Journal of Physical Studies 22(2), Article 2901 [8 pages] (2018) DOI: https://doi.org/10.30970/jps.22.2901 GAS AND DUST EMMISION IN COLD ENVIRONMENTS WITH ENHANCED CONTENT OF RADIOACTIVE 2244Ti ISOTOPE D. M. Doikov1, S. M. Andrievsky2, A. V. Yushchenko3 1Odesa National Maritime University, Department of Mathematics, Physics and Astronomy, 34, Mechnikov St., Odesa, UA-65029, Ukraine 2Department of Astronomy and Astronomical Observatory, Odesa National University, 1v, Marazliyivska St., Odesa, UA-65014, Ukraine 3Astrocamp Contents Research Institute, Goyang, 10329, Republic of Korea

The spectroscopy of cold gas-dust envelopes of supernovae is the subject of this article. To define the quantitative characteristics of the matter in these envelopes, a possibility of additional sources of energy is discussed -- in particular, the intense, diffusely distributed flows of high-energy positrons formed by the recently discovered chain of radioactive decays: ${}_{22}^{44}{\rm Ti}\xrightarrow{85\,{\rm y}}{}_{21}^{44}{\rm Sc}\xrightarrow{6\,{\rm h}}{}_{20}^{44}{\rm Ca}$. The quantitative characteristics of radiation distribution function $S(E,r)$ and electron distribution function $F(E,r)$ are obtained for certain rarefied layers of the supernova remnant SN1987A. An additional feature of the kinetic ensemble of the envelope's gas with the mentioned radioactive decay is the presence of the recoil nuclei of the final elements of this decay's chain. In the case under consideration, these are the nuclei of ${}_{20}^{44}{\rm Ca}$II. The paper notes that the motion of recoil nuclei in a rarefied supernova gas at a sufficiently high kinetic energy accumulated by radioactive decay determines that the recoil nuclei exist only in an ionized state, and the remaining nuclei, after hydrogen recombination, -- in a neutral state. In the discussed case, ${}_{20}^{44}{\rm Ca}$II can be observed only in an ionized state, and ${}_{20}^{44}{\rm Ca}$II -- only in a neutral state. This remark can be applied to the recoil nuclei of other elements formed at earlier times during the hydrogen recombination. It is shown that this method is suitable for isotopic separation of the final elements of radioactive decay chains occurring in young supernova envelopes. The presence of a nonthermal component in the obtained distributions of $S(E,r)$ and $F(E,r)$ causes an additional IR emission of the dust formed during the expansion of a supernova envelope in the modern epoch of observations. The presence of spectral lines at the moment of the Hubble telescope observation allowed us to conclude that the existence of the numerous observed spectral lines in the optical, UV, and near-infrared regions of the spectrum requires the presence of the astronomical silicates with extensive passbands extending over these spectral intervals in the observed dust shells. The presence of graphite dust in these bunches excludes the existence of the observed optical component of the spectrum and requires its presence in separate shell structures enriched with C-N-O elements. However, in this case, the presence of decaying ${}_{22}^{44}{\rm Ti}$II isotopes which form the fast positrons is unlikely. The graphite particles, as well as H$_2$ molecules, are influenced by positrons only when the density of the shell allows them to reach its outer layers. In this case, the number of collisions with atoms should not exceed several thousands. It is necessary to decelerate them before the complete annihilation with atomic electrons of the shell's atoms and molecules.

PACS number(s): 98.58.-w, 98.58.Mj, 95.30.Dr

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