1、BRITISH STANDARD AEROSPACE SERIES BS ISO 15390:2004 Space environment (natural and artificial) Galactic cosmic ray model ICS 49.140 BS ISO 15390:2004 This British Standard was published under the authority of the Standards Policy and Strategy Committee on 8 September 2004 BSI 8 September 2004 ISBN 0
2、 580 44387 6 National foreword This British Standard reproduces verbatim ISO 15390:2004 and implements it as the UK national standard. The UK participation in its preparation was entrusted by Technical Committee ACE/68, Space systems and operations, to Subcommittee ACE/68/-/4, Space environment (nat
3、ural and artificial), which has the responsibility to: A list of organizations represented on this subcommittee can be obtained on request to its secretary. Cross-references The British Standards which implement international publications referred to in this document may be found in the BSI Catalogu
4、e under the section entitled “International Standards Correspondence Index”, or by using the “Search” facility of the BSI Electronic Catalogue or of British Standards Online. This publication does not purport to include all the necessary provisions of a contract. Users are responsible for its correc
5、t application. Compliance with a British Standard does not of itself confer immunity from legal obligations. aid enquirers to understand the text; present to the responsible international/European committee any enquiries on the interpretation, or proposals for change, and keep the UK interests infor
6、med; monitor related international and European developments and promulgate them in the UK. Summary of pages This document comprises a front cover, an inside front cover, the ISO title page, pages ii and iii, a blank page, pages 1 to 6, an inside back cover and a back cover. The BSI copyright notice
7、 displayed in this document indicates when the document was last issued. Amendments issued since publication Amd. No. Date Comments Reference number ISO 15390:2004(E)INTERNATIONAL ADNATSDR ISO 10935 tide tsriFino 4002-0610- Space environment (natural and artificial) Galactic cosmic ray model Environ
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12、lsaee inform ttneC ehlar Secrteiraat ta the serddaig sleb nevwo. ii BSISO15390:2004 iiiForeword ISO (the International Organization for Standardization) is a worldwide federation of national standards bodies (ISO member bodies). The work of preparing International Standards is normally carried out t
13、hrough ISO technical committees. Each member body interested in a subject for which a technical committee has been established has the right to be represented on that committee. International organizations, governmental and non-governmental, in liaison with ISO, also take part in the work. ISO colla
14、borates closely with the International Electrotechnical Commission (IEC) on all matters of electrotechnical standardization. International Standards are drafted in accordance with the rules given in the ISO/IEC Directives, Part 2. The main task of technical committees is to prepare International Sta
15、ndards. Draft International Standards adopted by the technical committees are circulated to the member bodies for voting. Publication as an International Standard requires approval by at least 75 % of the member bodies casting a vote. Attention is drawn to the possibility that some of the elements o
16、f this document may be the subject of patent rights. ISO shall not be held responsible for identifying any or all such patent rights. ISO 15390 was prepared by Technical Committee ISO/TC 20, Aircraft and space vehicles, Subcommittee SC 14, Space systems and operations. BSISO15390:2004BSISO15390:2004
17、INTENRATIONAL TSANDADR IS:09351 O4002(E)1Space environment (natural and artificial) Galactic cosmic ray model 1 Scope This International Standard specifies a model for estimating the radiation impact of galactic cosmic rays (GCR) on hardware and on biological and other objects when in space. This In
18、ternational Standard can also be used in scientific research to generalize the available experimental evidence for GCR fluxes. This International Standard establishes the model parameters and characteristics of variations in the 10 1MeV to 10 5MeV GCR particles (electrons, protons, and Z = 2 to 92 n
19、uclei in the near-Earth space beyond the Earths magnetosphere). 2 Terms and definitions For the purposes of this document, the following terms and definitions apply. 2.1 galactic cosmic rays GCR high-energy charged particle fluxes penetrating the heliosphere from local interstellar space 2.2 Wolf nu
20、mber W W = 10g +f where g is sunspot group number; f is the total sunspot number on the suns visible disk 2.3 rigidity spectrum i (R) rigidity distribution of cosmic ray particle fluxes 2.4 energy spectrum F i (E) energy distribution of cosmic ray particle fluxes 3 Principles of the model 3.1 The mo
21、del describes the variations of GCR fluxes due to variations in solar activity and in the large- scale heliospheric magnetic field (the suns polar magnetic field) throughout 22-year cycles. BSISO15390:2004 2 3.2 The angular distribution of galactic cosmic ray fluxes in the Earths orbit beyond the Ea
22、rths magnetosphere is to be isotropic. 3.3 Solar activity is characterized by 12-month averages of Wolf numbers (sunspot numbers) . W 3.4 The variations of the large-scale heliospheric magnetic field are assumed to be proportional to the variations of the Suns polar magnetic field whose intensity an
23、d polarity are taken to be dependent on solar activity and on whether a given solar cycle is even or odd: () ( ) () 2,7 min 1 max min ,1 1 n n nn Wt W MWtn S WW = (1) where S = 1 at 0 n tt W (otherwise, S = 1); n t is the sign reversal moment of the polar magnetic field in the nth solar cycle identi
24、fied with solar maximum (values suggested for particle flux prediction: 19 1958,21; t = 20 1968,87; t = 21 1979,96; t = 22 1989,46; t = 23 2 000,71 t = and 24 2 011,3); t = max n W is the highest level of solar activity in the nth solar cycle; min n W is the least solar activity level that borders t
25、he nth solar cycle. 3.5 The dynamics of the large-scale GCR modulation is characterized by the effective modulation potential of the heliosphere, R 0(t,R), (for particles of rigidity R at a given moment t) calculated as () () 41 , 4 5 0 , , 0,37 3 10 , , R Wt tnRt W t tnRt = + (2) 3.6 The lag, t (n,
26、R,t), of GCR flux variations relative to solar activity variations is taken to depend on magnetic rigidity, R, of particles, on whether a solar cycle is odd or even (n), and on solar cycle phase: ( ) () () ( ) , 0 , 5 0 , 5 tnRt T T R T T R W + + =+ (3) where the lag amplitude is independent of part
27、icle rigidity in even cycles (T + ): T += 15 months (4) and in odd cycles (T ) is T (R) = 7,5 R 0,45months (5) The time function of the lag variations from Equation (3) to be () () () 0,2 min max 1 n wn n Wt t W W W = (6) where w t = 16 months. BSISO15390:2004 34 GCR rigidity and energy spectra 4.1
28、General In terms of the GCR model, the particle flux rigidity and energy spectra are calculated consecutively. 4.2 GCR particle rigidity spectra 4.2.1 GCR particle rigidity spectra i (R, t) (s m 2 sr GeV) 1for particles of rigidity R at moment t are calculated using the following equation: () () ( )
29、 , 0 , , i i i R t i i C R Rt RRR t R = + (7) where i (R, t) is a dimensionless parameter calculated using the following equation: () () () () 00 , 5,5 1,13 , exp , i i i Z RR Rt MWt n Z RR t RR t =+ (8) where is the particle velocity-to-luminal velocity ratio: 2 2 ii i R Am R Z = + (9) where A iand
30、 Z iare particle mass number and particle charge respectively (see Tables 1 and 2); m iis particle rest mass, namely, m e= 5,1 10 4GeV for electrons, m p= 0,938 GeV for protons, m Z W 2= 0,939 GeV/nucleon for nuclei. C i , i , iare parameters of non-modulated rigidity spectrum of i-specie particles.
31、 For particles with Z u 28 see Table 1. For particles with Z W 29, i= 26and i= 26 , C i , is calculated from equation 26 26 i i C CC C = where 26 i C Cdata is found in Table 2. BSISO15390:20044 4.2.2 The standard deviation values, i (R, t) , are calculated using the following equation: () () () , 2
32、0 0,08 , 1 , i i C i Rt i Rt C R RR t =+ + (10) 4.3 GCR energy spectra 4.3.1 The energy spectra F i (E,t) (s m 2 sr GeV) 1of GCR particles of energy E at moment t are calculated using the following equation: () () 3 10 , i ii i A FE t Rt Z = (11) For particles with A i= 1, the units are (s m 2 sr Me
33、V) 1 . For particles with A iW 2, the units are (s m 2 sr MeV/nucleon) 1 . 4.3.2 With prescribed rigidity R of GCR particles, the kinetic energy E, in GeV (GeV/nucleon for nuclei), is calculated using the following equation: 2 2 i ii i Z Emm R A = + + (12) 4.3.3 With prescribed kinetic energy of par
34、ticles, the rigidity R and the relative velocity of the particles are calculated using the following equation: () 2 i i i A R EE m Z =+ (13) () 2 i i EEm Em + = +(14) 4.3.4 Standard deviation values F i (E, t) are calculated using the following equation: () () () () , , , , i i Rt i FEt i F Et Rt =
35、(15) BSISO15390:2004 5Table 1 Parameters of GCR rigidity spectra for particles Z u 28 Z Particle A iC i C i i i1 e 1,0 170 e a 1 H 1,0 (1,85 0,13) 10 42,74 0,02 2,85 0,02 2 He 4,0 (3,69 0,22) 10 32,77 0,02 3,12 0,02 3 Li 6,9 19,5 1,5 2,82 0,02 3,41 0,11 4 Be 9,0 17,7 1,3 3,05 0,02 4,30 0,12 5 B 10,8
36、 49,2 1,6 2,96 0,01 3,93 0,05 6 C 12,0 103,0 3,0 2,76 0,01 3,18 0,04 7 N 14,0 36,7 1,2 2,89 0,01 3,77 0,05 8 O 16,0 87,4 2,1 2,70 0,01 3,11 0,04 9 F 19,0 3,19 0,28 2,82 0,03 4,05 0,06 10 Ne 20,2 16,4 0,70 2,76 0,01 3,11 0,07 11 Na 23,0 4,43 0,28 2,84 0,02 3,14 0,09 12 Mg 24,3 19,3 0,70 2,70 0,01 3,6
37、5 0,27 13 Al 27,0 4,17 0,22 2,77 0.02 3,46 0,21 14 Si 28,1 13,4 0,50 2,66 0,01 3,00 0,10 15 P 31,0 1,15 0,04 2,89 0,01 4,04 0,41 16 S 32,1 3,06 0,12 2,71 0,02 3,30 0,22 17 Cl 35,4 1,30 0,08 3,00 0,04 4,40 0,30 18 Ar 39,9 2,33 0,07 2,93 0,01 4,33 0,21 19 K 39,1 1,87 0,05 3,05 0,01 4,49 0,20 20 Ca 40,
38、1 2,17 0,06 2,77 0,01 2,93 0,16 21 Sc 44,9 0,74 0,02 2,97 0,01 3,78 0,19 22 Ti 47,9 2,63 0,08 2,99 0,01 3,79 0,17 23 V 50,9 1,23 0,04 2,94 0,01 3,50 0,14 24 Cr 52,0 2,12 0,06 2,89 0,01 3,28 0,17 25 Mn 54,9 1,14 0,05 2,74 0,02 3,29 0,27 26 Fe 55,8 9,32 0,24 2,63 0,01 3,01 0,07 27 Co 58,9 0,10 0,08 2,
39、63 4,25 0,79 28 Ni 58.7 0,49 0,02 2,63 0,01 3,52 0,28 NOTE 1 In the case of Z 2 nuclei, the C i , i , ivalues are for a mixture of the respective isotopes. NOTE 2 Atomic masses corresponding to the natural elemental abundances are taken to be mass numbers A ifor Z 2 nuclei in conformity with the per
40、iodic system chart. This is within the model accuracy. aIn the case of electrons, the parameter e e 3,0 1,4 exp R R = , where e 1 R = GeV. BSISO15390:2004 6 Table 2 Parameters and GCR rigidity spectra for particles Z W 29 Z Particle A iC i /C 26Z Particle A iC i /C 2629 Cu 63,5 6,8 10 461 Pm 144,2 1
41、,9 10 730 Zn 65,4 8,8 10 462 Sm 145,0 1,8 10 631 Ga 69,7 6,5 10 563 Eu 150,4 3,1 10 732 Ge 72,6 1,4 10 464 Gd 152,0 1,4 10 633 As 74,9 8,9 10 665 Tb 157,3 3,5 10 734 Se 79,0 5,2 10 566 Dy 158,9 1,4 10 635 Br 79,9 9,7 10 667 Ho 162,5 5,3 10 736 Kr 83,8 2,7 10 568 Er 164,9 8,8 10 737 Rb 85,5 8,8 10 66
42、9 Tu 167,3 1,8 10 738 Sr 87,6 2,9 10 570 Yb 168,9 8,9 10 739 Y 88,9 6,5 10 671 Lu 173,0 1,3 10 740 Zr 91,2 1,6 10 572 Hf 175,0 8,1 10 741 Nb 92,9 2,9 10 673 Ta 178,5 7,3 10 842 Mo 95,9 8,1 10 674 W 180,9 8,1 10 743 Tc 97,0 9,5 10 775 Re 183,9 2,8 10 744 Ru 101,0 3,1 10 676 Os 186,2 1,2 10 645 Rh 102
43、,9 1,6 10 677 Ir 190,2 7,9 10 746 Pd 106,4 4,6 10 678 Pt 192,2 1,5 10 647 Ag 107,9 1,5 10 679 Au 195,1 2,8 10 748 Cd 112,4 4,0 10 680 Hg 197,0 4,9 10 749 In 114,8 8,8 10 781 Tl 200,6 1,5 10 750 Sn 118,7 4,7 10 682 Pb 204,4 1,4 10 651 Sb 121,8 9,9 10 783 Bi 207,2 7,3 10 852 Te 127,6 5,7 10 684 Po 209
44、,0 0 53 J 126,9 1,1 10 685 At 210,0 0 54 Xe 131,3 2,7 10 686 Rn 222,0 0 55 Cs 132,9 6,5 10 787 Fr 223,0 0 56 Ba 137,3 6,7 10 688 Ra 226,0 0 57 La 138,9 6,0 10 789 Ac 227,0 0 58 Ce 140,1 1,8 10 690 Th 232,0 8,1 10 859 Pr 140,9 4,3 10 791 Pa 231,0 0 60 Nd 144,2 1,6 10 692 U 238,0 4,9 10 8BSISO15390:20
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