LBT observations of the HR 8799 planetary system - First detection of HR 8799e in H band
LBT observations of the HR 8799 planetary system - First detection of HR 8799e in H band
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HR 8799 行星系统的 LBT 观测 - 首次在 H 波段检测到 HR 8799e
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发表时间：
2012
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通讯作者：
C. Woodward
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作者：
S. Esposito;D. Mesa;A. Skemer;C. Arcidiacono;R. Claudi;S. Desidera;R. Gratton;F. Mannucci;F. Marzari;E. Masciadri;L. Close;P. Hinz;C. Kulesa;D. McCarthy;J. Males;G. Agapito;J. Argomedo;K. Boutsia;R. Briguglio;G. Brusa;L. Busoni;G. Cresci;L. Fini;A. Fontana;J. Guerra;J. Hill;D. Miller;D. Paris;E. Pinna;A. Puglisi;F. Quirós;A. Riccardi;P. Stefanini;V. Testa;M. Xompero;C. Woodward
我们利用大双目望远镜和PISCES相机上的新AO系统对HR 8799周围的行星系统进行了H和KS波段的观测。出色的仪器性能（在H波段的Strehl比率高达80%）使最内侧的行星HR 8799 e首次被发现，这是tH波段。HR 8799 e的H和KS星等与行星c和d相似，行星e稍亮。因此，HR 8799 e的质量可能比c和d稍大。我们确认行星B、c和e的轨道是圆的且共面;行星d的轨道偏心率应该是0.1左右，或者相对于B和c是不共面的。行星e不能在圆形和共面轨道中与c和d以4：2：1的平均运动共振，而共面和圆形轨道允许5：2的共振。动力学稳定性分析表明，当B的行星质量约为5 MJ，其它行星质量约为7 MJ时，系统是高度不稳定或混沌的。当HR 8799 b、c、d、a分别采用约3.5、5、5和5 MJ的行星质量时，发现了数十万年时间尺度的动力学稳定性的重要区域。这些质量低于目前基于恒星年龄（3000万年）和亚恒星天体理论模型的估计。
We have performed H and KS band observations of the planetary system around HR 8799 using the new AO system at the Large Binocular Telescope and the PISCES Camera. The excellent instrument performance (Strehl ratios up to 80% in H band) enabled the detection of the innermost planet, HR 8799e ,a tH band for the first time. The H and KS magnitudes of HR 8799e are similar to those of planets c and d, with planet e being slightly brighter. Therefore, HR 8799e is likely slightly more massive than c and d .W e also explored possible orbital configurations and their orbital stability. We confirm that the orbits of planets b, c and e are consistent with being circular and coplanar; planet d should have either an orbital eccentricity of about 0.1 or be non-coplanar with respect to b and c. Planet e can not be in circular and coplanar orbit in a 4:2:1 mean motion resonances with c and d, while coplanar and circular orbits are allowed for a 5:2 resonance. The analysis of dynamical stability shows that the system is highly unstable or chaotic when planetary masses of about 5 MJ for b and 7 MJ for the other planets are adopted. Significant regions of dynamical stability for timescales of tens of Myr are found when adopting planetary masses of about 3.5, 5, 5, and 5 MJ for HR 8799b, c, d ,a nde respectively. These masses are below the current estimates based on the stellar age (30 Myr) and theoretical models of substellar objects.