Mechanism of cosmic ray high-energy particles charging test mass

Han Rui-Long; Cai Ming-Hui; Yang Tao; Xu Liang-Liang; Xia Qing; Han Jian-Wei

doi:10.7498/aps.70.20210747

Abstract

The testing mass is the core sensor for measuring the spatial gravitational waves. The high-energy cosmic ray particles penetrating the outer structure of the spacecraft result in the electrical charges on the testing mass. The Coulomb force produced by the charges on the surrounding conducting surface and the Lorentz force generated by the motion through the interplanetary magnetic field will exert a serious influence on the geodesic motion of the testing mass. In this paper are investigated the process and mechanism of charging the testing mass by high-energy particles from different cosmic rays through using the Monte Carlo simulation method. It is concluded that the charging rate gradually increases with the decrease of cut-off energy under the same energy spectrum. The positive charging rate (elementary charges per second) in the years of minimum solar activity is predicted to be 39.5 +e/s, and the protons account for approximately 83.16% of the total quantity of galactic cosmic rays. The positive charging rate of the testing mass during the years of maximum solar activity is about 12.5 +e/s, and the charging rate of the testing mass of the worst solar energetic particle event in 1989 is about 120700 +e/s. The charging rate of the components of the galactic cosmic ray depends on the deposition of primary particles of each component in the testing mass during the years of minimum solar activity, with primary particles accounting for 73% of the total charging rate. The charging contribution of protons in years of minimum solar activity is mainly in an energy range of 0.1–1 GeV, accounting for about 65%. The research results can be used to assess the charging patterns of test quality on-orbit charges and provide a basis for designing the charge management and on-orbit work.

Keywords:

Authors and contacts

1.
National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
2.
School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, China

Corresponding author: Cai Ming-Hui, caiminghui@nssc.ac.cn

Funds: Project supported by National Key Research and Development Program (Grant No. 2020YFC2201300), the Major Software Development Special Project of the Science and Technology Bureau, China (Grant No. E01Z360101), and the Joint Fund for Independent Innovation of the Future Laboratory of the Second Academy of Aerospace Science and Industry, China(Grant No. YQQT202102645)

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References

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[23]	Grimani C, Vocca H, Barone M, Stanga R, Vetrano F, Viceré A, Amico P, Bosi L, Marchesoni F, Punturo M, Travasso F 2004 Classical. Quantum Gravity. 21 S629 Google Scholar

Cited By

图 1 LISA航天器模型　(a)整体模型; (b)惯性传感器模型

Figure 1. LISA spacecraft model: (a) Overall model; (b) inertial sensor model.

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图 2 本文航天器模型图　(a) geant4模型图; (b)模型平面示意图

Figure 2. The spacecraft model diagram in this paper: (a) Geant4 model diagram; (b) schematic diagram of the model plane.

DownLoad: Full-Size Img PowerPoint

图 3 1 AU处GCR各粒子微分能谱

Figure 3. Differential energy spectra of each element of GCR at 1 AU.

DownLoad: Full-Size Img PowerPoint

图 4 1AU处1989年SEP微分能谱

Figure 4. 1989 SEP differential energy spectra at 1AU.

DownLoad: Full-Size Img PowerPoint

图 5 宇宙线Proton和He(³He和⁴He)微分能谱

Figure 5. Differential energy spectra of cosmic rays Proton and He (³He and ⁴He).

DownLoad: Full-Size Img PowerPoint

图 6 不同截断长度的充电速率

Figure 6. Charging rate with different cut-off lengths.

DownLoad: Full-Size Img PowerPoint

图 7 宇宙线各粒子的充电率　(a) 太阳活动极小年; (b) 太阳活动极大年

Figure 7. The charging rate of each particle of cosmic rays: (a) Solar minimum year; (b) solar maximum year.

DownLoad: Full-Size Img PowerPoint

图 8 宇宙线各粒子的充电能力

Figure 8. The charging ability of each particle of the cosmic ray

DownLoad: Full-Size Img PowerPoint

图 9 太阳活动极小充电能力　(a) 不同能量充电能力和质子通量; (b) 充电能力和结合质子通量的总充电比例

Figure 9. Solar minimum charging capacity: (a) Different energy charging capacity and proton flux; (b) charging capacity and total charge ratio of combined proton flux.

DownLoad: Full-Size Img PowerPoint

表 1 航天器几何尺寸和材料构成

Table 1. Spacecraft geometric dimensions and material composition.

名称	组成成分	密度/(g·cm^–3)	尺寸	厚度/mm
测试质量	Au(70%); Pt(30%)	19.837	46 mm立方体	—
钼电极	Mo	10.28	74—86 mm立方体壳层	6
钛室	Ti	4.54	75—80 mm球壳层	5
碳外壳	C	2.10	80—100 mm球壳层	20

DownLoad: CSV

表 2 太阳极小年³He/⁴He的参数化比例C(m)

Table 2. The parameterized ratio C(m) of ³He/⁴He in solar minimum.

E/(GeV·n^–1)	0.10 ≤ E ≤ 0.36	0.36 ≤ E ≤ 1.00	1.00 ≤ E ≤ 1.40	E > 1.40
C(m)	0.335 × E^0.569	0.187	0.187 × E^0.491	0.22

DownLoad: CSV

表 3 太阳极大年³He/⁴He的参数化比例C(M)

Table 3. The parameterized ratio C(M) of ³He/⁴He during solar maximum.

E/(GeV·n^–1)	0.10 ≤ E ≤ 0.30	0.30 ≤ E ≤ 0.80	0.80 ≤ E ≤ 2.50	E > 2.50
C(M)	0.239 × E^0.538	0.125	0.140 × E^0.496	0.22

DownLoad: CSV

表 4 太阳极小年宇宙线主要粒子仿真参数

Table 4. The main particle simulation parameters of cosmic rays during solar minimum.

粒子种类	粒子数目/个	暴露时间/s	积分通量/(cm^–2·s^–1)
Proton	700000	353.65	4.375
³He	100000	3563.35	0.062
⁴He	120000	806.26	0.329
C	100000	21052.63	0.0105
N	100000	77561.47	0.00285
O	100000	22128.79	0.00999
Ne	10000	13644.98	0.00162
Mg	10000	10476.25	0.00211
Si	10000	14542.70	0.00152
Fe	10000	19562.20	0.00113

DownLoad: CSV

表 5 太阳极大年宇宙线主要粒子仿真参数

Table 5. The main particle simulation parameters of cosmic rays during solar maximum.

粒子种类	粒子数目/个	暴露时间/s	积分通量/(cm^–2·s^–1)
Proton	700000	353.65	4.375
³He	100000	3563.35	0.062
⁴He	120000	806.26	0.329

DownLoad: CSV

表 6 1989年9月29日太阳高能粒子事件仿真参数

Table 6. Simulation parameters of the SEP event on September 29, 1989.

粒子种类	粒子数目/个	暴露时间/s	积分通量/(cm^–2·s^–1)
Proton	500000	0.150	7385.53

DownLoad: CSV

表 7 宇宙线初、次级粒子造成的充电率

Table 7. Charge rate caused by primary and secondary particles of cosmic rays.

粒子种类	初级粒子充电率/(+e·s^–1)	次级粒子充电率/(+e·s^–1)	初级粒子充电率占比
Proton	22.016	10.805	67.07%
³He	1.196	–0.029	100%
⁴He	5.125	–0.100	100%
C	0.182	0.023	88.78%
N	0.042	0.009	82.35%
O	0.123	0.020	86.01%
Ne	0.0132	0.0026	83.54%
Mg	0.0137	0.0064	68.16%
Si	0.0087	0.0058	60%
Fe	0	0.0084	0%

DownLoad: CSV

[1]	Sathyaprakash B S, Schutz B F 2009 Living Rev. Relativ. 12 1 Google Scholar
[2]	雷中华, 兰明建, 汪先友, 李建杰 2008 物理学报 57 7408 Google Scholar Lei Z H, Lan M J, Wang X Y, Li J J 2008 Acta Phys. Sin. 57 7408 Google Scholar
[3]	Jafry Y, Sumner T J, Buchman S 1996 Classical Quantum Gravity 13 A97 Google Scholar
[4]	Jafry Y, Sumner T J 1997 Classical Quantum Gravity 14 1567 Google Scholar
[5]	Sumner T J, Jafry Y 2000 Adv. Space Res. 25 1219 Google Scholar
[6]	Araújo H M, Howard A, Shaul D, Sumner T J 2003 Classical Quantum Gravity 20 S311 Google Scholar
[7]	Shaul D N A, Sumner T J, Araújo H M, Rochester G K, Wass P J, Lee C G Y 2004 Classical Quantum Gravity 21 S647 Google Scholar
[8]	Sumner T, Araújo H, Davidge D, Howard A, Lee C, Rochester G, Shaul D, Wass P 2004 Classical Quantum Gravity 21 S597 Google Scholar
[9]	Vocca H, Grimani C, Amico P, Bosi L, Marchesoni F, Punturo M, Travasso F, Barone M, Stanga R, Vetrano F, Viceré A 2004 Classical Quantum Gravity 21 S665 Google Scholar
[10]	包纲, 倪维斗, 柳磊, Araújo H, Shaul D, Sumner T 2004 紫金山天文台台刊 23 105 Bao G, Ni W T, Liu L, Araújo H, Shaul D, Sumner T 2004 Publ. Purple Mt. Observatory 23 105
[11]	Bao G, Ni W T, Shaul D N A, Araújo H M, Liu L, Sumner T J 2008 Int. J. Mod. Phys. D 17 965 Google Scholar
[12]	Grimani C, Fabi M, Lobo A, Mateos I, Telloni D 2015 Classical. Quantum Gravity. 32 035001 Google Scholar
[13]	Wass P J, Araújo H M, Shaul D N A, Sumner T J 2005 Classical. Quantum Gravity. 22 S311 Google Scholar
[14]	Armano M, Audley H, Auger G, Baird J T, Binetruy P, Born M, Bortoluzzi D, Brandt N, Bursi A, Caleno M, Cavalleri A, Cesarini A, Cruise M, Danzmann K, Silva M, Diepholz I, Dolesi R, Dunbar N, Ferraioli L, Ferroni V, Fitzsimons E D, Flatscher R, Freschi M, Gallegos J, Marirrodriga C, Gerndt R, Gesa L, Gibert F, Giardini D, Giusteri R, Grimani C, Grzymisch J, Harrison I, Heinzel G, Hewitson M, Hollington D, Hueller M, Huesler J, Inchauspé H, Jennrich O, Jetzer P, Johlander B, Karnesis N, Kaune B, Killow C J, Korsakova N, Lloro I, Liu L, López-Zaragoza J P, Maarschalkerweerd R, Madden S, Mance D, Martín V, Martin-Polo L, Martino J, Martin-Porqueras F, Mateos I, McNamara P W, Mendes J, Mendes L, Moroni A, Nofrarias M, Paczkowski S, Perreur-Lloyd M, Petiteau A, Pivato P, Plagnol E, Prat P, Ragnit U, Ramos-Castro J, Reiche J, Perez J A, Robertson D I, Rozemeijer H, Rivas F, Russano G, Sarra P, Schleicher A, Slutsky J, Sopuerta C, Sumner T J, Texier D, Thorpe J I, Trenkel C, Vetrugno D, Vitale S, Wanner G, Ward H, Wass P J, Wealthy D, Weber W J, Wittchen A, Zanoni C, Ziegler T, Zweifel P 2017 Phys. Rev. Lett. 118 171101 Google Scholar
[15]	Araújo H M, Wass P, Shaul D, Rochester G, Sumner T J 2005 Astropart. Phys. 22 451 Google Scholar
[16]	罗子人, 白姗, 边星, 陈葛瑞, 董鹏, 董玉辉, 高伟, 龚雪飞, 贺建武, 李洪银, 李向前, 李玉琼, 刘河山, 邵明学, 宋同消, 孙保三, 唐文林, 徐鹏, 徐生年, 杨然, 靳刚 2013 力学进展 43 415 Google Scholar Luo Z R, Bai S, Bian X, Chen G R, Dong P, Dong Y H, Gao W, Gong X F, He J W, Li H Y, Li X Q, Li Y Q, Liu S H, Shao M X, Song T X, Sun B S, Tang W L, Xu P, Xu S N, Yang R, Jin G 2013 Adv. Mech. 43 415 Google Scholar
[17]	Myers Z D, Seo E S, Abe K, Anraku K, Imori M, Maeno T, Makida Y, Matsumoto H, Mitchell J, Moiseev A, Nishimura J, Nozaki M, Ormes J F, Orito S, Sanuki T, Sasaki M, Shikaze Y, Streitmatter R E, Suzuki J, Tanaka K, Yamagami T, Yamamoto A, Yoshida T, Yoshimura K 2003 In International Cosmic Ray Conference Tsukuba, Japan, July 31–August 7, 2003 p1805
[18]	Wang J Z, Seo E S, Anraku K, Fujikawa M, Imori M, Maeno T, Matsui N, Matsunaga H, Motoki M, Orito S, Saeki T, Sanuki T, Ueda I, Yoshimura K, Makida Y, Suzuki J, Tanaka K, Yamamoto A, Yoshida T, Mitsui T, Matsumoto H, Nozaki M, Sasaki M, Mitchell J, Moiseev A, Ormes J, Streitmatter R, Nishimura J, Yajima Y, Yamagami T 2002 Astrophys. J. 564 244 Google Scholar
[19]	Casolino M, Santis C D, Simone N D, Formato V, Nikonov N, Picozza P 2011 Astrophys. Space Sci. Trans. 7 465 Google Scholar
[20]	Abe K, Fuke H, Haino S, Hams T, Hasegawa M, Horikoshi A, Itazaki A, Kim K C, Kumazawa T, Kusumoto A, Lee M H, Makida Y, Matsuda S, Matsukawa Y, Matsumoto K, Mitchell J W, Moiseev A A, Nishimura J, Nozaki M, Orito R, Ormes J F, Picot-Clémente N, Sakai K, Sasaki M, Seo E S, Shikaze Y, Shinoda R, Streitmatter R E, Suzuki J, Takasugi Y, Takeuchi K, Tanaka K, Thakur N, Yamagami T, Yamamoto A, Yoshida T, Yoshimura K 2014 Adv. Space Res. 53 1426 Google Scholar
[21]	Grimani C, Vocca H, Bagni G, Marconi L, Stanga R, Vetrano F, Viceré A, Amico P, Gammaitoni L, Marchesoni F 2005 Classical. Quantum Gravity. 22 S327 Google Scholar
[22]	Papini P, Grimani C, Stephens S A 1996 Il Nuovo Cim. C 19 367 Google Scholar
[23]	Grimani C, Vocca H, Barone M, Stanga R, Vetrano F, Viceré A, Amico P, Bosi L, Marchesoni F, Punturo M, Travasso F 2004 Classical. Quantum Gravity. 21 S629 Google Scholar

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Vol. 70, Issue 22 - 2021-11-20

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