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CARMENES 对 M 矮星周围系外行星的搜寻：极低质量恒星周围类地行星的出现率

The CARMENES search for exoplanets around M dwarfs. Occurrence rates of Earth-like planets around very low-mass stars

A. Kaminski, S. Sabotta, J. Kemmer, P. Chaturvedi, R. Burn, J. C. Morales, J. A. Caballero, I. Ribas, A. Reiners, A. Quirrenbach, P. J. Amado, V. J. S. Béjar, S… 展开作者

A. Kaminski, S. Sabotta, J. Kemmer, P. Chaturvedi, R. Burn, J. C. Morales, J. A. Caballero, I. Ribas, A. Reiners, A. Quirrenbach, P. J. Amado, V. J. S. Béjar, S. Dreizler, E. W. Guenther, A. P. Hatzes, Th. Henning, M. Kürster, D. Montes, E. Nagel, E. Pallé, V. Pinter, S. Reffert, M. Schlecker, Y. Shan, T. Trifonov, M. R. Zapatero Osorio, M. Zechmeister

备注：
Number of pages: 25; number of figures: 23 (12 in main + 11 in appendix). Accepted in A&A; DOI (pending): 10.1051/0004-6361/202453381 (Volume 696, Article number A101)
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AI总结：

本文利用 CARMENES 视向速度数据研究 15 颗极低质量 M 矮星周围行星出现率，发现四颗新行星，并揭示低质量恒星更倾向于拥有短周期、低质量行星，证实出现率随恒星质量变化。

摘要：

目的：此前对 CARMENES 巡天中行星出现率的估计表明，质量低于 0.34 M⊙ 的 M 矮星在短周期轨道上拥有更多行星。本文聚焦于该巡天中质量最低的恒星样本，包括 15 颗质量低于 0.16 M⊙ 的非活跃目标。方法：为修正探测偏差，我们确定了单个目标及整个样本的探测灵敏度图。利用蒙特卡洛模拟，我们估计了轨道周期为 1 天至 100 天、最小质量为 0.5 M⊕ 至 10 M⊕ 的行星出现率。结果：来自 CARMENES 的视向速度（RV）数据揭示了样本中三颗恒星周围的四颗新行星，即 G 268–110 b、G 261–6 b 和 G 192–15 b 与 c。三颗 b 行星的最小质量为 1.03–1.52 M⊕，轨道周期为 1.43–5.45 天，而 G 192–15 c 是一颗 14.3 M⊕ 的行星，位于宽幅偏心轨道上，P ≈ 1218 天，e ≈ 0.68。我们的出现率结果表明其与恒星质量存在显著依赖关系。对于质量低于 3 M⊕ 的行星，我们发现在所有研究的周期范围内出现率与每颗恒星一颗行星一致，但对于质量高达 10 M⊕ 的更大质量行星，出现率几乎下降了一个数量级。与先前研究相比，低质量恒星倾向于拥有更多 P < 10 天的行星。我们还证明，基于标准核心吸积情景的合成行星族群预测的行星质量略大且轨道更宽，与观测结果不符。结论：我们的发现证实，即使在 M 矮星内部，行星出现率也随恒星质量变化，因为与质量更大的 M 矮星相比，我们在极低质量恒星子样本中发现了更多质量更低、轨道更短的行星。因此，我们强调未来研究中有必要进行更细致的区分。

英文摘要：

Aims: Previous estimates of planet occurrence rates in the CARMENES survey indicated increased numbers of planets on short orbits for M dwarfs with masses below 0.34\,M$_\odot$. Here we focused on the lowest-mass stars in the survey, comprising 15 inactive targets with masses under 0.16\,M$_\odot$. Methods: To correct for detection biases, we determined detection sensitivity maps for individual targets and the entire sample. Using Monte Carlo simulations, we estimated planet occurrence rates for orbital periods of 1\,d to 100\,d and minimum masses from 0.5\,M$_\oplus$ to 10\,M$_\oplus$. Results: The radial velocity (RV) data from CARMENES reveal four new planets around three stars in our sample, namely G~268--110\,b, G~261--6\,b, and G~192--15\,b and c. All three b planets have minimum masses of 1.03--1.52\,M$_\oplus$ and orbital periods of 1.43--5.45\,d, while G~192--15\,c is a 14.3\,M$_\oplus$ planet on a wide, eccentric orbit with $P \approx 1218$\,d and $e \approx 0.68$. Our occurrence rates suggest considerable dependencies with respect to stellar masses. For planets below 3\,M$_\oplus$ we found rates consistent with one planet per star across all investigated periods, but the rates decrease almost by an order of magnitude for larger planet masses up to 10\,M$_\oplus$. Compared to previous studies, low-mass stars tend to harbor more planets with $P <10$\,d. We also demonstrate that synthetic planet populations based on the standard core accretion scenario predict slightly more massive planets on wider orbits than observed. Conclusions: Our findings confirm that planet occurrence rates vary with stellar masses even among M dwarfs, as we found more planets with lower masses and on shorter orbits in our subsample of very low-mass stars compared to more massive M dwarfs. Therefore, we emphasize the need for additional differentiation in future studies.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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