论文标题
探测具有多云和圆盘模型的潮汐破坏事件IPTF16AXA
Probing the tidal disruption event iPTF16axa with CLOUDY and disc-wind models
论文作者
论文摘要
我们介绍了有关潮汐破坏事件（TDE）IPTF16AXA光谱线的光学/紫外线发射连续性和多云建模的圆盘模型，以了解影响TDE的线路亮度的大气的盘状发射以及大气的性质。假设由于圆盘超级 - 埃德丁顿阶段引起的风向/紫外线发射，我们使用具有恒定速度的球形风稳定的结构化圆盘模型，以适应多天的观测。提取的参数为恒星质量$ m _ {\ star} = 6.20 \ pm 1.19 m _ {\ odot} $，盘辐射效率$ \ log _ {\ rm 10}（η）（η）= -1.22 10^{14}〜{\ rm cm} $和速度$ v_w = 18999.4 \ pm 1785.1〜 {\ rm km〜s^{ - 1}} $。风发射的光球温度为$ \ sim 2 \ times 10^4〜 {\ rm k} $，光盘单个黑体温度为$ \ sim 0.995 \ times 10^5〜 {\ rm k} $。我们还执行多云的建模来解释观察到的HE和H线发光度，这些发光性估计了风内半径$ r_l = 7.07 \ times 10^{14}〜{\ rm cm} $和速度$ v_w = 1.3 \ times 10^4〜 {\ rm km〜s^s^{\ rm km〜s^{-1}} $。使用多云和圆盘模型对IPTF16AXA的独立分析显示出与观察结果一致的可比结果。多云的建模发现，HE的超太阳丰度和较小的He II线光学深度都造成了H $α$线亮度上He II线的发光度的提高。 He II的超极性与相对较大的恒星质量一致，并表明破坏的恒星可能是一个红色的巨人。
We present both a disc-wind model on the optical/UV emission continuum and CLOUDY modelling on the spectral lines of the tidal disruption event (TDE) iPTF16axa to understand the disc-wind emission and the properties of the atmosphere that impacts the line luminosity of the TDE. Assuming the optical/UV emission from the wind due to the disc super-Eddington phase, we use the steady structured disc-wind model with a spherical wind with constant velocity to fit the observations on multiple days. The extracted parameters are stellar-mass $M_{\star} = 6.20 \pm 1.19 M_{\odot}$, disc radiative efficiency $\log_{\rm 10}(η) = -1.22 \pm 1.327$, wind inner radius $r_l = (2.013 \pm 0.551) \times 10^{14}~{\rm cm}$ and velocity $v_w = 18999.4 \pm 1785.1 ~{\rm km~s^{-1}}$. The photosphere temperature for wind emission is $ \sim 2 \times 10^4~{\rm K}$ and the disc single blackbody temperature is $\sim 0.995 \times 10^5~{\rm K}$. We also perform CLOUDY modelling to explain the observed He and H line luminosities that estimate a wind inner radius $r_l = 7.07 \times 10^{14}~{\rm cm}$ and velocity $v_w = 1.3 \times 10^4~{\rm km~s^{-1}}$. The independent analyses of iPTF16axa using CLOUDY and disc-wind models show comparable results that agree with observations. The CLOUDY modelling finds that both the super solar abundance of He and a smaller He II line optical depth is responsible for the enhancement of He II line luminosity over the H$α$ line luminosity. The super-solar abundance of He II agrees with a relatively large stellar mass and suggests that the disrupted star might have been a red giant.
