BS ISO 17761-2015 Space environment (natural and artificial) Model of high energy radiation at low altitudes (300 km to 600 km)《航天环境 (天然和人造) 低海拔 (300 km至600 km) 的高能量辐射模型》.pdf

《BS ISO 17761-2015 Space environment (natural and artificial) Model of high energy radiation at low altitudes (300 km to 600 km)《航天环境 (天然和人造) 低海拔 (300 km至600 km) 的高能量辐射模型》.pdf》由会员分享，可在线阅读，更多相关《BS ISO 17761-2015 Space environment (natural and artificial) Model of high energy radiation at low altitudes (300 km to 600 km)《航天环境 (天然和人造) 低海拔 (300 km至600 km) 的高能量辐射模型》.pdf（18页珍藏版）》请在麦多课文档分享上搜索。

1、BSI Standards PublicationBS ISO 17761:2015Space environment (naturaland artificial) Model ofhigh energy radiation at lowaltitudes (300 km to 600 km)BS ISO 17761:2015 BRITISH STANDARDNational forewordThis British Standard is the UK implementation of ISO 17761:2015.The UK participation in its preparat

2、ion was entrusted to TechnicalCommittee ACE/68, Space systems and operations.A list of organizations represented on this committee can beobtained on request to its secretary.This publication does not purport to include all the necessaryprovisions of a contract. Users are responsible for its correcta

3、pplication. The British Standards Institution 2015.Published by BSI Standards Limited 2015ISBN 978 0 580 85087 5ICS 49.140Compliance with a British Standard cannot confer immunity fromlegal obligations.This British Standard was published under the authority of theStandards Policy and Strategy Commit

4、tee on 31 December 2015.Amendments/corrigenda issued since publicationDate T e x t a f f e c t e dBS ISO 17761:2015 ISO 2015Space environment (natural and artificial) Model of high energy radiation at low altitudes (300 km to 600 km)Environnement spatial (naturel et artificiel) Modle de radiations n

5、ergie leve basses altitudes (300 km 600 km)INTERNATIONAL STANDARDISO17761First edition2015-11-15Reference numberISO 17761:2015(E)BS ISO 17761:2015ISO 17761:2015(E)ii ISO 2015 All rights reservedCOPYRIGHT PROTECTED DOCUMENT ISO 2015, Published in SwitzerlandAll rights reserved. Unless otherwise speci

6、fied, no part of this publication may be reproduced or utilized otherwise in any form or by any means, electronic or mechanical, including photocopying, or posting on the internet or an intranet, without prior written permission. Permission can be requested from either ISO at the address below or IS

7、Os member body in the country of the requester.ISO copyright officeCh. de Blandonnet 8 CP 401CH-1214 Vernier, Geneva, SwitzerlandTel. +41 22 749 01 11Fax +41 22 749 09 47copyrightiso.orgwww.iso.orgBS ISO 17761:2015ISO 17761:2015(E)Foreword ivIntroduction v1 Scope . 12 Terms and definitions . 13 Gene

8、ral concepts and assumptions 2Annex A (informative) Tables for proton and electron fluxes 3Bibliography 6 ISO 2015 All rights reserved iiiContents PageBS ISO 17761:2015ISO 17761:2015(E)ForewordISO (the International Organization for Standardization) is a worldwide federation of national standards bo

9、dies (ISO member bodies). The work of preparing International Standards is normally carried out through 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 organizatio

10、ns, governmental and non-governmental, in liaison with ISO, also take part in the work. ISO collaborates closely with the International Electrotechnical Commission (IEC) on all matters of electrotechnical standardization.The procedures used to develop this document and those intended for its further

11、 maintenance are described in the ISO/IEC Directives, Part 1. In particular the different approval criteria needed for the different types of ISO documents should be noted. This document was drafted in accordance with the editorial rules of the ISO/IEC Directives, Part 2 (see www.iso.org/directives)

12、. Attention is drawn to the possibility that some of the elements of this document may be the subject of patent rights. ISO shall not be held responsible for identifying any or all such patent rights. Details of any patent rights identified during the development of the document will be in the Intro

13、duction and/or on the ISO list of patent declarations received (see www.iso.org/patents). Any trade name used in this document is information given for the convenience of users and does not constitute an endorsement.For an explanation on the meaning of ISO specific terms and expressions related to c

14、onformity assessment, as well as information about ISOs adherence to the WTO principles in the Technical Barriers to Trade (TBT) see the following URL: Foreword - Supplementary informationThe committee responsible for this document is ISO/TC 20, Aircraft and space vehicles, Subcommittee SC 14, Space

15、 systems and operations.iv ISO 2015 All rights reservedBS ISO 17761:2015ISO 17761:2015(E)IntroductionThe International Standard is intended for the estimation of high energy charged particle fluxes at low altitudes (300 km to 600 km) in the Earths magnetosphere. Detailed information on high energy c

16、harged particle fluxes is essential for developing spacecrafts and spacecraft equipment.High energy galactic cosmic rays1approaching the Earth interact with the atmosphere resulting in a production of secondary particles. The flux of secondary particles is composed mainly by electrons, protons, neut

17、rons and gamma-rays which execute their trajectories in the Earths magnetic field.2An appreciable fraction of charged secondary particles with rigidity less than geomagnetic cut-off3can travel backward in space along the Earths magnetic field lines and can reach the satellite altitudes forming a hig

18、h energy radiation halo in the Earth vicinity. The other fraction of secondary protons is trapped by geomagnetic field for years forming the inner radiation belt. These protons with kinetic energies greater than some tens of MeV mainly originated from the -decay of albedo neutrons according to the s

19、o-called “Cosmic Ray Albedo Neutron Decay” (CRAND) mechanism.4According to this mechanism, the Earth is surrounded in its equatorial region by shaped ring of high radiation. Because of a shift of geomagnetic dipole with respect to the Earth centre, in South Atlantic Anomaly (SAA) trapped particles a

20、re observed at low altitudes approximately 300 km.On the basis of the data primarily taken from mid-sixties to early seventies of the last century, the model of the Earths trapped proton radiation has been provided by the NASA AP-8 models.4Significant improvements of radiation environment modelling

21、in low Earth orbit (LEO) was carried out thanks to data from satellite experiments, such as CRRES, SAMPEX/PET and the TIROS/NOAA series.567These models can be used for estimations of radiation environment for energies below 100 eV with some procedures taking into account secular variations of the ge

22、omagnetic filed and drift of SAA for current epoch (e.g. Reference 8).Modern, more accurate measurements of the high energy (Ekin above 100 MeV) cosmic ray radiation in LEO have been reported by the PAMELA mission.9These new measurements including trapped component and charged albedo components are

23、the basis of this International Standard. ISO 2015 All rights reserved vBS ISO 17761:2015BS ISO 17761:2015Space environment (natural and artificial) Model of high energy radiation at low altitudes (300 km to 600 km)1 ScopeThis International Standard describes the fluxes of charged particles for near

24、-Earth space on base of the PAMELA experiment data. This International Standard can be used to calculate fluxes of protons with energy more than 100 MeV up to geomagnetic cut-off rigidity at low altitudes (300 km to 600 km). The main goal of this International Standard is determining the impact of e

25、nergetic charged particle flux upon spacecraft instrumentation and astronauts.2 Terms and definitionsFor the purposes of this document, the following terms and definitions apply.2.1International Geomagnetic Reference Field modelIGRF modelgeomagnetic reference field in the form of a series of spheric

26、al harmonic functions10Note 1 to entry: The International Association of Geomagnetism and Aeronomy (IAGA) is responsible for IGRF model development and modifications and approves its coefficients every five years.102.2particle magnetic rigiditymagnetic rigidity of particle, R, is related to particle

27、 momentum, p, and its charge, Z, by:R = pc/Zwhere c is the speed of light.32.3cut-off rigiditylocation of a transition for primary charged cosmic ray particles, in rigidity space, from allowed to forbidden trajectories as rigidity is decreased32.4geomagnetic coordinates L and Bused to map differenti

28、al fluxes j of energetic geomagnetically trapped particlesNote 1 to entry: B is absolute value of geomagnetic field in the point of observation. In the dipole approximation of the geomagnetic field, L-shell is distance to magnetic field line in equatorial plane.Note 2 to entry: Geomagnetic coordinat

29、es L-shell and B are introduced by MacIlwain.112.5Albedo trapped particlespart of cosmic ray charged radiation with rigidity below geomagnetic cut-off produced in interactions of high energy cosmic rays with residual atmosphere of the Earth which execute their trajectories in the Earth magnetic fiel

30、dINTERNATIONAL STANDARD ISO 17761:2015(E) ISO 2015 All rights reserved 1BS ISO 17761:2015ISO 17761:2015(E)3 General concepts and assumptionsThis International Standard determines the fluxes of high energy radiation at the altitudes from 300 km to 600 km over the Earth sea level which is recommended

31、to use for an estimation of radiation environment. Tables A.1 to A.3 provide differential vertical fluxes of albedo trapped protons, jp(Ekin) (Annex A, Tables A.1 and A.2), and albedo positron and electron, je(Ekin) (Table A.3), as a function of kinetic energy Ekin from Ekin100 MeV up to a maximum e

32、nergy corresponding to lowest geomagnetic cut-off.3Above maximum Ekin in Tables A.1 and A.2 primary cosmic ray dominates and for flux calculation, it is necessary to use ISO 15390. Tables of fluxes are based on smoothed PAMELA experimental data.12131415To map differential fluxes of particles geomagn

33、etic coordinates (LB)11calculated for IGRF model3are used.The model presents vertical flux averaged over low altitude orbits for fixed geomagnetic coordinates. No longitudinal and time variations of fluxes are suggested for high energy trapped particles into inner magnetosphere.2 ISO 2015 All rights

34、 reservedBS ISO 17761:2015ISO 17761:2015(E)Annex A (informative) Tables for proton and electron fluxesTable A.1 Differential fluxes of protons Jp(Ekin)for the 20062009 epoch averaged over altitude from 300 km up to 600 km, particles/(m2sr s MeV)121314Equatorial regionL-shell 0,90 to 1,20,90 to 1,2 0

35、,90 to 1,2 0,90 to 1,2 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5B, GsEkin, GeV0,9 to 0,20,2 to 0,21 0,21 to 0,220,22 0,19 to 0,20 0,20 to 0,210,21 to 0,220,22 to 0,230,23204,0 61,37 1,921 0,162 23,08 3,73 0,406 0,130 0,0810,119 192,0 57, 52 1,784 0,155 21,32 3,42 0,342 0,123 0,0780,133

36、179,8 53,6 1,65 0,151 19,6 3,10 0,319 0,114 0,0760,149 154,7 45,7 1,38 0,143 16,3 2,42 0,265 0,093 0,0720,168 129,2 37, 80 1,13 0,134 13,04 1,83 0,191 0,084 0,0620,188 105,9 30,6 0,907 0,117 10,20 1,36 0,162 0,060 0,0600,211 84,5 24,09 0,698 0,115 7,78 0,946 0,148 0,057 0,0540,237 66,2 18,51 0,525 0

37、,103 5,82 0,641 0,114 0,054 0,0480,266 50,8 13,97 0,399 0,100 4,18 0,421 0,091 0,053 0,0410,299 37, 8 10,1 0,273 0,098 2,95 0,274 0,063 0,050 0,0360,335 27, 5 7, 25 0,193 0,091 2,01 0,178 0,044 0,048 0,0290,376 19,5 4,99 0,152 0,077 1,36 0,112 0,036 0,038 0,0260,422 13,3 3,31 0,118 0,077 0,915 0,069

38、 0,034 0,031 0,0210,473 8,97 2,13 0,099 0,073 0,582 0,047 0,030 0,032 0,0180,531 5,86 1,365 0,081 0,057 0,345 0,029 0,029 0,029 0,0150,596 3,79 0,812 0,064 0,051 0,214 0,020 0,026 0,023 0,0130,669 2,35 0,492 0,049 0,042 0,113 0,016 0,020 0,017 0,0100,751 1,38 0,300 0,044 0,033 0,055 0,015 0,013 0,01

39、3 0,0080,842 0,781 0,173 0,037 0,025 0,029 0,012 0,008 0,009 0,0070,945 0,434 0,096 0,029 0,021 0,019 0,009 0,005 0,007 0,0051,06 0,244 0,058 0 0,023 0,016 0,009 7 0,007 9 0,005 9 0,006 3 0,004 31,19 0,129 0,039 0,019 3 0,016 5 0,006 8 0,006 1 0,006 1 0,005 2 0,003 41,33 0,057 0 0,027 0,015 0,012 0,

40、003 9 0,005 5 0,005 5 0,004 0 0,002 81,49 0,031 2 0,020 0,011 0,009 5 0,002 2 0,003 7 0,005 5 0,001 8 0,002 11,68 0,018 0,016 5 0,010 0,007 2 0,001 1 0,002 8 0,004 9 0,001 3 0,001 81,88 0,0140 0,012 8 0,008 9 0,006 3 0,001 6 0,002 4 0,003 4 0,001 9 0,001 42,11 0,012 0,007 9 0,006 7 0,004 6 0,001 6 0

41、,002 2 0,002 5 0,001 1 0,001 22,37 0,007 89 0,005 2 0,005 1 0,004 2 0,001 3 0,001 9 0,002 5 0,001 1 0,001 12,66 0,004 77 0,003 9 0,004 1 0,003 4 0,001 3 0,001 3 0,002 0 0,001 5 0,001 02,99 0,003 49 0,002 3 0,002 3 0,002 2 0,001 8 7,9E- 4 0,001 4 0,001 2 9,4E-43,35 0,002 37 0,001 2 0,001 9 0,001 5 0,

42、001 6 9,8E-4 0,001 7 8,6E-4 9,5E-4 ISO 2015 All rights reserved 3BS ISO 17761:2015ISO 17761:2015(E)L-shell 0,90 to 1,20,90 to 1,2 0,90 to 1,2 0,90 to 1,2 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5 1,2 to 1,5B, GsEkin, GeV0,9 to 0,20,2 to 0,21 0,21 to 0,220,22 0,19 to 0,20 0,20 to 0,210,21 to 0,220,

43、22 to 0,230,233,76 8,4E-4 9,3E-4 0,001 7 9,4E-4 0,001 4 0,001 0 0,001 5 9,0E-44,22 4,0E-4 4,8E-4 6,5E-4 5,4E-4 0,001 44,73 4,4E-4 4,2E-4 5,2E-4 4,6E-4 0,001 25,31 1,8E-4 2,7E-4 4,3E-45,96 5,2E-5 2,2E-4Table A.2 Differential fluxes of protons Jp(Ekin)for the 20062009 epoch averaged over altitude from

44、 300 km up to 600 km, particles/(m2sr s MeV)121314Middle and pole latitudesL-shell 1,5 to 2 1,2 to 1,2 1,5 to 2 1,5 to 2 2 to 2,4 2 to 2,4 2,4 to 3,0 3,0 to 4,0 4 to 5,5B, GsEkin, GeV0,2 to 0,21 0,21 to 0,220,22 to 0,230,23 0,22 to 0,230,23 0,23 0,23 0,230,106 1,44 0,407 0,209 0,116 0,239 0,182 0,27

45、0 0,489 1,0260,119 1,20 0,358 0,197 0,111 0,240 0,177 0,266 0,474 1,0410,133 1,09 0,326 0,191 0,108 0,232 0,170 0,263 0,464 1,0740,149 0,694 0,235 0,127 0,097 0,215 0,152 0,249 0,4420,168 0,515 0,167 0,111 0,084 0,196 0,132 0,236 0,4130,188 0,311 0,130 0,109 0,077 0,172 0,117 0,224 0,3980,211 0,233

46、0,108 0,092 0,069 0,151 0,098 0,207 0,3890,237 0,112 0,090 0,067 0,058 0,131 0,086 0,188 0,3880,266 0,077 0,085 0,061 0,048 0,108 0,075 0,1670,299 0,058 0,074 0,061 0,043 0,094 0,067 0,1480,335 0,055 0,066 0,049 0,036 0,089 0,059 0,1310,376 0,048 0,056 0,046 0,030 0,068 0,053 0,1140,422 0,045 0,042

47、0,045 0,024 0,054 0,043 0,0990,473 0,028 0,043 0,036 0,018 0,046 0,038 0,0880,531 0,017 0,038 0,030 0,014 0,035 0,033 0,0760,596 0,018 0,034 0,026 0,012 0,028 0,030 0,0710,669 0,016 0,027 0,017 0,009 0,027 0,026 0,0790,751 0,013 0,021 0,012 0,008 0,023 0,0230,842 0,016 0,014 0,013 0,007 0,021 0,0210

48、,945 0,014 0,011 0,010 0,006 0,020 0,0181,06 0,010 4 0,010 7 0,009 1 0,006 0,017 3 0,015 31,19 0,008 2 0,010 3 0,007 1 0,005 2 0,015 0,0141,33 0,006 8 0,009 9 0,004 7 0,004 51,49 0,005 0 0,008 8 0,002 7 0,004 21,68 0,005 0 0,007 0 0,003 1 0,003 71,88 0,002 4 0,005 9 0,001 7 0,003 52,11 0,001 4 0,006

49、 12,37 0,001 4Table A.1 (continued)4 ISO 2015 All rights reservedBS ISO 17761:2015ISO 17761:2015(E)L-shell 1,5 to 2 1,2 to 1,2 1,5 to 2 1,5 to 2 2 to 2,4 2 to 2,4 2,4 to 3,0 3,0 to 4,0 4 to 5,5B, GsEkin, GeV0,2 to 0,21 0,21 to 0,220,22 to 0,230,23 0,22 to 0,230,23 0,23 0,23 0,232,66 6,4E-4Table A.3 Total positrons and electrons differential fluxes Je(Ekin) for the 20062009 epoch averaged over altitude from 300 km up to 600 km, particles/(m2sr s MeV) 1315L-shell 0,