1、BSI Standards PublicationBS EN 16603-10-04:2015Space engineering SpaceenvironmentBS EN 16603-10-04:2015 BRITISH STANDARDNational forewordThis British Standard is the UK implementation of EN 16603-10-04:2015.It supersedes BS EN 14092:2002 which is withdrawn.BSI, as a member of CEN, is obliged to publ
2、ish EN 16603-10-04 as aBritish Standard. However, attention is drawn to the fact that duringthe development of this European Standard, the UK committee votedagainst its approval as a European Standard. The UK committee are of the opinion that parts of Clause 10 conflictwith ISO 14200:2012 which has
3、already been adopted by BSI. In partic-ular, Clause 10 requires the use of ESAs MASTER-2005 space debris andmeteoroid flux model, whereas ISO 14200:2012 does not prescribe theuse of a particular flux model but sets out a process for selecting andusing a model from several that are available.Further,
4、 MASTER-2005 is a relatively old flux model that has since beensuperseded by MASTER-2009. The UK Committee are of the opinionthat ISO 14200:2012 should be used to select a space debris/meteoroidflux model for the purpose of performing an impact risk assessment.ISO 14200:2012 can also be used in conj
5、unction with ISO 16126:2014which defines two different procedures for analysing impact risk.The UK participation in its preparation was entrusted to TechnicalCommittee ACE/68, Space systems and operations.A list of organizations represented on this committee can be obtainedon request to its secretar
6、y.This publication does not purport to include all the necessary provisionsof a contract. Users are responsible for its correct application. The British Standards Institution 2015.Published by BSI Standards Limited 2015ISBN 978 0 580 83404 2ICS 49.140Compliance with a British Standard cannot confer
7、immunity fromlegal obligations.This British Standard was published under the authority of the StandardsPolicy and Strategy Committee on 28 February 2015.Amendments/corrigenda issued since publicationDate Text affectedBS EN 16603-10-04:2015EUROPEAN STANDARDNORME EUROPENNEEUROPISCHE NORMEN 16603-10-04
8、 January 2015 ICS 49.140 Supersedes EN 14092:2002 English version Space engineering - Space environment Ing?ierie spatiale - Environnement spatial Raumfahrttechnik - Raumfahrtumweltbedingungen This European Standard was approved by CEN on 28 December 2013. CEN and CENELEC members are bound to comply
9、 with the CEN/CENELEC Internal Regulations which stipulate the conditions for giving this European Standard the status of a national standard without any alteration. Up-to-date lists and bibliographical references concerning such national standards may be obtained on application to the CEN-CENELEC M
10、anagement Centre or to any CEN and CENELEC member.This European Standard exists in three official versions (English, French, German). A version in any other language made by translation under the responsibility of a CEN and CENELEC member into its own language and notified to the CEN-CENELEC Managem
11、ent Centre has the same status as the official versions. CEN and CENELEC members are the national standards bodies and national electrotechnical committees of Austria, Belgium, Bulgaria, Croatia, Cyprus, Czech Republic, Denmark, Estonia, Finland, Former Yugoslav Republic of Macedonia, France, German
12、y, Greece, Hungary, Iceland, Ireland, Italy, Latvia, Lithuania, Luxembourg, Malta, Netherlands, Norway, Poland, Portugal, Romania, Slovakia, Slovenia, Spain, Sweden, Switzerland, Turkey and United Kingdom. CEN-CENELEC Management Centre: Avenue Marnix 17, B-1000 Brussels 2015 CEN/CENELEC All rights o
13、f exploitation in any form and by any means reservedworldwide for CEN national Members and for CENELECMembers. Ref. No. EN 16603-10-04:2015 E BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 2 Table of contents Foreword 12 Introduction 13 1 Scope . 14 2 Normative references . 15 3 Terms, definitions an
14、d abbreviated terms 17 3.1 Terms defined in other standards . 17 3.2 Terms specific to the present standard . 17 3.3 Abbreviated terms. 26 4 Gravity . 29 4.1 Introduction and description 29 4.1.1 Introduction . 29 4.1.2 Gravity model formulation . 29 4.1.3 Third body gravitation 31 4.1.4 Tidal effec
15、ts. 31 4.2 Requirements for model selection and application 31 4.2.1 General requirements for gravity models . 31 4.2.2 Selection and application of gravity models . 32 5 Geomagnetic fields 33 5.1 Introduction and description 33 5.1.1 The geomagnetic field and its sources 33 5.1.2 The internal field
16、 . 33 5.1.3 External field: ionospheric components . 34 5.1.4 External magnetic field: magnetospheric components . 34 5.1.5 Models of the internal and external geomagnetic fields . 34 5.2 Requirements for model selection and application 36 5.2.1 The internal field . 36 5.2.2 The external field 36 5.
17、3 Tailoring guidelines . 37 BS EN 16603-10-04:2015EN 16603-10-04:2015 (E)BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 2 Table of contents Foreword 12 Introduction 13 1 Scope . 14 2 Normative references . 15 3 Terms, definitions and abbreviated terms 17 3.1 Terms defined in other standards . 17 3.2
18、Terms specific to the present standard . 17 3.3 Abbreviated terms. 26 4 Gravity . 29 4.1 Introduction and description 29 4.1.1 Introduction . 29 4.1.2 Gravity model formulation . 29 4.1.3 Third body gravitation 31 4.1.4 Tidal effects. 31 4.2 Requirements for model selection and application 31 4.2.1
19、General requirements for gravity models . 31 4.2.2 Selection and application of gravity models . 32 5 Geomagnetic fields 33 5.1 Introduction and description 33 5.1.1 The geomagnetic field and its sources 33 5.1.2 The internal field . 33 5.1.3 External field: ionospheric components . 34 5.1.4 Externa
20、l magnetic field: magnetospheric components . 34 5.1.5 Models of the internal and external geomagnetic fields . 34 5.2 Requirements for model selection and application 36 5.2.1 The internal field . 36 5.2.2 The external field 36 5.3 Tailoring guidelines . 37 BS EN 16603-10-04:2015EN 16603-10-04:2015
21、 (E) 3 6 Natural electromagnetic radiation and indices 38 6.1 Introduction and description 38 6.1.1 Introduction . 38 6.1.2 Electromagnetic radiation and indices . 38 6.2 Requirements . 41 6.2.1 Electromagnetic radiation 41 6.2.2 Reference index values . 42 6.2.3 Tailoring guidelines . 42 6.3 Tables
22、 . 43 7 Neutral atmospheres 45 7.1 Introduction and description 45 7.1.1 Introduction . 45 7.1.2 Structure of the Earths atmosphere 45 7.1.3 Models of the Earths atmosphere . 45 7.1.4 Wind model of the Earths homosphere and heterosphere 46 7.2 Requirements for atmosphere and wind model selection 47
23、7.2.1 Earth atmosphere . 47 7.2.2 Earth wind model 48 7.2.3 Models of the atmospheres of the planets and their satellites . 48 8 Plasmas . 49 8.1 Introduction and description 49 8.1.1 Introduction . 49 8.1.2 Ionosphere 49 8.1.3 Plasmasphere . 50 8.1.4 Outer magnetosphere . 50 8.1.5 Solar wind . 51 8
24、.1.6 Magnetosheath . 51 8.1.7 Magnetotail . 51 8.1.8 Planetary environments 52 8.1.9 Induced environments . 52 8.2 Requirements for model selection and application 52 8.2.1 General . 52 8.2.2 Ionosphere 53 8.2.3 Auroral charging environment . 53 8.2.4 Plasmasphere . 54 8.2.5 Outer magnetosphere . 54
25、 8.2.6 The solar wind (interplanetary environment) 55 BS EN 16603-10-04:2015EN 16603-10-04:2015 (E)BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 4 8.2.7 Other plasma environments 55 8.2.8 Tables . 56 9 Energetic particle radiation . 57 9.1 Introduction and description 57 9.1.1 Introduction . 57 9.1.
26、2 Overview of energetic particle radiation environment and effects 57 9.2 Requirements for energetic particle radiation environments 60 9.2.1 Trapped radiation belt fluxes . 60 9.2.2 Solar particle event models . 62 9.2.3 Cosmic ray models 63 9.2.4 Geomagnetic shielding 63 9.2.5 Neutrons . 63 9.2.6
27、Planetary radiation environments 64 9.3 Preparation of a radiation environment specification . 64 9.4 Tables . 65 10 Space debris and meteoroids 66 10.1 Introduction and description 66 10.1.1 The particulate environment in near Earth space 66 10.1.2 Space debris . 66 10.1.3 Meteoroids 67 10.2 Requir
28、ements for impact risk assessment and model selection 67 10.2.1 General requirements for meteoroids and space debris 67 10.2.2 Model selection and application 68 10.2.3 The MASTER space debris and meteoroid model . 69 10.2.4 The meteoroid model 69 10.2.5 Impact risk assessment . 70 10.2.6 Margins an
29、d worst case fluxes 71 11 Contamination 72 11.1 Introduction and description 72 11.1.1 Introduction . 72 11.1.2 Description of molecular contamination . 72 11.1.3 Transport mechanisms 73 11.1.4 Description of particulate contamination 73 11.1.5 Transport mechanisms 74 11.2 Requirements for contamina
30、tion assessment . 74 Annex A (normative) Natural electromagnetic radiation and indices . 75 BS EN 16603-10-04:2015EN 16603-10-04:2015 (E)BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 4 8.2.7 Other plasma environments 55 8.2.8 Tables . 56 9 Energetic particle radiation . 57 9.1 Introduction and descr
31、iption 57 9.1.1 Introduction . 57 9.1.2 Overview of energetic particle radiation environment and effects 57 9.2 Requirements for energetic particle radiation environments 60 9.2.1 Trapped radiation belt fluxes . 60 9.2.2 Solar particle event models . 62 9.2.3 Cosmic ray models 63 9.2.4 Geomagnetic s
32、hielding 63 9.2.5 Neutrons . 63 9.2.6 Planetary radiation environments 64 9.3 Preparation of a radiation environment specification . 64 9.4 Tables . 65 10 Space debris and meteoroids 66 10.1 Introduction and description 66 10.1.1 The particulate environment in near Earth space 66 10.1.2 Space debris
33、 . 66 10.1.3 Meteoroids 67 10.2 Requirements for impact risk assessment and model selection 67 10.2.1 General requirements for meteoroids and space debris 67 10.2.2 Model selection and application 68 10.2.3 The MASTER space debris and meteoroid model . 69 10.2.4 The meteoroid model 69 10.2.5 Impact
34、risk assessment . 70 10.2.6 Margins and worst case fluxes 71 11 Contamination 72 11.1 Introduction and description 72 11.1.1 Introduction . 72 11.1.2 Description of molecular contamination . 72 11.1.3 Transport mechanisms 73 11.1.4 Description of particulate contamination 73 11.1.5 Transport mechani
35、sms 74 11.2 Requirements for contamination assessment . 74 Annex A (normative) Natural electromagnetic radiation and indices . 75 BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 5 A.1 Solar activity values for complete solar cycle 75 A.2 Tables . 76 Annex B (normative) Energetic particle radiation 80
36、B.1 Historical dates of solar maximum and minimum 80 B.2 GEO model (IGE-2006) 80 B.3 ONERA MEOv2 model . 80 B.4 FLUMIC model . 81 B.4.1 Overview . 81 B.4.2 Outer belt (L2,5 Re) 81 B.4.3 Inner belt (L10 MeV) and electrons (10 MeV) at 400 km altitude showing the inner radiation belts “South Atlantic a
37、nomaly” and, in the case of electrons, the outer radiation belt encountered at high latitudes . 164 Figure I-4 : Comparison of POLE with AE8 (flux vs. Energy) for 15 year mission (with worst case and best case included) 165 Figure I-5 : Comparison of ONERA/GNSS model from 0,28 MeV up to 1,12 MeV (be
38、st case, mean case and worst case) with AE8 (flux vs. Energy) for 15 yr mission (with worst case E is the energy; m is the particle mass. 3.2.12 dose quantity of radiation delivered at a position NOTE In its broadest sense this can include the flux of particles, but in the context of space energetic
39、 particle radiation effects, it usually refers to the energy absorbed locally per unit mass as a result of radiation exposure. 3.2.13 dose equivalent radiation quantity normally applied to biological effects and includes scaling factors to account for the more severe effects of certain kinds of radi
40、ation 3.2.14 dust particulates which have a direct relation to a specific solar system body and which are usually found close to the surface of this body (e.g. Lunar, Martian or Cometary dust) 3.2.15 Earth infrared thermal radiation emitted by the Earth NOTE It is also called outgoing long wave radi
41、ation. 3.2.16 energetic particle particles which, in the context of space systems radiation effects, can penetrate outer surfaces of spacecraft NOTE For electrons, this is typically above 100 keV, while for protons and other ions this is above 1 MeV. Neutrons, gamma rays and X-rays are also consider
42、ed energetic particles in this context. 3.2.17 equivalent fluence quantity which attempts to represent the damage at different energies and from different species NOTE 1 For example: For solar cell degradation it is often taken that one 10 MeV protons is “equivalent” to 3 000 electrons of 1 MeV. Thi
43、s concept also occurs in consideration of Non-ionizing Energy Loss effects (NIEL). NOTE 2 Damage coefficients are used to scale the effect caused by particles to the damage caused by a standard particle and energy. BS EN 16603-10-04:2015EN 16603-10-04:2015 (E)BS EN 16603-10-04:2015EN 16603-10-04:201
44、5 (E) 20 3.2.18 exosphere part of the Earths atmosphere above the thermosphere for which the mean free path exceeds the scale height, and within which there are very few collisions between atoms and molecules NOTE 1 Near the base of the exosphere atomic oxygen is normally the dominant constituent. N
45、OTE 2 With increasing altitude, the proportion of atomic hydrogen increases, and hydrogen normally becomes the dominant constituent above about 1 000 km. Under rather special conditions (i.e. winter polar region) He atoms can become the major constituent over a limited altitude range. NOTE 3 A small
46、 fraction of H and He atoms can attain escape velocities within the exosphere. 3.2.19 external field part of the measured geomagnetic field produced by sources external to the solid Earth NOTE the external sources are mainly: electrical currents in the ionosphere, the magnetosphere and coupling curr
47、ents between these regions. 3.2.20 F10.7 flux solar flux at a wavelength of 10.7 cm in units of 104Jansky (one Jansky equals 10-26 Wm-2Hz-1) 3.2.21 fluence time-integration of the flux 3.2.22 flux amount of radiation crossing a surface per unit of time, often expressed in “integral form” as particle
48、s per unit area per unit time (e.g. electrons cm-2s-1) above a certain threshold energy NOTE The directional flux is the differential with respect to solid angle (e.g. particles cm-2steradian-1s-1) while the “differential” flux is differential with respect to energy (e.g. particles cm-2MeV-1s-1). In
49、 some cases fluxes are also treated as a differential with respect to Linear Energy Transfer (see 3.2.32). 3.2.23 free molecular flow regime condition where the mean free path of a molecule is greater than the dimensions of the volume of interest (characteristic length) 3.2.24 geocentric solar magnetospheric coordinates (GSM) elements of a right-handed Cartesian coordinate system (X,Y,Z) with the origin at the centre of the Earth BS EN 16603-10-04:2015EN 16603-10-04:2015 (E)BS EN 16603-10-04:2015EN 16603-10-04:2015 (E) 20 3.2.18 exosphere part of the Earths atmosphere above t
