The recent data on cosmic ray positron flux measured near the Earth by the Alpha Magnetic Spectrometer (AMS-02) experiment extends to TeV energy. The recently observed data by AMS-02 clearly confirms that the positron flux rises with energy and shows a peak near a few hundred GeV. This rising positron flux cannot be explained by interactions of cosmic rays with interstellar hydrogen gas. Pulsars, dark matter and many other innovative physical scenarios have been studied to explain this rising of the positron flux, also known as positron excess. In this paper, our goal is to study whether secondary production due to cosmic ray interactions in nearby Galactic Molecular Clouds (GMCs) can contribute significantly to the observed positron spectrum on Earth. Due to the progress in multi-wavelength astronomy, many new GMCs have been discovered in our Galaxy recently. Using large scale CO survey, 1064 GMCs were detected in the Galaxy, which reside in the Galactic plane. Alongside that, very recent survey implemented the optical/IR dust extinction measurements, to trace 567 GMCs within 4 kpc of Earth, also residing in the Galactic plane. We use the updated list of GMCs reported in recent papers, which are distributed in the Galactic plane, to find the secondary positrons produced in them in interactions of cosmic rays with molecular hydrogen. Moreover, by analyzing the Fermi-LAT data, new GMCs have been discovered near the Galactic plane. We also include some of these GMCs closest to the Earth where cosmic ray interactions are producing secondaries. It has been speculated earlier that cosmic rays may be reaccelerated in some GMCs. We select 7 GMCs out of 567 GMCs recently reported, within 4 kpc of Earth, where reacceleration due to magnetized turbulence is assumed. We include a small hardened component of secondary positrons, produced from interaction of reaccelerated CRs in those 7 GMCs. We use publicly available code DRAGON for our simulation setup to study CR propagation in the Galaxy and show that the observed positron spectrum can be well explained in the energy range of 1 to 1000 GeV by our self consistent model.

Alpha电磁谱仪在地球附近测得的宇宙射线正电子通量的最新数据（AMS-02）实验扩展到TeV能量。AMS-02最近观察到的数据清楚地证实了正电子通量随能量的增加而上升，并在几百个GeV附近出现一个峰值。正电子通量的上升无法用宇宙射线与星际氢气的相互作用来解释。已经研究了脉冲星，暗物质和许多其他创新的物理情况，以解释正电子通量（也称为正电子过量）上升的原因。在本文中，我们的目标是研究由于附近银河分子云（GMC）中的宇宙射线相互作用而引起的二次生产是否可以对地球上观察到的正电子光谱做出重大贡献。由于多波长天文学的进步，最近在我们的银河系中发现了许多新的GMC。使用大规模一氧化碳调查，在银河系中发现了1064个GMC，居住在银河系飞机上。除此之外，最近的一项调查还实施了光学/红外消光测量，以追踪同样位于银河平面内的地球4 kpc内的567个GMC。我们使用在最近的论文中报道的GMC的更新列表（分布在银河平面中）来查找宇宙射线与分子氢相互作用时在其中产生的次级正电子。此外，通过分析Fermi -LAT数据显示，在银河系飞机附近发现了新的GMC。我们还包括其中一些离地球最近的GMC，宇宙射线相互作用在这些GMC中产生次级。早先有人推测宇宙射线可能会在某些GMC中重新加速。我们在最近报告的567个GMC中选择了7个GMC，它们位于地球4 kpc内，其中假定了由于磁化湍流而产生的加速。我们包括次级正电子的少量硬化成分，该成分是由这7个GMC中加速CR相互作用产生的。我们使用可公开获得的代码DRAGON作为我们的仿真设置，以研究银河中的CR传播，并表明，通过我们的自洽模型，可以在1至1000 GeV的能量范围内很好地解释观察到的正电子光谱。