AI 中文总结
研究IIb型超新星SN 2025aico，通过分析早期光学光变曲线和光谱数据，利用混合模型等方法限制其爆炸参数、前身星性质等，得出其爆炸时刻、光度、\(^{56}Ni\)质量等物理性质，揭示其起源于紧凑双星系统中的中等质量剥离氦星。
AI 中文摘要
我们旨在研究IIb型超新星SN 2025aico的物理性质和潜在爆炸机制。通过对早期光学光变曲线和光谱数据的全面分析，我们旨在限制基本爆炸参数并评估该事件的物理状态。我们展示了对IIb型超新星SN 2025aico的早期多波段光学成像和低分辨率光学光谱后续观测，从爆炸起跨度约70天。我们通过利用结合激波冷却发射和放射性驱动扩散的混合模型以及分析光谱演化来限制SN 2025aico的性质。我们使用各种方法从早期数据限制\(^{56}Ni\)混合，还将我们的光谱与模型比较以限制前身星的性质。估计SN 2025aico的爆炸时刻为MJD 61032.69，而在\(r_M\)波段的上升时间为22.30±0.70天。光学波段的峰值假热光度为\(L_{opt}=(4.07±0.10)\times10^{41}erg/s\)。拟合得出中等至相对较低的\(^{56}Ni\)质量\(M_{Ni}=0.033_{-0.004}^{+0.006}M_{sun}\)和抛射质量\(M_{ej}=2.79_{-0.18}^{+0.21}M_{sun}\)。从\(Fe II\lambda5169\)线测量的热光球速度在光度峰值附近为6450±180km/s。推导的包层性质表明其前身星是一个紧凑的氦星，拥有约\(0.01M_{sun}\)的富氢包层和约6 - 10\(R_{sun}\)的半径。推导的SN 2025aico的物理性质表明它起源于一个紧凑双星系统中的中等质量剥离氦星，其特征是残留氢包层最小。爆炸本身在整个抛射中表现出弱至中等的\(^{56}Ni\)混合。
英文摘要
We aimed to investigate the physical properties and the underlying explosion mechanisms of the Type IIb SN 2025aico. Through a comprehensive analysis of early-phase optical light curves and spectroscopic data, we aim to constrain the fundamental explosion parameters and evaluate the physical state of the event. We present early multi-band optical imaging and low-resolution optical spectroscopic follow-up observations of the Type IIb SN 2025aico, spanning approximately 70 days from the explosion. We constrain the properties of SN 2025aico by utilizing a hybrid model that combines shock-cooling emission and radioactively powered diffusion, as well as by analyzing the spectroscopic evolution. We use various approaches to constrain the 56Ni mixing from early data, and also compared our spectra with models to constrain the properties of the progenitor. The explosion epoch of SN 2025aico is estimated to be MJD 61032.69, while the rise time in the r_M-band is 22.30 +/- 0.70 days. The peak pseudo-bolometric luminosity in the optical bands is L_opt = (4.07 +/- 0.10) x 10^41 erg/s. The fitting yields a moderate to relatively low 56Ni mass of M_Ni = 0.033 +0.006/-0.004 M_sun and an ejecta mass of M_ej = 2.79 +0.21/-0.18 M_sun. The photospheric velocity near the bolometric peak, measured from the Fe II lambda 5169 line, is 6450 +180/-160 km/s. The derived envelope properties suggest a compact He-star progenitor possessing an H-rich envelope of M_env approx. 0.01 M_sun and a radius of R_env approx. 6-10 R_sun. The derived physical properties of SN 2025aico indicate an origin from a moderate-mass, stripped He-star in a compact binary system, characterized by a minimal residual hydrogen envelope. The explosion itself demonstrates weak to moderate 56Ni mixing throughout the ejecta.
Comments20 pages, 14 figures, submit to Astronomy & Astrophysics
