Galactic Cosmic Ray induced absorbed dose rate in deep space – Accounting for detector size, shape, material, as well as for the solar modulation
Galactic Cosmic Ray induced absorbed dose rate in deep space – Accounting for detector size, shape, material, as well as for the solar modulation
复制标题
银河宇宙线在深空引起的吸收剂量率 â 考虑探测器的尺寸、形状、材料以及太阳调制
DOI：
10.1051/swsc/2019014
复制
发表时间：
2019
影响因子：
3.3
通讯作者：
R. Wimmer-Schweingruber
中科院分区：
文献类型：
--
作者：
Banjac S;L. Berger;S. Burmeister;J. Guo;B. Heber;K. Herbst;R. Wimmer-Schweingruber
根据辐射场的不同，吸收剂量率可能在很大程度上取决于探测器或模型中使用的体模的大小。在深空（行星际介质）中，辐射场一般由银河宇宙线（GCR）核控制。在这里，一个典型的小硅板探测器测量的深空剂量率与一个较大的体模相比较，该体模对应于一个由水组成的半径为15 cm的ICRU球体。为了分离和理解探测器中的成分、尺寸和形状差异的相应影响，这种比较分几个步骤进行。对每个模型，计算了Z = 28的GCR核的吸收剂量率随太阳调制条件的变化，GCR通量的主要成分是质子，其次是氦核和电子，Z> 2的核约占总粒子数的1%。在Z> 2的轻核中，C、N和O的丰度最高。在这项研究中，我们使用GEANT 4模型来计算吸收剂量（能量沉积为电离，除以质量）由于GCR通量提供的Badhwar-O 'Neill 2010（BON-10）模型。此外，我们调查如何确定的吸收剂量率在整个太阳周期的变化，通过不同的GCR模型从太阳最小到太阳最大的条件。对宇宙射线望远镜的辐射效应（CRaTER）微剂量计测量所开发的模型进行了验证。在我们目前的方法中，我们没有考虑屏蔽的影响，这将始终存在于现实的cross.A第二个研究的目标是量化的贡献，每个Z = 1，...，28 GCR核吸收剂量率，与体模的特性。对于每一个Z，我们确定最相关的能量范围内的GCR谱吸收剂量率估计。此外，我们还计算了太阳调制相关的转换因子，将硅中测得的吸收剂量率转换为水中的吸收剂量率。这些信息将提高我们对近地深空GCR辐射环境的理解，并通过限制必须考虑的初级粒子种类的数量和能量范围来进一步建模。
Depending on the radiation field, the absorbed dose rate can depend significantly upon the size of the detectors or the phantom used in the models. In deep space (interplanetary medium) the radiation field is on avarage dominated by Galactic Cosmic Ray (GCR) nuclei. Here, the deep space dose rate that a typical small silicon slab detector measures is compared to a larger phantom corresponding to an ICRU sphere with a 15 cm radius composed of water. To separate and understand respective effects from the composition, size and shape differences in the detectors, this comparison is implemented in several steps. For each phantom, the absorbed dose rate due to GCR nuclei up toZ= 28, as a function of solar modulation conditions, is calculated.The main components of the GCR flux are protons, followed by helium nuclei and electrons, withZ> 2 nuclei accounting for approximately 1% of the total number of particles. Among the light nuclei withZ> 2, most abundant ones are C, N and O. In this study, we use the GEANT4 model to calculate the absorbed dose (energy deposited as ionization, divided by mass) due to the GCR flux provided by the Badhwar-O’Neill 2010 (BON-10) model. Furthermore, we investigate how the determined absorbed dose rate changes throughout the solar cycle by varying the GCR models from solar minimum to solar maximum conditions. The developed model is validated against the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) microdosimeter measurements. In our current approach, we do not consider the effects of shielding, which will always be present under realistic scenarios.A second goal of this study is to quantify the contribution of eachZ= 1, …, 28 GCR nuclei to absorbed dose rate, in relation to the phantom characteristics. For eachZwe determine the most relevant energy range in the GCR spectra for absorbed dose rate estimations. Furthermore, we calculate a solar modulation dependent conversion factor to convert absorbed dose rate measured in silicon to absorbed dose rate in water. This information will improve our understanding of the radiation environment due to GCR in the near-Earth deep space and also benefit further modeling efforts by limiting the number and energy range of primary particle species that have to be considered.
登录
查看更多内容
ICRU 报告 33：辐射量和单位
DOI：
--
发表时间：
1980
期刊：
影响因子：
--
作者：
A. Jansen
通讯作者：
A. Jansen
人类在太空中的银河宇宙射线暴露：银河宇宙射线模型和屏蔽对近地轨道和近地行星际空间剂量计算的影响
DOI：
--
发表时间：
2014
期刊：
影响因子：
--
作者：
A. Mrigakshi
通讯作者：
A. Mrigakshi
DOI：
--
发表时间：
2015
期刊：
影响因子：
--
作者：
T. Nordheim;L. Dartnell;L. Desorgher;A. Coates;G. Jones
通讯作者：
G. Jones
银河宇宙线重和超重成分的电荷谱：奥林皮亚实验的结果
DOI：
--
发表时间：
2016
期刊：
影响因子：
--
作者：
V. Alexeev;A. Bagulya;M. Chernyavsky;A. Gippius;L. Goncharova;S. Gorbunov;M. Gorshenkov;G. Kalinina;N. Konovalova;Jieying Liu;P. Zhai;N. Okatyeva;Tatyana N. Pavlova;N. Polukhina;N. Starkov;T. N. Soe;C. Trautmann;E. Savchenko;T. Shchedrina;A. Vasiliev;A. Volkov
通讯作者：
A. Volkov
影响因子：
5
作者：
K. Nakamura;K. Hagiwara;K. Hikasa;H. Murayama;M. Tanabashi;T. Watari;C. Amsler;M. Antonelli
通讯作者：
K. Nakamura;K. Hagiwara;K. Hikasa;H. Murayama;M. Tanabashi;T. Watari;C. Amsler;M. Antonelli