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The Wide Field Monitor onboard the Chinese-European X-ray mission eXTP 期刊论文  OAI收割
SPACE TELESCOPES AND INSTRUMENTATION 2022: ULTRAVIOLET TO GAMMA RAY, 2022, 卷号: 12181, 页码: 121811Y
作者:  
eXTP
  |  收藏  |  浏览/下载:4/0  |  提交时间:2023/11/09
High energy Millihertz quasi-periodic oscillations in 1A 0535+262 with Insight-HXMT challenge current models 期刊论文  OAI收割
Monthly Notices of the Royal Astronomical Society, 2022, 卷号: 517, 期号: 2, 页码: 1988-1999
作者:  
HXMT
  |  收藏  |  浏览/下载:1/0  |  提交时间:2023/11/09
Detection of a quasi-periodic oscillation at 40 mHz in Cen X-3 with Insight-HXMT 期刊论文  OAI收割
Monthly Notices of the Royal Astronomical Society, 2022, 卷号: 516, 期号: 4, 页码: 5579
作者:  
Liu, Q.;  Wang, W.;  Chen, X.;  Yang, W.;  Lu, F. J.
  |  收藏  |  浏览/下载:2/0  |  提交时间:2023/11/10
Pulsar Glitches: A Review 期刊论文  OAI收割
UNIVERSE, 2022, 卷号: 8, 期号: 12, 页码: 641
作者:  
Zhou, SQ;  Guegercinoglu, E;  Yuan, JP;  Ge, MY;  Yu, C
  |  收藏  |  浏览/下载:0/0  |  提交时间:2023/11/13
Timing analysis of 2S 1417-624 observed with NICER and Insight-HXMT 期刊论文  OAI收割
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2020, 卷号: 491, 期号: 2, 页码: 1851-1856
作者:  
Ji, L.;  Doroshenko, V;  Santangelo, A.;  Gungor, C.;  Zhang, S.
  |  收藏  |  浏览/下载:20/0  |  提交时间:2020/10/19
Switches between accretion structures during flares in 4U 1901+03 期刊论文  OAI收割
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2020, 卷号: 493, 期号: 4, 页码: 5680-5692
作者:  
Ji, L.;  Ducci, L.;  Santangelo, A.;  Zhang, S.;  Suleimanov, V
  |  收藏  |  浏览/下载:32/0  |  提交时间:2020/10/19
The braking index of PSR B0540-69 and the associated pulsar wind nebula emission after spin-down rate transition 期刊论文  OAI收割
Monthly Notices of the Royal Astronomical Society, 2020, 卷号: 494, 页码: 1865-1870
作者:  
HXMT
  |  收藏  |  浏览/下载:39/0  |  提交时间:2022/02/08
stars: magnetic field  stars: neutron  pulsars: general  Astrophysics  - High Energy Astrophysical Phenomena  Abstract: In 2011 December, PSR B054-69 experienced a spin-down rate transition (SRT), after which the spin-down power of the pulsar increased by $\sim 36{{\ \rm per\ cent}}$. About 1000 d after the SRT, the X-ray luminosity of the associated pulsar wind nebula (PWN) was found to brighten by $32\pm 8{{\ \rm per\ cent}}$. After the SRT, the braking index n of PSR B0540-69 changes from n = 2.12 to 0.03 and then keeps this value for about five years before rising to n = 0.9 in the following years. We find that most of the current models have difficulties in explaining the measured braking index. One exceptive model of the braking index evolution is the increasing dipole magnetic field of PSR B0540-69. We suggest that the field increase may result from some instabilities within the pulsar core that enhance the poloidal component at the price of toroidal component of the magnetic field. The increasing dipole magnetic field will result in the X-ray brightening of the PWN. We fit the PWN X-ray light curve by two models: one assumes a constant magnetic field within the PWN during the brightening and the other assumes an enhanced magnetic field proportional to the energy density of the PWN. It appears that the two models fit the data well, though the later model seems to fit the data a bit better. This provides marginal observational evidence that magnetic field in the PWN is generated by the termination shock. Future high-quality and high-cadence data are required to draw a solid conclusion.  
Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity 期刊论文  OAI收割
Monthly Notices of the Royal Astronomical Society, 2020, 卷号: 497, 页码: 5498-5506
作者:  
HXMT
  |  收藏  |  浏览/下载:36/0  |  提交时间:2022/02/08
stars: neutron  pulsars: individual: Swift J0243.6+6124  X-rays:  binaries  Astrophysics - High Energy Astrophysical Phenomena  Abstract: Based on Insight-HXMT data, we report on the pulse fraction evolution during the 2017-2018 outburst of the newly discovered first Galactic ultraluminous X-ray (ULX) source Swift J0243.6+6124. The pulse fractions of 19 observation pairs selected in the rising and fading phases with similar luminosity are investigated. The results show a general trend of the pulse fraction increasing with luminosity and energy at supercritical luminosity. However, the relative strength of the pulsation between each pair evolves strongly with luminosity. The pulse fraction in the rising phase is larger at luminosity below 7.71 × 1038 erg s-1, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomenon is first confirmed by Insight-HXMT observations and we speculate that it may have relation with the radiation-pressure-dominated accretion disc.  
Long-term evolutions of the cyclotron line energies in her x-1, vela x-1, and cen x-3 as observed with swift/bat 期刊论文  iSwitch采集
Monthly notices of the royal astronomical society, 2019, 卷号: 484, 期号: 3, 页码: 3797-3805
作者:  
Ji, L.;  Staubert, R.;  Ducci, L.;  Santangelo, A.;  Zhang, S.
收藏  |  浏览/下载:64/0  |  提交时间:2019/04/22
Long-term evolutions of the cyclotron line energies in her x-1, vela x-1, and cen x-3 as observed with swift/bat 期刊论文  iSwitch采集
Monthly notices of the royal astronomical society, 2019, 卷号: 484, 期号: 3, 页码: 3797-3805
作者:  
Ji, L.;  Staubert, R.;  Ducci, L.;  Santangelo, A.;  Zhang, S.
收藏  |  浏览/下载:64/0  |  提交时间:2019/04/22