Computer Science
Scientific paper
Aug 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jena.confe..38i&link_type=abstract
"JENAM-2007, "Our non-stable Universe", held 20-25 August 2007 in Yerevan, Armenia. Abstract book, p. 38-38"
Computer Science
Scientific paper
It is known that radioactive 44Ti is mostly produced in supernovae explosions and is a primary isotope in the radioactive decay chain of 44Ti-44Sc-44Ca. Here we present a critical review of the amount of radioactive 44Ti produced by the core-collapse supernovae (SNe) that have given birth to the Cas A and RX J0852.0-4622/GRO J0852-4642 supernova remnants (SNRs) [1]. The 1.157 MeV line detections by COMPTEL [2,3,4] and the following from those detections the 44Ti mass estimates, derived with the use of the 1.157 MeV line flux, are compared to the mass estimates based on the measurements of Beppo-SAX PDS [5] and IBIS (ISGRI) [6] of the 44Sc line intensities at ~68 and ~78 keV, for Cas A. The non-detection of 44Sc lines from RX J0852.0-4622/GRO J0852-4642 by IBIS (ISGRI) and SPI instruments of INTEGRAL is confronted with the COMPTEL detection of the 44Ti (44Ca) line flux, as well as with the derived by COMPTEL shape of the 1.157 MeV line. Most recent results on the expansion velocity of the high-velocity debris of Cas A SNR [7], and XMM-Newton results on the expansion velocity of RX J0852.0-4622/GRO J0852-4642 [8] are compared to the COMPTEL derived expansion velocities of both SNRs, and are used to evaluate possible consequences of the heavy ions interaction with the ambient and/or SNR shell matter and the contribution of such interactions to the 44Ca line shape and intensity. The X-ray and optical observations that can be, and were used to derive an amount of 44Ti produced in SNRs are described and discussed. Undisputable advantages of using multiwavelength observations to derive 44Ti mass in SNR are confronted with the critical restrictions of the appropriate observations. Difficulties of such measurements for point-like and extended sources are evaluated for each of the potential wavelength range available at present or in future experiments. The derived quantities of 44Ti and of 44Sc are compared with the latest nucleosynthesis theory predictions. The new estimates of the 44Ti masses that were derived with the use of the above analysis for two SNRs, as well as the dynamical properties of remnants are used to constrain SN explosion models [9,10].
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