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Issue A&A
Volume 374, Number 2, August I 2001
Page(s) 629 - 637
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20010725



A&A 374, 629-637 (2001)
DOI: 10.1051/0004-6361:20010725

ISO/SWS observations of SN 1987A

II. A refined upper limit on the mass of $^\mathsf{44}$Ti in the ejecta of SN 1987A
P. Lundqvist1, C. Kozma1, J. Sollerman1, 2 and C. Fransson1

1  Stockholm Observatory, 133 36 Saltsjöbaden, Sweden
2  European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany

(Received 2 March 2001 / Accepted 17 May 2001)

Abstract
ISO/SWS observations of SN 1987A on day 3425 show no emission in [Fe I] 24.05 $\mu{\rm m}$ and [Fe II] 25.99 $\mu{\rm m}$ down to the limits ~0.39 Jy and ~0.64 Jy, respectively. Assuming a homogeneous distribution of 44Ti inside $2000 \rm km s^{-1}$ and negligible dust cooling, we have made time dependent theoretical models to estimate an upper limit on the mass of ejected 44Ti. Assessing various uncertainties of the model, and checking the late optical emission it predicts, we obtain an upper limit of $\simeq$ $1.1\times 10^{-4} {M}_\odot$. This is lower than in our previous estimate using other ISO data, and we compare our new result with other models for the late emission, as well as with expected yields from explosion models. We also show that steady-state models for the optical emission are likely to overestimate the mass of ejected 44Ti. The low limit we find for the mass of ejected 44Ti could be higher if dust cooling is important. A direct check on this is provided by the gamma-ray emission at 1.157 Mev as a result of the radioactive decay of 44Ti.


Key words: supernova: individual: SN 1987A -- nucleosynthesis -- supernovae: general

Offprint request: P. Lundqvist, peter@astro.su.se

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