Nucleonic gamma-ray production in Vela X
Nucleonic gamma-ray production in Vela X
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DOI：
10.1051/0004-6361:20065116
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发表时间：
2006-06
影响因子：
6.5
通讯作者：
D. Horns;F. Aharonian;A. Santangelo;A. Hoffmann;C. Masterson
中科院分区：
文献类型：
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作者：
D. Horns;F. Aharonian;A. Santangelo;A. Hoffmann;C. Masterson
上下文。最近发现的从至少三个脉冲星风星云系统(MSH15-52、G18.0-07和船帆座X)发出的扩展的甚高能伽马射线(E>；0.1TeV=10 11 eV)可能暗示了一类可能的新天体，在下文中被称为“TeV星云”。在其中一些系统中，粒子加速可能是由相对论脉冲星风中的离子驱动的。这些离子预计会通过与周围介质的非弹性散射产生伽马射线发射。目标。研究了与脉冲星PSR B0833-45有关的船帆TeV标准的伽马射线发射。我们在核子伽马射线产生的框架内计算了包括初级电子和次级电子的同步辐射和逆康普顿辐射在内的伽马射线发射，并将模型与观测数据进行了比较。结果。该模型计算的能谱很好地描述了伽马射线数据。在脉冲星风中释放的铁核所需的能量为Wp=1.3x1049(n/0.6 cm-3)-1erg(质子)和WFe≈(1048erg)。二次电子在≈10 32erg/S水平上产生从光学到软X射线的发射.我们给出了νμ和Ve中微子发射的一个预测，其中包括一个简单的νμ通量的参数化，用于计算下一代中微子望远镜的探测率.结论。观测到的伽马射线辐射可以由脉冲星风产生，脉冲星风以相对论原子核的形式携带着很大一部分自旋下降光度。我们预测中微子通量是这个模型的唯一特征。基于这一预测，船帆TeV标准将是下一代中微子望远镜最著名的探测候选者之一。
Context. The recently discovered extended very high energy gamma-ray (E > 0.1 TeV = 10 11 eV) emission from at least three pulsar wind nebula systems (MSH 15-52, G18.0-07, and Vela X) could be hinting at a possibly new class of objects which is called in the following "TeV plerions". In some of these systems, particle acceleration could be driven by ions in the relativistic pulsar wind. These ions are expected to produce gamma-ray emission via inelastic scattering with the ambient medium. Aims. The gamma-ray emission from the Vela TeV plerion associated with the pulsar PSR B0833-45 is investigated Methods. We calculate the gamma-ray emission in the framework of nucleonic gamma-ray production including the synchrotron and inverse Compton emission from primary and secondary electrons and compare the model with observational data. Results. The spectra calculated in this model give a very good description of the gamma-ray data. The required energy in nuclei is W p = 1.3 x 10 49 (n/0.6 cm -3 ) -1 erg for protons and W Fe ≈ 10 48 erg for iron nuclei released in the pulsar wind. The secondary electrons produce optical to soft X-ray emission at the level of ≈10 32 erg/s. We give a prediction for the ν μ and V e neutrino emission including a simple parameterization of the ν μ flux useful for calculating detection rates in next generation neutrino telescopes. Conclusions. The observed gamma-ray emission can be produced by a pulsar wind which carries a large fraction of the spin down luminosity in the form of relativistic nuclei. We predict the neutrino flux as a unique signature for this model. Based upon this prediction, the Vela TeV plerion would be one of the best known candidates for detection with next generation neutrino telescopes.