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GBZ44002-2024: Space environment - Method of the solar energetic protons fluences and peak fluxes determination
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Space environment - Method of the solar energetic protons fluences and peak fluxes determination
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GB/Z 44002-2024
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Basic data | Standard ID | GB/Z 44002-2024 (GB/Z44002-2024) | | Description (Translated English) | Space environment - Method of the solar energetic protons fluences and peak fluxes determination | | Sector / Industry | National Standard | | Classification of Chinese Standard | V06 | | Classification of International Standard | 49.020 | | Word Count Estimation | 30,348 | | Date of Issue | 2024-04-25 | | Date of Implementation | 2024-04-25 | | Issuing agency(ies) | State Administration for Market Regulation, China National Standardization Administration | GBZ44002-2024: Space environment - Method of the solar energetic protons fluences and peak fluxes determination
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GB /Z 44002-2024: Determination of proton injection and peak flux of solar energy in space environment
ICS 49:020
CCSV06
Guiding technical documents of the People's Republic of China on national standardization
Space environment solar energy proton injection and
Method for determining peak flux
Released on 2024-04-25
2024-04-25 implementation
State Administration for Market Regulation
The National Standardization Administration issued
Table of Contents
Preface III
1 Scope 1
2 Normative references 1
3 Terms and Definitions 1
4 Abbreviations 2
5 SPE event classification 3
6 Main principles 3
7 Calculation method 4
8 Basic Table 4
Appendix A (Informative) Structure Number Comparison List 9
Appendix B (Informative) Differences between this document and ISO /T R18147:2014 and their causes 10
Appendix C (Informative) Main Method Principles 11
Appendix D (Informative) Comparison of model and experimental data 17
Reference 21
Foreword
This document is in accordance with the provisions of GB/T 1:1-2020 "Guidelines for standardization work Part 1: Structure and drafting rules for standardization documents"
Drafting:
This document is modified to adopt ISO /T R18147:2014 "Space environment (natural and artificial) Solar energy proton injection and peak flux
Determine the method:
Compared with ISO /T R18147:2014, this document has many structural adjustments:
See Appendix A for a list:
This document has many technical differences compared with ISO /T R18147:2014:
A single vertical line (︱) is used to indicate these differences: A list of these technical differences and their causes is given in Appendix B:
The following editorial changes were made to this document:
--- To be consistent with my country's technical standard system, the name of this document is changed to "Space Environment Solar Energy Proton Injection and Peak Flux"
Determine the method";
---Added explanations of variables in formulas;
---Adjusted references:
Please note that some of the contents of this document may involve patents: The issuing organization of this document does not assume the responsibility for identifying patents:
This document was proposed by the Chinese Academy of Sciences:
This document is under the jurisdiction of the National Technical Committee on Aerospace Technology and Its Applications Standardization (SAC/TC425):
This document was drafted by: Beijing Satellite Environment Engineering Research Institute, Harbin Institute of Technology, Beijing Tiangong Keyi Space Technology Co:, Ltd:,
Xiangtan University, Harbin Institute of Technology (Shenzhen), Beijing Space Vehicle Design Department, National Space Science Center of the Chinese Academy of Sciences, China Geophysical Research Institute
Institute of Geophysics, China Seismological Bureau, Xi’an Jiaotong University, China Institute of Space Standardization, and China Academy of Space Technology:
The main drafters of this document are: Shen Zicai, Ouyang Xiaoping, Li Xingji, Qiu Zhenyu, Hu Yanqi, Ji Qizheng, Mao Xin, Wang Yue, Feng Xueshang, Jiao Liguo,
Wang Xinyue, Zuo Pingbing, Lu Ziwei, Ying Tao, Li Changhong, Xu Dongyan, Sun Wei, and Liu Wei:
Space environment solar energy proton injection and
Method for determining peak flux
1 Scope
This document gives the solar energy proton flux and peak value during the on-orbit operation of spacecraft in the extra-magnetic space under different solar activity conditions:
The differential energy spectrum of the flux has an energy range of 0:1MeV~103MeV: If the change with the distance from the sun is taken into account, this method is suitable for determining the entire
The solar energy proton injection and peak flux in the heliosphere: When the geomagnetic shielding effect is taken into account, this method is suitable for calculating the near-Earth orbit aerospace
Solar energy proton flux and peak flux for spacecraft and manned space station orbits:
This document is applicable to the calculation of the probability of occurrence of solar energy protons that have important effects on materials, electronic components and organisms:
2 Normative references
The contents of the following documents constitute the essential clauses of this document through normative references in this document:
For referenced documents without a date, only the version corresponding to that date applies to this document; for referenced documents without a date, the latest version (including all amendments) applies to
This document:
GB/T 32452-2015 Spacecraft space environment terminology
GB/T 37834 Galactic cosmic ray model
3 Terms and definitions
The terms and definitions defined in GB/T 32452-2015 and GB/T 37834 and the following apply to this document:
3:1
sunspot number
Wolf number wolfnumber
An index that represents the degree of sunspot activity:
Note: w=k(10×gf), where g is the number of sunspot groups, f is the total number of sunspots on the visible solar disk, and k is the coefficient:
3:2
Solar cosmic rays
High-energy particles emitted from the sun:
3:3
Solar proton event solarprotonevent
An event in which the proton flux above 10 MeV in geosynchronous orbit reaches 10 pfu during a solar activity outburst:
[Source: GB/T 32452-2015, 3:7:2:4]
3:4
Solar activity
A general term for all active phenomena on the sun:
Note: These mainly include sunspots, bright spots, spectral spots, flares, prominences and coronal transient events:
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