materials