Old cold dust heated by supernova 1987A

  title={Old cold dust heated by supernova 1987A},
  author={Patrick F. Roche and David K. Aitken and C. H. Smith and S. D. James},
The mid-infrared emission (at wavelengths near 10 μm) from SN1987A, which had been fading steadily since reaching a peak about 120 days after outburst, began to increase again on about day 4501. This increase has continued up to at least day 578, and is probably due to heating of dust grains by light emitted at the optical maximum. Here we present additional observations and discuss the mass, location and nature of the emitting dust. The dust grains cannot have formed in the ejecta of the… 

Infrared and optical evidence for a dust cloud behind supernova 1987A

THE 8–13-μm flux from supernova 1987A has increased substantially1 since around May 1988 (∼ 450 days after the explosion), and the 8–13-μm source has been resolvable1, having a full width at half

Far-infrared observations of thermal dust emission from supernova 1987A

INFRARED observations of supernova 1987A are important for studying both the evolution of the ejecta and its interaction with the surrounding interstellar medium. Here we report observtions of

Dust Condensation in the Ejecta of SN 1987A

Work at ESO on the formation of dust from newly synthesized elements in the ejecta of SN 1987A began in late January when blue shifts of ≃ 600 km s-1 were found for various optical emission lines in

Infrared Emission from SN 1987A: Light Echoes or Dust Formation?

The presence of an infrared (IR) continuum in the spectrum of SN 1987A was discovered in the early stages of its evolution by various photometric and spectral observations in the 5 — 20 µm wavelength

The Chemistry of Supernova 1987A

Approximately 170,000 years ago the core of a blue supergiant star in the Large Magellanic Cloud collapsed and the star exploded, becoming a supernova. The light from the supernova reached the earth

Thermal Evolution of the Envelope of SN 1987A

We model the heating and cooling processes in the hydrogen- and helium-rich zones of the envelope of SN 1987A from t = 200 to 1200 days after outburst and use these results to calculate the light

Helium abundance and asymmetry in the wind from the precursor to supernova 1987A

TO explain why the progenitor of supernova 1987A exploded as a blue supergiant star, models of stellar evolution require that there must have been extensive mixing into the hydrogen-rich envelope of

Optical and infrared photometry of the Type IIn SN 1998S: days 11–146

We present contemporaneous optical and infrared (IR) photometric observations of the Type IIn SN 1998S covering the period between 11 and 146 d after discovery. The IR data constitute the first ever

SN 1987A: Observations of the Later Phases

The last observations (until April 1993) of SN 1987A made at ESO, La Silla, are presented. Our data show that: (i) the criterion of line shifts proves that dust is still present and is absorbing more

Modelling supernova line profile asymmetries to determine ejecta dust masses: SN 1987A from days 714 to 3604

The late time optical and near-IR line profiles of many core-collapse supernovae exhibit a red-blue asymmetry as a result of greater extinction by internal dust of radiation emitted from the receding



Discovery of an IR echo from a supernova dust cloud

Supernova (SN) 1982g in NGC1332 was discovered by Maza on 28 March 1982 at mpg=14.0 (ref. 1) some 30kpc (Ho = 50 km s−1 Mpc−1) from the nucleus of the parent galaxy (distance, 30Mpc; type, SO)2. No

The infrared echo of a type II supernova with a circumstellar dust shell: applications to SN 1979c and SN 1980k

Merrill (1980) and Telesco et al. (1981) have reported observations according to which supernovae developed a thermal infrared excess about 7-9 months after visual maximum. The two supernovae

Dust Formation Processes Around Red Giants and Supergiants

Nucleation theory, and its application to non-LTE circumstellar envelopes, is discussed. It is shown that the important temperature controlling grain formation is the vibrational temperature of small

Tabulated optical properties of graphite and silicate grains

On donne les fonctions dielectriques complexes pour le graphite et le «silicate astronomique» pour les longueurs d'onde λ comprises entre 2000 μm et 200 A, ainsi que Q abs , l'albedo et pour des

Infrared supernova light curves and asymmetric stellar mass loss

Infrared dust emission echos from Type II supernovae are a natural consequence of the heating of circumstellar dust by the supernova light. Red supergiants, the likely progenitors of most Type II