Astron. Astrophys. 346, 831-842 (1999)

⁴⁴Ti: its effective decay rate in young supernova remnants, and its abundance in Cassiopeia A

Y. Mochizuki ¹, K. Takahashi ², H.-Th. Janka ², W. Hillebrandt ² and R. Diehl <sup>3

1</sup> The Institute of Physical and Chemical Research (RIKEN), Hirosawa 2-1, Wako, Saitama 351-0198, Japan
² Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching, Germany
³ Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85740 Garching, Germany

Received 18 February 1999 / Accepted 30 March 1999

Abstract

Radioactive isotopes such as ⁴⁴Ti offer probably the most direct probe into nucleosynthesis environments in the interior of exploding stars, when the associated -ray activities in the explosion remnant are detected and translated back to the isotopic abundances at the time of the explosion. In this paper, we assert that the procedure may not necessarily be straightforward, at least in the case of ⁴⁴Ti, an orbital-electron capture decay isotope. Using the analytic model of McKee & Truelove (1995) for young supernova remnants, and assuming the existence of overdense ⁵⁶Fe-dominated clumps that contain also ⁴⁴Ti, we show that a high degree of ionization may be caused by the reverse shock so that the electron-capture rate of ⁴⁴Ti could be significantly reduced from its laboratory value. When applied to Cas A, this increases under certain conditions the current ⁴⁴Ti-activity by a factor , which yields a better compatibility between the COMPTEL observation of the 1.16 MeV line activity associated with the ⁴⁴Ti decay and the SN model predictions of the initial ⁴⁴Ti abundance. This possibility is, however, subject to various uncertainties, and in particular to the unknown properties and radial distribution of the clumps in the ejecta.

Key words: stars: supernovae: general stars: supernovae: individual: Cas A ISM: supernova remnants nuclear reactions, nucleosynthesis, abundances

Send offprint requests to: Y. Mochizuki (motizuki@postman. riken.go.jp)

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Contents

• 1. Introduction
• 2. Young supernova remnants
• 3. The model
  • 3.1. A model for young supernova remnants
  • 3.2. Thermodynamic conditions just behind the reverse shock
  • 3.3. Post reverse-shock evolution
    • 3.3.1. Ionic abundances
    • 3.3.2. Ion and electron temperatures
• 4. Results
  • 4.1. Thermodynamic evolution of post-shock clumps
  • 4.2. Effective decay rates of ⁴⁴Ti and its radioactivity as an observable
  • 4.3. ⁴⁴Ti radioactivity in Cas A
• 5. Summary
• Acknowledgements
• Appendix A: reaction rates and related uncertainties
• References

© European Southern Observatory (ESO) 1999

Online publication: June 17, 1999
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