机构

• 计算技术研究所 [1]
• 高能物理研究所 [1]
• 沈阳自动化研究所 [1]

采集方式

• OAI收割 [3]

内容类型

• 期刊论文 [3]

发表日期

• 2020 [3]

学科主题

筛选

浏览/检索结果: 共3条，第1-3条 帮助 条数/页： 5101520253035404550556065707580859095100 排序方式： 请选择题名升序题名降序提交时间升序提交时间降序作者升序作者降序发表日期升序发表日期降序 On truthful auction mechanism for cloud resources allocation and consumption shifting with different time slots 期刊论文  OAI收割 CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE, 2020, 页码: 20 作者:  Song, Heng;  Zhu, Junwu;  Jiang, Yi   |  收藏  |  浏览/下载：25/0  |  提交时间：2021/12/01 cloud computing  mechanism design  price curve  resources allocation  time‐  of‐  use pricing   Volatility modeling and the asymmetric effect for China's carbon trading pilot market 期刊论文  OAI收割 Physica A: Statistical Mechanics and its Applications, 2020, 卷号: 542, 页码: 1-11 作者:  Fu Y(傅洋);  Zheng ZY(郑泽宇)   |  收藏  |  浏览/下载：48/0  |  提交时间：2019/12/30 Carbon emissions  Carbon price behavior  ARMA–EGARCH–SGED process  News impact curve  Asymmetric effect  Backtesting Value-at-Risk   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：68/0  |  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.