《BS-ISO-23038-2006.pdf》由会员分享，可在线阅读，更多相关《BS-ISO-23038-2006.pdf（14页珍藏版）》请在三一文库上搜索。
1、BRITISH STANDARD BS ISO 23038:2006 Space systems Space solar cells Electron and proton irradiation test methods ICS 49.140 ? Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI BS ISO 23038:2006 This British Standard was published under the auth
2、ority of the Standards Policy and Strategy Committee on 31 October 2006 BSI 2006 ISBN 0 580 48703 2 National foreword This British Standard was published by BSI. It is the UK implementation of ISO 23038:2006. The UK participation in its preparation was entrusted by Technical Committee ACE/68, Space
3、systems and operations, to Subcommittee ACE/68/-/1, Space systems and operations Engineering Design production. A list of organizations represented on ACE/68/-/1 can be obtained on request to its secretary. This publication does not purport to include all the necessary provisions of a contract. User
4、s are responsible for its correct application. Compliance with a British Standard cannot confer immunity from legal obligations. Amendments issued since publication Amd. No. DateComments Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI Refere
5、nce number ISO 23038:2006(E) INTERNATIONAL STANDARD ISO 23038 First edition 2006-10-01 Space systems Space solar cells Electron and proton irradiation test methods Systmes spatiaux Cellules solaires spatiales Mthodes dessai dirradiation dlectrons et de protons BS ISO 23038:2006 Licensed Copy: sheffi
6、eldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI ii Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI iii Foreword ISO (the International Organization for Standardization) is a worldwide federation of natio
7、nal standards bodies (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. Internati
8、onal organizations, 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. International Standards are drafted in accordance with the rul
9、es given in the ISO/IEC Directives, Part 2. The main task of technical committees is to prepare International Standards. 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
10、least 75 % of the member bodies casting a vote. 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. ISO 23038 was prepared by Technical Committee ISO/TC
11、20, Aircraft and space vehicles, Subcommittee SC 14, Space systems and operations. BS ISO 23038:2006 Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI blank Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncont
12、rolled Copy, (c) BSI 1 Space systems Space solar cells Electron and proton irradiation test methods 1 Scope This International Standard specifies the requirements for electron and proton irradiation test methods of space solar cells. It addresses only test methods for performing electron and proton
13、irradiation of space solar cells and not the method for data analysis. 2 Terms and definitions For the purposes of this document, the following terms and definitions apply. NOTE Physical constants are given to four significant figures only and reflect current knowledge. 2.1 differential energy spect
14、rum spread of energies of some specific group NOTE In this document, this refers to the number of particles possessing an energy value that lies in the infinitesimal range E, E+dE divided by the size of the range (dE). Integration of the differential particle spectrum over all particle energies yiel
15、ds the total number of particles. This quantity is given in units of particles per unit area per unit energy. 2.2 electron e elementary particle of rest mass m = 9,109 1031 kg, having a negative charge of 1,602 1019 C 2.3 flux number of particles passing through a given area in a specified time NOTE
16、 Flux may also be specified in terms of the number of particles per unit time passing through a unit area from source directions occupying a unit solid angle. Typical units are particles per cm2 per second per steradian (sr) (1 sr is the solid angle subtended at the centre of a unit sphere by a unit
17、 area of the surface of the sphere). 2.4 fluence total number of particles per unit area in any given time period NOTE Fluence is also known as time-integrated flux. 2.5 integral energy spectrum total number of particles per unit area in a specified group that possess energies greater than, or equal
18、 to, a specified value 2.6 irradiation exposure of a substance to energetic particles that penetrate the material and have the potential to transfer energy to the material BS ISO 23038:2006 Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI 2 2
19、.7 non-ionizing energy loss NIEL rate at which the incident particle transfers energy to the crystal lattice through non-ionizing events NOTE Typical unit is MeV cm2 g1. 2.8 omnidirectional flux number of particles of a particular type which have an isotropic distribution over 4 steradians and that
20、would traverse a test sphere of 1 cm2 cross-sectional area in 1 s NOTE Expressed in units of particles per cm2 per second. 2.9 proton p+ positively charged particle of mass number one, having a mass of 1,672 1027 kg and a charge equal in magnitude but of opposite sign to that of the electron NOTE A
21、proton is the nucleus of a hydrogen atom. 3 Symbols and abbreviated terms eV electronvolt NOTE A unit of energy commonly used for ions, electrons, elementary particles, etc. (1 eV 1,602 1019 J.) 4 Space radiation environments 4.1 Space radiation Primarily electrons and protons with a wide range of e
22、nergies characterize the space radiation environment. Gamma rays can be used as a substitute for electron irradiation with the proper transformation. Some reasonable electron and proton fluence limits usually attained in typical space conditions are given below. For 1 MeV electrons and 10 MeV proton
23、s, these typical but not inclusive fluence limits are 1015 and 1013 particles per cm2, respectively. Alpha particles and other charged particles are usually of negligible quantity as far as solar-cell damage is concerned. The particles come from the solar wind and are trapped by the Earths magnetic
24、field to form radiation belts with widely varying intensities 1. Solar wind is usually associated with particles of low energy (typically below 100 keV), whereas the particles of concern for solar cells are generally of higher energies. The inner portion of the belts consists mainly of protons and o
25、f an inner electron belt, whereas the outer portion consists primarily of electrons. Outside of these radiation belts, there is a likelihood of sudden bursts of protons and electrons originating from coronal mass ejections from the Sun, referred to generally as solar flares. Thus, the differential s
26、pectrum of electrons and protons for any given mission is dependent on the specific mission orbit. Owing to the large variability of the involved phenomena, the prediction of the particle spectrum for a given mission is affected by a significant uncertainty. The most widely accepted tools for its ca
27、lculation are the AP8 (protons) and AE8 (electrons) codes developed by NASA for the trapped particles, whereas the solar flares are modelled with other tools such as the JPL 91 code. 4.2 Shielding effects Space solar cells are typically flown with some material covering the cell surface, most typica
28、lly a piece of glass (coverglass), and are mounted on some support structure. These front and rear covering materials act to shield the solar cell from some of the incident irradiation. Because of this, the solar cell in space is actually irradiated by a modified particle spectrum, usually referred
29、to as a slowed down spectrum. An example showing such a slowed down spectrum calculation can be found in item 2 of the bibliography. BS ISO 23038:2006 Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI 3 5 General radiation effects in solar cel
30、ls 5.1 Solar-cell radiation damage Solar cells, like all semiconductor devices, are subject to electrical degradation when exposed to particle irradiation. In terms of radiation damage to solar cells used in space, the primary particles of interest are electrons and protons. When these energetic par
31、ticles are incident upon the solar-cell material, they collide with the atoms of the crystal lattice of the solar cell. In these atomic collisions, energy is transferred from the incident particle to the target atom. This energy can be transferred in several ways. The majority of the energy is trans
32、ferred through ionization of the target atom, where electrons of the target atom absorb the transferred energy and are promoted to higher energy levels. Another energy transfer mechanism is through non-ionizing events, which result in displacement of the target atom. If enough energy is transferred
33、in a non-ionizing event, then the displaced target atom may, in turn, displace other atoms, creating a cascade of displaced atoms. The displacement damage induced by the non-ionizing interactions is the primary cause of most solar-cell degradation. When an atom is displaced in a lattice, the electro
34、n energy band structure of the material is disturbed, and localized energy levels can be created near the site of the defect. These defect energy levels can act to trap electrical charge carriers, thus restricting their ability to move through the material, which is characterized by a reduction in t
35、he minority carrier diffusion length. Since solar-cell operation depends on the motion of photogenerated charge carriers through the material, these defect sites tend to degrade the solar-cell performance. The amount of displacement damage caused by an incident particle is a function of the type of
36、incident particle (i.e. electron or proton), the particle energy, and the composition of the crystal lattice. The rate at which the incident particle transfers energy to the crystal lattice through non-ionizing events is referred to as the non-ionizing energy loss (NIEL). Electrons become more damag
37、ing as the incident electron energy increases. The opposite is true for protons, where the lower energy protons are the most damaging. Also, protons are significantly more damaging in comparison to electrons, primarily due to the increased proton differential scattering cross-section for atomic disp
38、lacements. There is a lower limit to displacement damage corresponding to the threshold energy for atomic displacements. 5.2 Radiation effects on solar-cell cover Although not specifically a solar-cell radiation effect, it is appropriate in this International Standard to note the effects of irradiat
39、ion on solar-cell coverglass material. Certain solar-cell coverglass material has been shown to darken under irradiation, thereby absorbing some of the incident light 4. This increased light absorption can reduce the solar-cell output in one of two ways: reduction of the amount of light that reaches
40、 the cell, or increase in operating temperature of array that reduces the cell electrical conversion efficiency. NOTE Testing cells with attached coverglass or different geometries require special care (see items 7 and 8 in the bibliography). 6 Radiation test methods 6.1 General As described in Clau
41、se 5, the space radiation environment consists of a spectrum of particle energies, and as described in this clause, solar-cell radiation damage is energy dependent. Irradiation by a spectrum of particles in a laboratory is not typical, so most ground radiation testing is done using a monoenergetic b
42、eam of particles. Therefore, any space solar-cell radiation testing shall be done in such a way as to enable extrapolation from monoenergetic radiation damage to damage produced by irradiation by a particle spectrum. This is typically done by using the ground test data to reduce the particle spectru
43、m to a fluence of monoenergetic particles that produce an equivalent amount of damage. The determination of the equivalent fluence can be achieved in different ways, the primary ones being the JPL and NRL methodologies 2, 3, 5. Although it is beyond the scope of this International Standard to discus
44、s these data analysis methods, it is important that the method to be used for a specific experiment be chosen and well understood prior to BS ISO 23038:2006 Licensed Copy: sheffieldun sheffieldun, na, Sun Nov 26 14:49:07 GMT+00:00 2006, Uncontrolled Copy, (c) BSI 4 performing any radiation testing.
45、Similarly, it should be noted that this International Standard gives guidelines on how to perform radiation testing on a space solar cell independent of the device technology. Differing cell technologies might exhibit differing radiation response characteristics that need to be understood in order t
46、o perform a meaningful test. On the basis of practical limitations, the recommended energy range for proton irradiations is 30 keV to 30 MeV. The recommended energy range for electron irradiations is 200 keV to 3 MeV. In special cases, lower energies might be achievable. Damage comparisons are usual
47、ly performed with 10 MeV protons and 1 MeV electrons. It can be convenient in some cases to perform particle transport calculations before performing the irradiations. These calculations can tell one how far the incident irradiation particle will travel within the solar cell before it stops. For exa
48、mple, if one wanted to irradiate a silicon solar cell, the irradiating particle would need to travel some distance on the order of 100 m to reach the active region of the solar cell and therefore cause significant damage. Therefore, it is necessary to perform the transport calculation to determine t
49、he particle energy required to cover this distance. For proton transport calculations, the Monte Carlo code SRIM 12 should be used; for electron irradiation, ITS TIGER 13 should be used. Post-irradiation annealing is one specific example. Silicon (Si) solar cells have been observed to anneal over time at room temperature after irradiation. It was found that the cell electrical output stabilized after a 24 h, 60 C anneal, so such a post-irradiation anneali