在本文中，我們嘗試估計脈衝星探測伽馬射線資源管理器（GRX）.GRX是一種軟伽瑪射線望遠鏡，預計於2020年執行衛星任務，有3次成功升空氣球在過去的十年。GRX具有良好的空間和能量分辨率，可以做的很好康普頓事件的重建，幫助我們探索軟伽瑪射線天體物理目標. 對於數據分析，GRX使用最大期望最大化（MLEM）算法來提高成像性能。我們的結論是GRX具有12.7個標準差在（L，B）=（0135）為5分鐘的曝光和大於10個標準差在（L，B）=（0,180），對於百萬電子伏特範圍蟹星雲<1分鐘。我們還對Vela脈衝星具有7.9個標準差在（L，B）=（0,180）在1天的觀察，和對於0.005蟹狀星雲通量在（L, B）=（0,180）位置有8.7個標準差，在2天的觀察。該結果比GRX的原型於2009年氣球飛行更好的在6個標準差6小時暴露。

In this thesis, we try to estimate the pulsar detection of Gamma Ray Explorer (GRX). GRX is a soft gamma-ray telescope, which is expected on satellite mission in 2020, with 3 times successful balloon launch in past decade. GRX has good spatial and energy resolution, which can do well Compton event reconstruction, to help us explore soft gamma-ray astrophysics objects. For data analysis, GRX use Maximum Likelihood Expectation Maximization (MLEM) algorithm to improve imaging property. We conclude that GRX has 12.7 sigma detection at (l,b)=(0,135) with a 5 minute exposure and > 10 sigma detection at (l,b)=(0,180) with 1 < minute for Crab nebula in MeV range. We also present Vela pulsar has 7.9 sigma detection at (l,b)=(0,180) in 1-day observation, and 8.7 sigma detection for 0.005 Crab flux at (l,b)=(0,180) in a 2-day observation. The results are much better than prototype balloon flight of GRX in 2009 with 6 sigma detection in 6 hours exposure time.

1 Introduction 11
1.1 Gamma ray line source
1.1.1 Nucleosynthesis
1.1.2 Positron annihilation
1.2 Gamma-ray Continuum Sources
1.2.1 Active Galactic Nuclei
1.2.2 Stellar-mass compact objects
1.2.3 Gamma-ray bursts
1.3 Gamma-ray interactions in matter
1.3.1 Photoelectric Absorption
1.3.2 Rayleigh Scattering
2 Gamma ray emission from MeV pulsars
3 Overview of Gamma-Ray Explorer
4 Estimate of MeV Pulsar detection

[1] Mahoney, W. A., et al. 1984, ApJ, 286,15
[2] Kurfess, J. D., et al. 1992. ApJ, 399, L137
[3] Morris, D. J., et al. 1994, A&AS,185,762
[4] Weidenspointner, G., et al. 2008. Nature, 451,159
[5] Robley, D. Evans. 1965. The Atomic Nucleus. McGraw-Hill
[6] Klein, O., Nishina, T. 1929. Z. Phys., 52,853
[7] Mahoney, W. A., Ling, J. C., Jacobson, A. S., Tapphorn, R. M. 1980.
Nucl. Instrum. Methods Phys. Res. A, 178,363
[8] Kanbach, G., et al. 1989. Space Sci. Rev.,49,69
[9] Halloin, H., et al. 2003. Nucl. Instrum. Methods Phys. Res. A, 504,120
[10] Gold, T. 1968. Nature,218,731
[11] Gunn, J. E., Ostriker, J. P. 1969. Nature, 221,454