预期中的北冕座T星爆发多信使辐射的射电成分
Radio component of the multi-messenger emission from the anticipated T Coronae Borealis outburst
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中文总结 AI 辅助
针对即将爆发的北冕座T星，通过三维模拟后处理预测其射电辐射，揭示吸收效应影响形态，并指出多频射电监测可约束星周介质与粒子加速。
中文摘要 AI 辅助
北冕座T星是最近的双星共生再发新星，预计即将发生新的爆发，这为研究激波演化和粒子加速提供了难得的机会。我们预测了爆发产生的射电辐射，并评估了射电观测如何约束星周介质（CBM）和宇宙射线加速。我们利用多区模型对三维（3D）流体动力学新星模拟进行后处理，以计算粒子加速和射电辐射，计算了热自由-自由辐射和非热同步加速辐射，包括Razin效应以及不同CBM构型下的自由-自由吸收和同步加速自吸收。早期的射电形态不应直接解释为内在激波几何结构，因为自由-自由吸收会选择性地遮蔽3D发射体积中的区域。内在射电辐射主要由前向激波处加速的电子产生的同步加速辐射主导，在第一天内，未吸收的通量在GHz频率下可达100-1000 Jy。致密的抛射物和被激波激发的CBM物质强烈吸收辐射，使可观测通量降低数个数量级。在大约一个月内，源在GHz频率下变得基本透明。在第一年内，射电辐射仍以非热辐射为主，而热辐射仅在致密的赤道增强区域变得重要。射电谱指数从由吸收引起的正值演化为数周后的约0.5的光学薄同步加速辐射值。如果红巨星的磁场对宇宙射线产生的磁场有贡献，则在最初几天内可能出现短暂的偏振信号。对即将到来的T CrB爆发的早期多频率射电监测和偏振测量将探测密度结构和磁场，检验共生再发新星中的粒子加速。
英文摘要
T Coronae Borealis is the nearest symbiotic recurrent nova and is expected to undergo a new eruption soon, offering a rare opportunity to study shock evolution and particle acceleration. We predict radio emission from the outburst and assess how radio observations can constrain the circumbinary medium (CBM) and cosmic-ray acceleration. We post-process three-dimensional (3D) hydrodynamic nova simulations with a multi-zone model for particle acceleration and radio emission, computing thermal free-free and non-thermal synchrotron radiation, including the Razin effect and free-free and synchrotron self-absorption for different CBM configurations. Early radio morphology should not be interpreted directly as the intrinsic shock geometry, because free-free absorption selectively obscures regions of the 3D emitting volume. The intrinsic radio emission is dominated by synchrotron radiation from electrons accelerated at the forward shock, with unabsorbed fluxes reaching 100-1000 Jy at GHz frequencies during the first day. Dense ejecta and shocked CBM material strongly absorb the emission, reducing the observable flux by several orders of magnitude. The source becomes largely transparent at GHz frequencies within about one month. Radio emission remains predominantly non-thermal during the first year, while thermal emission becomes important only for dense equatorial enhancements. The radio spectral index evolves from positive values caused by absorption to the optically thin synchrotron value of about 0.5 after several weeks. A short-lived polarized signal may arise during the first few days if the red giant's magnetic field contributes to the cosmic-ray-generated field. Early multi-frequency radio monitoring and polarimetry of the forthcoming T CrB eruption will probe density structure and magnetic field, testing particle acceleration in symbiotic recurrent novae.
发表机构
- INAF - Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）
- Institute for Applied Problems in Mechanics and Mathematics, National Academy of Sciences of Ukraine（乌克兰国家科学院应用力学与数学问题研究所）
- Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学系数据密集与时域天文中心）
- Dipartimento di Fisica e Chimica E. Segrè, Università degli Studi di Palermo（巴勒莫大学E. Segrè物理化学系）
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