发表机构
National Astronomical Observatories, Chinese Academy of Sciences; The International Centre for Theoretical Physics Asia-Pacific, University of Chinese Academy of Sciences (UCAS); Taiji Laboratory for Gravitational Wave Universe (Beijing/Hangzhou), UCAS（中国科学院国家天文台; 中国科学院大学亚太理论物理中心; 中国科学院大学太极引力波宇宙实验室（北京/杭州））
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
提出一种基于亥姆霍兹轨道和球贝塞尔通量平衡的新方法，用于生成致密双星从旋进到振铃的波形，并在GW250114和GW170817上验证了其与模型波形的匹配。
AI 中文摘要
波形是通过在延迟质量核的亥姆霍兹轨道上平衡能量与辐射得到的，其中通量采用球贝塞尔函数形式。该平衡源于具有修正顶点的狄拉克-麦克斯韦方程，其中单一的U(1)耦合被源相互作用的八个算符所取代。在接触后，该平衡表现为一个波包的能量损失：对于黑洞残骸是一个有界势阱，对于中子星残骸则是单星的库仑阶梯。振铃从该终态的球投影开始，该终态包含其自旋。比较采用已发表参数下的模型波形。对于GW250114，在库仑半径接触处并经过-16毫秒的时移后，在100-200赫兹频段内，与NRSur7dq4中位数的噪声加权范数比在已发表的距离区间内保持在1.36至1.94之间。在2.4倍该半径处停止，该比率降至1.11，同一区间内该比率从0.94变化至1.35。若将接触点置于已发表的并合时刻且无时移，则该比率在库仑半径处为3.32，在2.4倍半径处为2.30。在较大半径处，该平衡的非延迟极限（单位球贝塞尔权重）在94赫兹处达到接触，在20-100赫兹频段内，经过+27毫秒的时移后，与亥姆霍兹平衡的范数比为1.12。对于GW170817，在100赫兹附近的|h+|为8.0×10^-23，与2.5PN旋进波的失配表现为相位差。
英文摘要
The waveform is obtained from one balance of energy and radiation on Helmholtz orbits of the retarded mass kernel, with a spherical-Bessel flux. That balance follows from the Dirac--Maxwell equation with a modified vertex, the single $U(1)$ coupling being replaced by the eight operators of the source interaction. After contact that balance is the energy loss of one packet: a bounded well for a black-hole remnant and the Coulomb ladder of one star for a neutron-star remnant. Ringdown starts from the spherical projection of that end state, which contains its spin. The comparisons use model waveforms at the published parameters. For GW250114, at the Coulomb-radius contact and after a shift of $-16\,\mathrm{ms}$, the noise-weighted norm ratio against the NRSur7dq4 median in $100$--$200\,\mathrm{Hz}$ stays between $1.36$ and $1.94$ across the published distance interval. Stopping at $2.4$ times that radius lowers the ratio to $1.11$, which the same interval moves from $0.94$ to $1.35$. With contact placed on the published merger time and with no time shift, that ratio is $3.32$ at the Coulomb radius and $2.30$ at $2.4$ times that radius. At the larger radius, the unretarded limit of this balance, with unit spherical-Bessel weights, reaches contact at $94\,\mathrm{Hz}$, and in $20$--$100\,\mathrm{Hz}$ the norm ratio to the Helmholtz balance is $1.12$ after a shift of $+27\,\mathrm{ms}$. For GW170817, $|h_{+}|$ near $100\,\mathrm{Hz}$ is $8.0\times10^{-23}$, and the mismatch against the $2.5$PN inspiral is a difference in phasing.
Comments20 pages, 18 figures
