发表机构
Centre for Astrophysics, University of Southern Queensland（南昆士兰大学天体物理中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究联合视向速度与Hipparcos-Gaia自行异常分析，更新了HD 65216双巨行星系统的质量与轨道参数，并模拟证明Gaia DR4数据可进一步精确约束其轨道与真实质量。
AI 中文摘要
我们提供了围绕HD 65216的行星系统的最新质量与轨道约束，该系统至少包含两颗位于偏心轨道上的巨行星。我们首先分析新的视向速度数据以约束两颗行星的周期和偏心率，然后应用Hipparcos-Gaia自行异常来约束HD 65216 c的轨道倾角。通过这一联合分析，我们发现HD 65216 c最可能处于偏心轨道（$e$ = 0.42$\pm$0.05），其周期（7007$^{+192}_{-161}$天）比先前确定的更长。自行异常与倾角的双峰分布一致，峰值位于sin$i\sim$0.5处，在假设行星共面的前提下，分别得出HD 65216 b和c的真实质量为2.23$^{+0.96}_{-0.77}$ M$_{\mathrm{J}}$和3.32$^{+1.40}_{-1.16}$ M$_{\mathrm{J}}$。最后，我们模拟了Gaia DR4历元天体测量和DR3-DR4自行异常。我们发现这些方法将足够灵敏，以进一步约束轨道参数和真实质量。
英文摘要
We provide updated mass and orbital constraints on the planetary system around HD 65216, consisting of at least two giant planets on eccentric orbits. We first analyse new RV data to constrain the periods and eccentricities of both planets, before applying the Hipparcos-Gaia proper motion anomaly to constrain the inclination of HD 65216 c. From this joint analysis, we find that HD 65216 c is most likely in an eccentric orbit ($e$ = 0.42$\pm$0.05) with a longer period (7007$^{+192}_{-161}$ days) than previously determined. The proper motion anomaly is consistent with a bimodal distribution of inclinations, with peaks at sin$i\sim$0.5, producing true masses of 2.23$^{+0.96}_{-0.77}$ M$_{\mathrm{J}}$ and 3.32$^{+1.40}_{-1.16}$ M$_{\mathrm{J}}$ for HD 65216 b and c respectively, assuming the planets are co-planar. Finally, we simulate Gaia DR4 epoch astrometry and the DR3-DR4 proper motion anomaly. We find that these methods will be sensitive enough to further constrain orbital parameters and true mass.
Comments9 pages, 8 figures, 4 tables, accepted for publication by PASA
