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Distributed Radioactivities

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Astronomy with Radioactivities

Part of the book series: Lecture Notes in Physics ((LNP,volume 812))

Abstract

Radioactive isotopes are ejected into the surroundings of their sources, and become observable through their gamma-ray line emission once having left dense production sites from where not even gamma-rays may escape. Nuclear gamma-rays can penetrate material layers of integrated thickness of a few grams/cm2. A typical interstellar cloud would have ∼0.1 g/cm2, SNIa envelopes are transparent to gamma-rays after 30–100 days, depending on explosion dynamics. In this chapter, we discuss such radioactivities in interstellar space. Depending on radioactive lifetime, we thus address isotopes which originate from single sources (the short-lived isotopes) or up to thousands of sources as accumulated in interstellar space over the radioactive lifetime of long-lived isotopes (see Table 7.1).

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Notes

  1. 1.

    The NuSTAR mission planned for 2012 is equipped with such imaging capability up to 80 keV.

  2. 2.

    Notice that the distinction between a point and a diffuse source depends also on the resolving power of the observing instrument, i.e. diffuse emission is seen if typical distances – projected on the sky – between point sources are larger than the instrument’s resolution. But even detectors with good spatial resolution would see diffuse emission if the emitting particles/nuclei travel far away from their sources during their lifetimes; this may be the case of Galactic positrons (see Sect. 7.7).

  3. 3.

    Stars are born with a mass distribution called Initial mass function (IMF). Observed IMFs of young stellar clusters in the Milky Way and other galaxies have similar IMFs, with the upper part (\(M>1 \mathrm{M}_{\odot}\)) described by a power-law (\(dN/dM \propto M^{-(1+X)}\!,\) where X is the slope of the IMF; in most cases, \(X=1.35\) (as determined by Salpeter (1955), for the local IMF.

  4. 4.

    In active galaxies the central supermassive black hole also plays a role, and even dominates over the impact from massive stars for central regions, and for entire galaxies in late (largely-processed) evolution such as at low redshifts.

  5. 5.

    In this book we only address the scales and processes within a galaxy, as it is driven by massive stars and can be traced by radioactive material; in this and further Sections of this Chapter, the broader (cosmic evolution) context is also relevant.

  6. 6.

    AGB stars form colorful planetary nebulae, massive-star winds form gas structures within the HII-regions created by the ionizing radiation of the same stars, and thus a similarly-rich variety of colorful filamentary structure from atomic recombination lines results. Supernova remnants are the more violent version of the same processes.

  7. 7.

    Feedback from supermassive black holes is small by comparison, but may become significant in AGN phases of galaxies and on the next-larger scale (clusters of galaxies, see (e)). Galaxy interactions and merging events are also important agents over cosmic times, their overall significance for cosmic evolution is a subject of many current studies.

  8. 8.

    Young stars which have been created rather recently in the cosmic history are called Population I. They are the only stellar population which contains massive (hence short-lived) stars observable today.

  9. 9.

    See also Appendix A for a specific and useful standard description by Clayton (1985, 1988).

  10. 10.

    The mass range commonly assumed is 8–120 M⊙; but both mass limits are subject to some uncertainty (see discussion in Zinnecker and Yorke, 2007). Limongi and Chieffi (2006) discuss in detail the impact of varying the slope of the mass distribution function, and the upper mass limit for the integrated range of masses.

  11. 11.

    A period of irritation occurred between 2002 and 2005, as nuclear cross sections and models were updated, and seemed to predict much higher ratios up to 1; see discussion in Woosley and Heger (2007) and Prantzos (2004).

  12. 12.

    Instrumental background from 60Co produced locally in the satellite by cosmic rays may be a remaining concern. Wang et al. (2007) have accounted for such contribution within instrumental knowledge. Note that insufficient subtraction of instrumental contributions would make the Galactic 60Fe contribution even smaller.

  13. 13.

    Only long GRBs are attributed to such collapsars. GRBs have been seen up to redshifts 8 and are thus the most-distant objects seen; understanding their nature will help to understand formation of stars at or before the epochs where galaxies formed.

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  1. Max Planck Institut für extraterrestrische Physik, 85748, Garching, Germany

    R. Diehl

  2. Clemson University, Clemson, SC, 29634-0978, USA

    D.H. Hartmann

  3. Institut d’Astrophysique, 75104, Paris, France

    N. Prantzos

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  1. MPI für extraterrestrische Physik, Giessenbachstr. 1, Garching, 85740, Germany

    Roland Diehl

  2. Dept. Physics & Astronomy, Clemson University, Clemson, 29634, South Carolina, USA

    Dieter H. Hartmann

  3. Institut d'Astrophysique de Paris, Boulevard Arago 98bis, Paris, 75014, France

    Nikos Prantzos

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Diehl, R., Hartmann, D., Prantzos, N. (2011). Distributed Radioactivities. In: Diehl, R., Hartmann, D., Prantzos, N. (eds) Astronomy with Radioactivities. Lecture Notes in Physics, vol 812. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-12698-7_7

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