论文标题
建模H $α$和HE 10830 WASP-52B的传输频谱
Modeling H$α$ and He 10830 transmission spectrum of WASP-52b
论文作者
论文摘要
通过$α$，h $α$的过量吸收和He Triplet（10830 $ \rmå$）线的过量吸收来检测到逃脱的气氛。同时对H $α$的吸收进行建模，而He 10830线可以提供有关外球星氛围的有用限制。在本文中，我们使用了与非本地热力学模型和新的蒙特卡洛模拟模型相结合的流体动力模型，以获得H（2）和He（2 $^3 $ s）种群。使用球形恒星LY $α$辐射的假设进行的蒙特卡洛模拟进行了LY $α$辐射转移，这是第一次计算ly $α$平均强度分布在行星内部内的ly $α$平均强度分布，这对于估计H（2）人群所必需。我们在Hot Jupiter Wasp-52b中同时对H $α$的传输光谱和10830线进行建模。我们发现，如果主机恒星具有（1）高X射线/极端紫外线（XUV）通量（$ f _ {\ rm Xuv} $），则可以很好地重现H/HA/HA的比率的模型，可以很好地重现H $α$的观察结果。 $β_M$。 He 10830 $ \rmå$三重态的模拟表明，需要高H/H/HE比率（$ \ sim $ 98/2）才能适应观察。符合这两条线的模型限制$ f _ {\ rm Xuv} $，约为基准价值的0.5倍，$β_M$的值约为0.3左右。这些模型还表明，氢和氦气源于逃避的气氛，质量损失率约为2.8 $ \ times 10^{11} $ g s $^{ - 1} $。
Escaping atmosphere has been detected by the excess absorption of Ly$α$, H$α$ and He triplet (10830$\rmÅ$) lines. Simultaneously modeling the absorption of the H$α$ and He 10830 lines can provide useful constraints about the exoplanetary atmosphere. In this paper, we use a hydrodynamic model combined with a non-local thermodynamic model and a new Monte Carlo simulation model to obtain the H(2) and He(2$^3$S) populations. The Monte Carlo simulations of Ly$α$ radiative transfer are performed with assumptions of a spherical stellar Ly$α$ radiation and a spherical planetary atmosphere, for the first time, to calculate the Ly$α$ mean intensity distribution inside the planetary atmosphere, necessary in estimating the H(2) population. We model the transmission spectra of the H$α$ and He 10830 lines simultaneously in hot Jupiter WASP-52b. We find that models with many different H/He ratios can reproduce the H$α$ observations well if the host star has (1) a high X-ray/extreme ultraviolet (XUV) flux ($F_{\rm XUV}$) and a relatively low X-ray fraction in XUV radiation ($β_m$), or (2) a low $F_{\rm XUV}$ and a high $β_m$. The simulations of He 10830 $\rmÅ$ triplet suggest that a high H/He ratio ($\sim$ 98/2) is required to fit the observation. The models that fit both lines well confine $F_{\rm XUV}$ to be about 0.5 times the fiducial value and $β_m$ to have a value around 0.3. The models also suggest that hydrogen and helium originate from the escaping atmosphere, and the mass-loss rate is about 2.8$\times 10^{11}$ g s$^{-1}$.
