AI 中文总结
本文通过多扇区TESS测光与SED分析，结合Gaia数据研究食双星CPD-82 291，确定其轨道倾角、测光质量比等参数，推断恒星半径，探讨环双星尘埃可能性及恒星演化阶段。
AI 中文摘要
我们对食双星CPD-82 291（RX J0853.1–8244）开展了多扇区TESS测光及光谱能量分布（SED）分析。8个TESS扇区数据显示出清晰的食现象，以及显著且随时间变化的食外调制。这种不对称性可通过不同epoch的不同表面亮度构型重现，与恒星活动强烈且演化的特征一致，不过拟合的圆形区域并非单个星斑的唯一映射。采用分离双星光变曲线模型，得到轨道倾角i≈82.1°，测光质量比q_phot≈0.464。由于缺乏光谱视向速度轨道，该质量比及绝对参数为模型依赖值，而非动力学测量值。结合光变曲线几何、SED半径标度与Gaia距离，得到R₁≈1.25R☉，R₂≈3.70R☉；相应模型推断的质量远不如无量纲光变曲线参数可靠。恒星光球从光学区到WISE W4都能重现观测到的SED，无统计显著的中红外过量。唯一的长波长偏差是低显著性的60μm测量值，90μm结果为上限。冷环双星尘埃模型可重现这一试探性信号，但测光并不要求存在该成分，其推断的质量和径向范围不唯一且强依赖模型。演化轨迹显示主星接近零龄主序，次星远高于主序位置；然而，因缺乏视向速度、光谱年轻度指标，且Gaia天体测量与蝘蜓I星协成员身份不符，无法确定其前主序分类。
英文摘要
We present a multi-sector $TESS$ photometric and spectral energy distribution analysis of the eclipsing binary CPD--82~291 (RX~J0853.1--8244). Eight $TESS$ sectors reveal well-defined eclipses and substantial, changing out-of-eclipse modulation. The asymmetries are reproduced by different surface-brightness configurations at different epochs, consistent with strong and evolving stellar activity, although the fitted circular regions are not unique maps of individual starspots. A detached-binary light-curve model yields an orbital inclination of $i\simeq82.1^\circ$ and a photometric mass ratio of $q_{\rm phot}\simeq0.464$. Without a spectroscopic radial-velocity orbit, the mass ratio and absolute parameters are model-dependent rather than dynamical measurements. Combining the light-curve geometry with the SED radius scale and \textit{Gaia} distance gives $R_1\simeq1.25\,R_\odot$ and $R_2\simeq3.70\,R_\odot$; the corresponding model-inferred masses remain substantially less secure than the dimensionless light-curve parameters. The stellar photospheres reproduce the observed SED from the optical region through WISE W4, with no statistically significant mid-infrared excess. The only positive long-wavelength deviation is a low-significance $60\,μ$m measurement, while the $90\,μ$m result is an upper limit. A cool circumbinary-dust model can reproduce this tentative signal, but such a component is not required by the photometry, and its inferred mass and radial extent are non-unique and strongly model dependent. Evolutionary tracks place the primary close to the zero-age main sequence and the secondary well above the main-sequence locus. However, the absence of radial velocities and spectroscopic youth indicators, together with $Gaia$ astrometry inconsistent with Chamaeleon~I membership, prevents a secure pre-main-sequence classification.
CommentsAccepted for publication in PASP. 41 pages, 18 figures, and 6 tables
