A study on the Emission Mechanism of X-ray and Gamma-rays from the pulsars

脉冲星X射线和伽马射线发射机制的研究

• 批准号: 12640229
• 负责人: SHIBATA Shinpei
• 金额: $ 0.64万
• 依托单位: Faculty of Science, Yamagata University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2000
• 资助国家: 日本
• 起止时间: 2000 至 2001
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-12640229/
• 关键词: pulsar; X-ray; gamma-ray; particle acceleration; neutron star; plasma; magnetosphere; うず糸; ガンマ線; 電場; パルス; 電子陽電子対

We presented for the first time the self-consistent model of the emitting region in high energies, for which the electric field, plasma motion, pari cration and gamma-ray emission are solved together self-consistently. It is shown that the previous belief that the electric field is screen out by the copious pair plasmas is shown to be unjustified.For the observational investigation, we discovered lots of pulsars in X-rays, e.g., PSR J0631+1036. Amongst them, the discovery of the fastest millisecond pulsar known, PSR 1937+21 has great importance. We find the main X-ray pulses coincide with the radio interpulses.We searched several SNRs for the central pulsars. Our important findings are(1) some pulsars are slow at first when they were born,and (2) pulsar nebulae shows disc and jet structure.We also observed unidentified gamma-ray sources along the milky way. We find that most of them has nebulosity indicating they are unknown pulsars. We observed some radio quiet neutron stars, which gives arise a problem on neutrons star population.We studied on vortex lines inside of the neutron star. We find that the vortex configuration with kinks is stable and yields the strongly pinned states. This suggests that pinning of a vortex line in a polycrystalline structure would still be strong enough to explain the large glitches.

本文首次提出了高能发射区的自洽模型，将电场、等离子体运动、粒子化和γ射线发射等问题自洽地统一求解。结果表明，以前认为电场是由丰富的等离子体对屏蔽掉的观点是不成立的。在观测研究中，我们发现了大量的X射线中的等离子体对，PSR J0631+1036。其中，已知最快的毫秒脉冲星PSR 1937+21的发现具有重要意义。我们发现主X射线脉冲与射电脉冲间隔相吻合，并在几个信噪比中寻找了中央射电脉冲。我们的重要发现是：（1）某些脉冲星在诞生之初是缓慢的;（2）脉冲星星云呈现出盘状和喷流结构;我们还观测到银河系沿着有不明的γ射线源。我们发现它们中的大多数都有星云状物质，表明它们是未知的恒星。我们观测到了一些射电宁静的中子星，这就引出了中子星星布居的问题，我们研究了中子星星内部的涡旋线。我们发现，具有扭结的涡旋位形是稳定的，并产生强钉扎态。这表明，多晶结构中涡旋线的钉扎仍然足以解释大的故障。

项目成果

Inoue, H. et al.: "Analytie Studies on the Structure and Emission of the SS433 Jots"Pub.Astron.Soc.Japan. 53. 127-132 (2001)

Inoue, H. 等人：“SS433 Jots 结构和发射的分析研究”Pub.Astron.Soc.Japan。

Luo Q, Shibata S., Melrose D.: "High-energy emission from millisecond pulsars: Polar cap models"Mon. Not. Rastr. Soc.. 318. 943-951 (2000)

罗庆，Shibata S.，Melrose D.：“毫秒脉冲星的高能发射：极冠模型”

Mineo T., Cusumano G., Kuiper L., Hermsen W., Massaro E., Becker W., Nicastro L., Sacco B., Verbunt F., Lyne, A. G., Stairs I. H., Shibata, S.: "The pulse shape and spectrum of the millisecond pulsar PSR J0218+4232 in the energy band 1-10 keV observed wit

Mineo T.、Cusumano G.、Kuiper L.、Hermsen W.、Massaro E.、Becker W.、Nicastro L.、Sacco B.、Verbunt F.、Lyne, A. G.、Stairs I. H.、Shibata, S.：“

Torii, K.; Kohmura, T.; Yokogawa, J.; Koyama, K.: "AX J0057.4-7325 and SMC X-2"LAUC. 7441 (2000)

鸟居，K.；

Takahashi, M. et al.: "Pulsed X-ray Emission from the Fastest Millisecond Pulsar PSR B1937+21 with ASCA"Astrophysical Journal. 554. 316-321 (2001)

Takahashi, M. 等人：“ASCA 最快毫秒脉冲星 PSR B1937 21 的脉冲 X 射线发射”天体物理学杂志。