AI中文摘要
高分辨率光谱观测揭示了He I发射线在经典TTauri星中的吸积几何结构,发现氢线无法追踪的区域。本文研究了近邻(47 pc)、宽轨道(~84 au)、~13 MJup的吸积circumbinary伴星Delorme 1 (AB)b的He I发射线,利用解析线形貌约束其起源。分析了33个高信噪比VLT/UVES光谱,覆盖近紫外到可见光波长,R~50,000。检测到7个He I线(3890, 4027, 4473, 4923, 5017, 5877, 6680 Ȧ)具有显著的epoch到epoch变化。He I 5877, 4923, 4473, 4027 Ȧ线不对称,显示接近0 km/s的窄成分和红移约15 km/s的宽成分。从中位数He I线光度推导出吸积光度(1.3+1.6-0.7×10^-5 L☉)和质量吸积率(0.7+0.9-0.4×10^-8 MJup yr^-1),与紫外过剩估计基本一致但略高。结论:Delorme 1 (AB)b的He I线形貌与经典TTauri星相似但宽度更小,三线-单线比、与紫外过剩的强相关性以及窄成分的近零红移速度表明其源于后激波区域,接近行星表面。宽成分的持续红移、线宽和与窄成分速度的相关性表明其源于激波结构,更接近激波前沿。发射似乎主要由吸积主导,但可能有色球活动贡献。
英文摘要
High-resolution spectroscopic observations of helium emission lines provide a powerful probe of accretion geometry in classical T Tauri stars, revealing regions not well traced by hydrogen lines. Parallel studies in the planetary-mass regime are lacking. In this work, we investigate helium emission from the nearby (47 pc), wide-orbit (~84 au), ~13 $M_{Jup}$ accreting circumbinary companion Delorme 1 (AB)b and use resolved line profiles to constrain their origin. We analyse 33 high-S/N VLT/UVES spectra spanning near-ultraviolet to optical wavelengths at R~50,000. We detect seven He I lines at >5$σ$ confidence - 3890, 4027, 4473, 4923, 5017, 5877, and 6680 Ȧ - with significant epoch-to-epoch variability. The He I 5877, 4923, 4473, and 4027 Ȧ lines are asymmetric, showing a narrow component near 0 km/s and a broad component redshifted by ~15 km/s. The accretion luminosity ($1.3^{+1.6}_{-0.7}\times 10^{-5} L_{\odot}$) and mass accretion rate ($0.7^{+0.9}_{-0.4} \times 10^{-8} M_{Jup} yr^{-1}$) inferred from the median He I line luminosities are broadly consistent with, but slightly higher than, estimates from the ultraviolet excess. We conclude that protoplanet Delorme 1 (AB)b shows asymmetric He I profiles analogous to those of classical T Tauri stars, but with much smaller narrow- and broad-component widths. The triplet-singlet line ratio, a strong correlation with ultraviolet excess and the near-zero, redshifted velocities obtained for the narrow component suggest that it originates within the post-shock region, close to the planet surface. The persistent redshift of the broad component, its line width, and velocity correlation with the narrow component imply an origin within the shock structure, closer to the shock front. Emission seems to be dominated by accretion based on the obtained accretion luminosities, but a contribution from chromospheric activity may be present.