The CARMENES search for exoplanets around M dwarfs: Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star
The CARMENES search for exoplanets around M dwarfs: Wolf 1069 b: Earth-mass planet in the habitable zone of a nearby, very low-mass star
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CARMENES 搜索 M 矮星周围的系外行星： Wolf 1069 b：位于附近一颗质量极低的恒星的宜居带中的地球质量行星
DOI：
10.1051/0004-6361/202245322
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发表时间：
2023
影响因子：
6.5
通讯作者：
Fauchez, T. J.
中科院分区：
文献类型：
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作者：
Kossakowski, D.;Kürster, M.;Trifonov, T.;Henning, Th.;Kemmer, J.;Caballero, J. A.;Burn, R.;Sabotta, S.;Crouse, J. S.;Fauchez, T. J.
我们发现了一颗地球质量的行星（Mbsini= 1.26±0.21M⊕），它在相对较近（d ~9.6 pc）和低质量（0.167±0.011M⊙）M5.0 V恒星Wolf 1069的15.6 d轨道上运行。Wolf 1069 b与主星的距离为0.0672±0.0014 au，位于宜居带（HZ），接收到的入射通量为s = 0.652±0.029S⊕。行星信号是使用CARMENES光谱仪的大地校正径向速度（RV）数据检测到的，总共进行了262次光谱观测，历时近四年。rv中还有额外的长周期信号，其中一个我们归因于恒星的自转周期。这要归功于我们的光度分析，包括利用OSN和TJO设施进行的新的、采样良好的监测活动，以补充档案光度测定（即来自地球和超级wasp），这产生了更新的旋转周期范围prot = 150-170 d，可能值为169.3−3.6+3.7。CARMENES光谱提供的恒星活动指标同样证明了缓慢自转周期的证据，尽管由于信号混叠或斑点演化等可能的因素而不那么准确。我们的可探测性极限表明，可以排除比地球质量大一倍、轨道周期小于10天的其他行星，这表明Wolf 1069 b可能有一个剧烈的形成历史。这颗行星也是继比邻星b、GJ 1061 d、蒂加登星c、GJ 1002 b和c之后，位于保守HZ的第六颗距离地球质量最近的行星。尽管没有凌日，Wolf 1069 b仍然是未来三维气候模型的一个非常有希望的目标，可以用来研究各种宜居性案例，以及用于亚m s - 1RV运动，以寻找潜在的亚地球质量内部行星，以测试行星形成理论。
We present the discovery of an Earth-mass planet (Mbsini= 1.26 ± 0.21M⊕) on a 15.6 d orbit of a relatively nearby (d ~9.6 pc) and low-mass (0.167 ± 0.011M⊙) M5.0 V star, Wolf 1069. Sitting at a separation of 0.0672 ± 0.0014 au away from the host star puts Wolf 1069 b in the habitable zone (HZ), receiving an incident flux ofS= 0.652 ± 0.029S⊕. The planetary signal was detected using telluric-corrected radial-velocity (RV) data from the CARMENES spectrograph, amounting to a total of 262 spectroscopic observations covering almost four years. There are additional long-period signals in the RVs, one of which we attribute to the stellar rotation period. This is possible thanks to our photometric analysis including new, well-sampled monitoring campaigns undergone with the OSN and TJO facilities that supplement archival photometry (i.e., from MEarth and SuperWASP), and this yielded an updated rotational period range ofProt= 150–170 d, with a likely value at 169.3−3.6+3.7. The stellar activity indicators provided by the CARMENES spectra likewise demonstrate evidence for the slow rotation period, though not as accurately due to possible factors such as signal aliasing or spot evolution. Our detectability limits indicate that additional planets more massive than one Earth mass with orbital periods of less than 10 days can be ruled out, suggesting that perhaps Wolf 1069 b had a violent formation history. This planet is also the sixth closest Earth-mass planet situated in the conservative HZ, after Proxima Centauri b, GJ 1061 d, Teegarden’s Star c, and GJ 1002 b and c. Despite not transiting, Wolf 1069 b is nonetheless a very promising target for future three-dimensional climate models to investigate various habitability cases as well as for sub-m s−1RV campaigns to search for potential inner sub-Earth-mass planets in order to test planet formation theories.