太阳黑子变化是太阳强磁扰动的表征。结合长短期记忆单元神经网络和一维卷积神经网络预测太阳黑子变化,使用3种不同的数据集,分别为1700—2020年年均太阳黑子数(yearly mean sunspot number,YSSN)、1749—2021年月均太阳黑子数(monthly ...太阳黑子变化是太阳强磁扰动的表征。结合长短期记忆单元神经网络和一维卷积神经网络预测太阳黑子变化,使用3种不同的数据集,分别为1700—2020年年均太阳黑子数(yearly mean sunspot number,YSSN)、1749—2021年月均太阳黑子数(monthly mean sunspot number,MSSN)和1874—2021年月均太阳黑子面积(monthly mean sunspot area,MSSA)。首先,基于YSSN数据集,预测得到2021年YSSN以及第25太阳周YSSN,2025年预测值达到最大,其值为163.4;其次,基于MSSN数据集,预测得到2021年6月MSSN以及第25太阳周MSSN,2024年10月预测值达到最大,其值为245.9;接着,基于MSSA数据集,预测得到2021年6月MSSA,其值为73.1;最后,基于MSSA数据集,将纬度划分为13个分区,发现可以重建太阳黑子蝴蝶图。以上均表明神经网络方法为探测太阳黑子变化提供了新的解决思路。展开更多
According to Bohr-Sommerfeld quantization rule,an equally spaced horizon area spectrum of a static,spherically symmetric black hole was obtained under an adiabatic invariant action.This method can be extended to the r...According to Bohr-Sommerfeld quantization rule,an equally spaced horizon area spectrum of a static,spherically symmetric black hole was obtained under an adiabatic invariant action.This method can be extended to the rotating black holes.As an example,this method is applied to the rotating BTZ black hole and the quantized spectrum of the horizon area is obtained.It is shown that the area spectrum of the rotating BTZ black hole is also equally spaced and irrelevant to the rotating parameter,which is consistent with the Bekenstein conjecture.Specifically,the derivation does not need the quasinormal frequencies and the small angular momentum limit.展开更多
文摘太阳黑子变化是太阳强磁扰动的表征。结合长短期记忆单元神经网络和一维卷积神经网络预测太阳黑子变化,使用3种不同的数据集,分别为1700—2020年年均太阳黑子数(yearly mean sunspot number,YSSN)、1749—2021年月均太阳黑子数(monthly mean sunspot number,MSSN)和1874—2021年月均太阳黑子面积(monthly mean sunspot area,MSSA)。首先,基于YSSN数据集,预测得到2021年YSSN以及第25太阳周YSSN,2025年预测值达到最大,其值为163.4;其次,基于MSSN数据集,预测得到2021年6月MSSN以及第25太阳周MSSN,2024年10月预测值达到最大,其值为245.9;接着,基于MSSA数据集,预测得到2021年6月MSSA,其值为73.1;最后,基于MSSA数据集,将纬度划分为13个分区,发现可以重建太阳黑子蝴蝶图。以上均表明神经网络方法为探测太阳黑子变化提供了新的解决思路。
基金supported by the National Natural Science Foundation of China(Grant Nos.10773002,10875012 and 11175019)the Fundamental Research Funds for the Central Universities(Grant No.105116)the Team Research Program of Hubei University for Nationalities(Grant No. MY2011T006)
文摘According to Bohr-Sommerfeld quantization rule,an equally spaced horizon area spectrum of a static,spherically symmetric black hole was obtained under an adiabatic invariant action.This method can be extended to the rotating black holes.As an example,this method is applied to the rotating BTZ black hole and the quantized spectrum of the horizon area is obtained.It is shown that the area spectrum of the rotating BTZ black hole is also equally spaced and irrelevant to the rotating parameter,which is consistent with the Bekenstein conjecture.Specifically,the derivation does not need the quasinormal frequencies and the small angular momentum limit.
