Advertisement

Pramana

, Volume 20, Issue 4, pp 287–292 | Cite as

A search for superheavy nuclei tracks in extraterrestrial olivine crystals

  • J S Yadav
  • A P Sharma
  • G N Flerov
  • V O Perelygin
  • S G Stetsenko
  • P Pellas
  • C Perron
  • R Antanasijevich
  • B Jakupi
  • Y Todorovich
Nuclear Physics

Abstract

A study is made for the search of superheavy nuclei in Marjalahti, Eagle Station and in other pallasite olivines. The olivine crystals are calibrated for heavy ion track lengths by using heavy ion beams from cyclotrons. The calibration for ultra heavy ions which are presently not available with sufficient energy to produce volume tracks in olivine crystals, is based on Katz and Kobetich model of track formation. The length spectrum of volume tracks, revealed by puncturing them with focussed Nd-glass laser beam, is measured and the abundances of different nuclei groups are calculated. Partial annealing has been used at 430°C for 32 hr which eliminates the interfering tracks due to nuclei of atomic numberS ≤ 50. During the scanning 4 cm3 olivine crystals, about 360 long tracks of uranium group as well as two very long tracks have been found. If these tracks belong to superheavy nuclei, the relative abundance of super heavies is found to be 6 × 10−11 in galactic cosmic rays.

Keywords

Meteorites volume tracks galactic cosmic rays superheavy nuclei 

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

References

  1. Cameron A G W 1973Space Sci. Rev. 15 201CrossRefADSGoogle Scholar
  2. Dolivo-Dobrovolskaya G I, Kalamensky V D, Gavrilova N N, Perelygin V P and Stetsenko S G 1976Geokhimiya 10 1476Google Scholar
  3. Fowler P H, Adams R A, Cowen V G and Kidd J M 1970Proc. R. Soc. 301 35Google Scholar
  4. Fowler P H, Alexandre C, and Clapham V M 1977Proc. 15th Int. Cosmic Ray Conf. Plovdiv 11 165Google Scholar
  5. Kapuscik A, Preelygin V P, Tretiakova S P and Shadieva N H 1966Proc. 6th Int. Conf. on Corpuscular Phot., Florence CEP, Roma 458Google Scholar
  6. Katz R and Kobetich E I 1968Phys. Rev. 170 402ADSGoogle Scholar
  7. Lhagvasuren D, Otgonsuren O, Perelygin V P, Stetsenko S G, Pellas P and Perron C 1980a Reprint from Solid State Nuclear Track Detectors 997Google Scholar
  8. Lhagvasuren D, Perelygin V P, Stetsenko S G and Murtazaev K H 1980b Reprint fromSSNTD 929Google Scholar
  9. Maurette M, Pallas P and Walker R M 1964Nature (London),204 821CrossRefADSGoogle Scholar
  10. Meyer J P 1979Proc. 16th Int. Cosmic Ray Conf. Kyoto 1 374ADSGoogle Scholar
  11. Otgonsuren O, Perelygin V P, Stetsenko S G, Gavrilova N N, Fieni C and Pellas P 1976Astrophys. J. 210 258CrossRefADSGoogle Scholar
  12. Perelygin V P, Stetsenko S G, Pellas P, Lhagvasuren D, Otgonsuren O and Jakupi B 1977Nucl. Track Detection 1 199CrossRefGoogle Scholar
  13. Shirk E K and Price P B 1978Astrophys. J. 220 719CrossRefADSGoogle Scholar
  14. Yadav J S 1982Study of charged particle tracks in SSNTD s Ph.D. thesis, Kurukshetra University, India.Google Scholar

Copyright information

© Indian Academy of Sciences 1983

Authors and Affiliations

  • J S Yadav
    • 1
  • A P Sharma
    • 1
    • 2
  • G N Flerov
    • 1
    • 3
  • V O Perelygin
    • 1
    • 3
  • S G Stetsenko
    • 1
    • 3
  • P Pellas
    • 1
    • 4
  • C Perron
    • 1
    • 4
  • R Antanasijevich
    • 1
    • 5
  • B Jakupi
    • 1
    • 5
  • Y Todorovich
    • 1
    • 5
  1. 1.Tata Institute of Fundamental ResearchBombayIndia
  2. 2.Physics DepartmentKurukshetra UniversityKurukshetraIndia
  3. 3.Joint Institute for Nuclear Research, DubnaMoscowUSSR
  4. 4.Laboratorie de Mineralogie du CNRS Rue Buffon 61ParisFrance
  5. 5.Institute of PhysicsBelgradeYugoslavia

Personalised recommendations