Impact of Space Radiation in the Earth s Atmosphere

American-Eurasian J. Agric. & Environ. Sci., 16 (5): 868-873, 2016 ISSN 1818-6769 IDOSI Publications, 2016 DOI: 10.5829/idosi.aejaes.2016.16.5.10440 Impact of Space Radiation in the Earth s Atmosphere A.E. Umahi Department of Industrial physics (Astrophysics unit), Faculty of Science, Ebonyi State University, Abakaliki, Nigeria Abstract: A review of the impact of space radiation in the Earth s atmospheric is presented in this work. The data for GCRs and GSRs were collected per day from observatories and placed in Microsoft excel spread sheet for statistical study. In the excel graph sheet, the data were treated with a threshold value. The results of the characterization of the major two events (i.e. GCRs and GSRs) against time (measured in hours) showed significant variations. The anti-correlation coefficient, r between GCRs and GSRs, ranging from -0.001 to -0.350, also shows that the events originates from different sources. The low level of r in this result indicates that other solar activities such as sunspot, coronal mass ejection, solar wind and directly enters the Earth s atmosphere. Key words: Solar Flare Ionization and Solar Activity INTRODUCTION atmosphere is absorbed. The most dangerous emissions from these radiations are protons, x- Rays and ultraviolent The impact of space radiation on astronauts, human radiations (UV). In the light of these, they continuous DNA and cells cannot be over emphasized. The research study of the Earth s mechanism and ionization remains will help in understanding the risk of space radiation as unlimited for astronomers, astrophysics and space well as to develop the methods or advice to migrate this scientist globally [1]. risk on space exploration. The major sources of space However, some authors stated that space radiation radiation are particles trapped in the earth s magnetic penetrates the atmosphere and ionization occurs at below field, sporadic particles release into space during solar ~60km [2, 3]. They also produce nuclear-electromagnetic flares, which are high energy protons within our solar cascade [4]. The effects of space radiation in the Earth s system and galactic cosmic rays, which are high energy atmosphere are globally discussed [5, 6]. The combination proton and heavy ions originating outside our solar of high galactic cosmic rays and solar rays (such as solar system. Space radiation is different from radiations flare) are used in this work. This paper will focus on the experience at earth surface such as x-rays or gamma rays. statistical review of space radiation in the Earth s This radiation comprises of atoms in which electrons have atmosphere as it mainly influences ionization and produce being stripped away as the atom accelerated in interstellar nuclear-electromagnetic cascade. space to speed reaching the speed of light. Eventually, The investigation of impact of cosmic rays and only the nucleus of the atom remains. The contribution solar energetic particles on the Earth s environment of these radiations is to generate ionizing radiation. were reported important, not only for the This ionizing radiation has so much energy that it can ionospheric process but also for the scientific, eject electrons out of any atom it strikes, which means technological and even biological system [7]. The ions ionizing the atom. This effect can destroy the atom in accelerated to several 10-100 MeV are very important for human cells leading to further human problem such as the radiation hazard effect during solar radiation storm cataracts, cancer and damaging the central navels system. with electronic elements failure on satellite, spacecraft and Space radiations also have very different effect on human airplanes, long distance communication and biological DNA. This is mainly due to the increase in ionization that consequences [8]. The energy deposition in materials takes place in the earth s atmosphere. The energy that causes permanent damage in silicon semiconductor ionizing radiation loses as it travels through the devices [9]. Corresponding Author: A.E. Umahi, Department of Industrial physics (Astrophysics unit), Faculty of Science, Ebonyi State University, Abakaliki, Nigeria. 868

Galactic Cosmic Rays: Galactic Cosmic Rays (GCRs) are was on September 1, 1859. Two scientists, Richard C. high energetic charged particles originated from galaxies Carrington and Richard Hodgson, were independently outside our solar system and interplanetary space [10]. observing sunspot when they viewed a large flare in white The GCRs that enters the Earth s atmosphere are light. The compositions of solar flare are protons, electron classified as primary cosmic rays [11]. The major and heavy nuclei. When they penetrate the Earth s dominated composition of these primary cosmic rays is atmosphere, they can cause ionization and expand the proton (~ 10%) while the minor composition are electrons Earth s upper atmosphere. Solar flares occur at solar (~1%). The scientific communities are interested in the minimum and at solar maximum every day. The number of effects of ionization and nuclear-electromagnetic cascade solar flare in the Earth s atmosphere increases with due to space radiation on the Earth s atmosphere. decreasing intensity to the limit of the sensitivity of Balloons [12-14], Rockets [15] and Spacecraft s [16], the instrument that has been used to detect them. are initially used in observing the ionization rates and The statistics of flares that were detected from 1980-1989 level in the Earth s atmosphere at different latitude. with the Hard x- rays Burst Spectrometer on the Solar Currently numerous ground base observatory Maximum Mission show that flares occurred at an average centers/networks and teams of astrophysics have been rate of ~1 per day at solar minimum. At solar maximum, the empowered to observe and measure the atmospheric average rate was as high as 20 per day (average over a 6 mechanism and ionization process [17]. months interval). So the rate at solar maximum is roughly The ionization due to galactic cosmic rays (GCRs) is a factor of 10> solar minimum. It is important to realize, always present in the atmosphere and it changes with the however, that the solar rate is very irregular. They can be 11-year solar cycle due to the solar modulation. Primary long period of time at solar minimum when no detectable cosmic rays initiate a nucleonic-electromagnetic cascade flare occur. Then, a large active region can form and in the atmosphere, with the main energy losses at produce many flares in just a few days [18]. altitudes below 30 km resulting in ionization, dissociation and excitation of molecules [18]. Atmospheric Mechanism and Ionization: The basic In addition, the impact of cosmic rays on the ozone mechanism which atmospheric ion formation by galactic layer and formation of clouds in the troposphere becomes cosmic rays (GCRs) could affect Earth s climate leading to a new interested area for study. It is important to know the growth of cloud condensation nuclei [21, 22] and the precisely that the cosmic ray induced ionization (CRII) removal of charged droplets from cloud [23]. They also and its variations with the location, time, solar and GCRs initiate nuclear-electromagnetic cascades involving geomagnetic activity. They also affect the ozone creation electrons, x-rays, mesons and nucleons with energies and depletion which the chemical process in the Earth s 9 more than 10 MeV in the atmosphere, with the main stratosphere [19]. energy losses, resulting in ionization, dissociation and excitation of molecules [24]. GCRs are always present in Galactic Solar Radiation: In the same way, sporadic solar the vicinity of the Earth s atmosphere and are subjected flare particles have been reported to have a direct effect to Galactic solar rays (GSRs) modulation [25]. In contrary, on the Earth s atmosphere [20]. The intensity of the solar GSRs does not produce nuclear-electromagnetic cascades flare radiation does travel in 8 10minutes interval to the in the Earth s atmosphere as stated in the roles of GCRs. Earth s surface. They are the most sudden, rapid, intense Various methods have been applied to interpret these variation in brightness and energetic explosions in the observations and measurements of ionization and nuclearsolar system. A solar flare occurs when magnetic energy electromagnetic cascades in the Earth s atmosphere. 27 32 ranging from 10 ergs/s to 10 erg/s that has built up in These methods are as follows: the empirical profiles of the the solar atmosphere is suddenly released from the corona ionization effects until 100 km, the quantitative model of of the sun. The radiation is emitted virtually across the the atmospheric ionization [27-29], the analytical entire electromagnetic spectrum from radio wave (at long approximation model of the cosmic ray ionization losses wavelength end) through optical emission to x-rays and [27, 29], the Monte Carlo CORSIKA (COsmic Ray gamma-rays (at the short wavelength end). The amount of Simulations for Kascade) for modeling the energy released is the equivalent of millions of hundred atmospheric nucleonic-electromagnetic cascade, megaton hydrogen bombs exploding at the same time. ionization and electrical parameters in the planetary The first solar flare recorded in astronomical literatures atmosphere [7, 30-32]. 869

Fig. 1: Galactic Cosmic Rays (GCRs) and Galactic Solar Rays (GSRs) Variations against Time/day in the months of January, February and March. Fig. 2: Galactic Cosmic Rays (GCRs) and Galactic Solar Rays (GSRs) Variations against Time/day in the months of April, May and June. Fig. 3: Galactic Cosmic Rays (GCRs) and Galactic Solar Rays (GSRs) Variations against Time/day in the months of July, August and September. Further, convincing works of COST-724 action 4 code for the cascade evolution in the atmosphere, (2003 2007) gave their interpretation as follows: the simulating the interactions and decays of various nuclei, numerical GCRs ionization models [33], Sofia model of hadrons, muons, electrons and photons. analytical approximation of the direct ionization [34, 35], CORSIKA Monte-Carlo package extended by FLUKA Data and Result Analysis: The data for GCRs and package to simulate the low-energy nuclear interactions GSRs were from Solar Soft Data Centre (SSDC) and [36 and 37], Oulu CRAC (Cosmic Ray Atmospheric Space Physics Interactive Data Resources (SPIDR). Cascade) model for direct ionization of GCR particles The measurements were grouped in three months interval [38, 39], Bern model (ATMOCOSMICS/ covering 12- month s events in 2007. The variations in PLANETOCOSMICS code) using the GEANT-4 Monte- each of the groups are shown in a graphical form in Carlo simulation package [40, 41], CORSIKA and GEANT- Figs. 1 to 4. In addition, a correlation analysis using excel 870

Fig. 4: Galactic Cosmic Rays (GCRs) and Galactic Solar Rays (GSRs) Variations against Time/day in the months of October, November and December. program were carried out in order to ascertain the level of 3. Tinsley, B.A. and L. Zhou, 2006. Initial results of a relationship between GCRs and GSRs. The results of the global circuit model with stratospheric and level of correlation coefficient, r, ranges from -0.001 to - tropospheric aerosols, J. Geophys. Res., 111: D16205. 0.350. 4. Dorman, L.I., 2004. Cosmic Rays in the Earth s Atmosphere and Underground, Kluwer Academic DISCUSSION Publishers, Dordrecht. 5. Tinsley, B.A. and R.A. Heelis, 1993. Correlations of The results of the statistical study of the two atmospheric dynamics with solar activity: evidence events (i.e. GCRs and GSRs) significant variations. for a connection via the solar wind, atmospheric This variations are in agreement with some authors [7, 33]. electricity and cloud microphysics, J. Geophys. Res., In the result no GCRs detection was observed in some 98: 10375-10384. months. On the other side of the events, solar flare 6. Tonev, P.T. and P.I.Y. Velinov, 2011. Model showed high significant variations in all the months study of the influence of solar wind parameters The correlation coefficients, r between GCRs and GSRs on electric currents and fields in middle are anti-correlation, ranging from -0.001 to -0.350. The anti- atmosphere at high latitudes, C.R. Acad. Bulg. Sci., correlation coefficient is in agreement with other authors 64(12): 1733-1742. [7, 33, 42]. 7. Velinov, P.I.Y., S. Asenovski, K. Kudela, In conclusions, the observatory stations exploring J. Lastovicka, L. Mateev, A. Mishev and P. Tonev, the earth s atmosphere records measurements of GCRs 2013. Impact of Cosmic Rays and Solar Energetic and GSRs on daily events. The interpretation of these Particles on the Earth s Ionosphere and Atmosphere, measurements is being investigated. The graphical J. Space Weatherspace Clim., 3(A14): 1-17. analysis showed that they are presents and variations of 8. Kudela, K., M. Storini, M.Y. Hofer and A. Belvo, GCRs and GSRs in the earth s atmosphere. The anti- 2000. Cosmic rays in relation to space weather, Space correlation coefficient result shows that the events Sci.Rev., 93(1-2): 153-174. originate from different sources [42]. 9. Kudela, K., H. Mavromichalaki, A. Papaioannou and M. Geronti-dou, 2010. On Mid-term periodicities in REFERENCES Cosmic rays, sol. Phys., 266: 173-180. 10. Shikaze, Y., S. Haino, K. Abe, H. Fuke and T. Hams, 1. Umahi, A.E., 2016a. Effects of Cosmic Rays and Solar 2007, Measurements of 0.2-20 GeV/n cosmic-ray Flare Variations in Earth s Atmospheric Mechanism proton and helium spectra from 1997 through 2002 and Ionization. Middle East Journal of Scientific with the BESS spectrometer, Astropart. Phys., Research (imprint). 28: 154. 2. Velinov, P., H. Ruder and L. Mateev, XXXX. Method 11. Seo, E.S., J.F. Ormes, R.E. Streitmatter, S.J. Stochaj for calculation of ionization profiles caused by and W.V. Jones, 1991. Measurement of cosmic-ray cosmic rays in giant planet ionospheres from jovian proton and helium spectra during the 1987 solar group, Adv. Space Res., 33: 232-239. minimum, Astrophys. J., 371: 763. 871

12. Bazilevskaya, G.A., 2000. Observations of Variability 27. O Brien, K., 1971. Cosmic Ray Propagation in the in Cosmic Rays, Space Sci. Rev., 94: 25-38. 13. Neher, H.V., 1971. Cosmic rays at high latitude and altitudes covering four solar maxima, J. Geophys. Res., 76: 1637-1651. 14. Lowder, W.M., P.D. Raft and H.L. Beck, 1972. Experimental determination of cosmic-ray charged particle intensity profiles in the atmosphere, in: Procs. National Symp. on Natural and Manmade Radiation in Space (Eds. E.A. Warman), Las Vegas, 1971, NASA, 908-913. 15. Burger, R.A., M.S. Potgieter and B. Heber., 2000. Rigidity dependence of cosmic ray proton latitudinal gradients measured by the Ulysses spacecraft: implications for the diffusion tensor, J. Geophys. Res., 105: 27447. 16. Shea, M.A. and D.F. Smart, 1996. Overview of the effects of solar-terrestrial phenomena on man and his environment. Nuovo Climento 19c(6): 945-952. 17. Simpson J.A., 2000. The cosmic Ray nucleonic component; the invention and scientific uses of the neutron monitor, space sci. Rev., 93: 11-32. 18. Dorman, L.I. and T.M. Krupitsakaya, 1975. Calcalution of Expected ratio of Solar Cosmic Ray ion generation speeds on different altitudes, in Cosmic Rays Nauka, Moscow, 15: 30-33. 19. Brasseur, G. and S. Solomon, 2005. Aeronomy of the Middle Atmosphere, Springer, Dordrecht. 20. Rosen, J.M., D.J. Hofmann and W. Gringel, 1985. Measurements of ion mobility to 30 km, J. Geophys. Res., 90(D4): 5876-5884. 21. Harrison, R.G. and K.S. Carlaw, 2003. Ion- aerosol- Cloud Process in the low atmosphere, Rev. Geophys. 41(3): 1012. 22. Yu, F. and R.P. Turco, 2001. From Molecular Clusters to nanoparticles; The role of ambient ionization in tropospheric areroseol formation, J. Geophy. Res., 106: 4797-4814. 23. Tripathi, S.N. and R.G. Harrison, 2002. Enhancement of contact nucleation by scavenging of charged aerosol, Atoms. Res., 62: 57-70. 24. Usoskin, I., K. Alanko-Huotari, G. Kovaltsov and K. Mursula, 2005. Heliospheric modulation of cosmic rays: Monthly Reconstruction for 1951-2004, J. Geophys. Res., 110(A12), CiteID: A12108. 25. Kudela, K., 2009. On energetic particles in space, Acta Phys. Slovaca, 59: 537-652. 26. Velinov, P.I.Y., 1966. An expression for ionospheric electron production rate by cosmic rays, C.R. Acad. Bulg. Sci., 19(2): 109-112. Atmosphere, J. Nuovo Climento A, 3(4): 521-547. 28. Dorman, L.I. and I.D. Kozin, 1983. Cosmic Radiation in the Upper Atmosphere, Fizmatgiz, Moscow. 29. Velinov, P.I.Y., 1970. Solar cosmic ray ionization in the low ionosphere, J. Atmos. Terr. Phys., 32: 139-147. 30. Heck, D., J. Knapp, J.N. Capdevielle, G. Schatz and T. Thouw, 1998. CORSIKA: A Monte Carlo Code to Simulate Extensive Air Showers, Forschungszentrum Karlsruhe Report FZKA, pp: 6019. 31. Vainio, R., L. Desorgher, D. Heynderickx, M. Storini and E. Flu ckiger, 2009. Dynamics of the Earth s particle radiation environment, Space Sci. Rev., 147: 187-231. 32. Singh, A.K., D. Singh and R.P. Singh, 2011. Impact of galactic cosmic rays on Earth s atmosphere and human health, Atmos. Environ., 45: 3806-3818. 33. Usoskin, I., L. Desorgher, P.I.Y. Velinov, M. Storini, E. Flueckiger, R. Buetikofer and G.A. Kovalstov, 2009. Solar and galactic cosmic rays in the Earth s atmosphere, Acta Geophys., 57(1): 88-101. 34. Velinov, P.I.Y., L. Mateev and H. Ruder, 2008. Generalized model of ionization profiles due to cosmic ray particles with charge Z in planetary ionospheres and atmospheres with 5 energy interval approximation of the ionization losses function, C.R. Acad. Bulg.Sci., 61(1): 133-146. 35. Buchvarova, M. and P.I.Y. Velinov, 2005. Modeling spectra of cosmic rays influencing on the ionospheres of earth and outer planets during solar maximum and minimum, J. Adv. Space Res., 36(11): 2127-2133. 36. Usoskin, I.G., G.A. Kovaltsov, I.A. Mironova, A.J. Tylka and W.F. Dietrich, 2001. Ionization effect of soalr Particle GLE events in low and Middle Atmosphere,Atmos Chem. Phy., 11: 1979-1988. 37. Mishev, A. and P.I.Y. Velinov, 2007. Atmosphere ionization due to cosmic ray protons estimated with CORSIKA code simulations, C.R. Acad. Bulg. Sci., 60(3): 225-230. 38. Usoskin, I., L. Desorgher, P.I.Y. Velinov, M. Storini, E. Flueckiger, R. Buetikofer and G.A. Kovalstov, 2008. In Solar and Galactic Cosmic Rays in the Earth s Atmosphere. Developing the Scientific Basis for Monitoring, Modeling and Predicting Space Weather, edited by Lilensten, J., COST 724 Final Report, COST Office, Brussels, 127-135. 872

39. Usoskin, I. and G. Kovaltsov, 2006. Cosmic ray 41. Desorgher, L., E. Fluckiger, M. Gurtner, M.R. Moser, induced ionization in the atmosphere: full R. and Bu tikofer 2005. Atmocosmics: a GEANT4 modeling and practical applications, J. Geophys. Res., code for computing the interaction of cosmic rays 111: D21206. with the Earths atmosphere, Int. J. Mod. Phys., A 40. Agostinelli, S., J. Allison, K. Amako, J. Apostolakis 20(29): 6802-6804. and H. Araujo, 2003. GEANT 4 - a simulation toolkit, 42. Umahi, A.E., 2016b. Impact of High Energy Charged Nucl. Instrum. Methods Phys. Res., A: Accelerators, Galactic Particle Variations in the Earth Atmosphere. Spectrometers, Detectors and Associated Equipment, Middle East Journal of Scientific Research (imprint). 506(3): 250-303. 873