The CARMENES search for exoplanets around M dwarfs The impact of rotation and magnetic fields on the radial velocity jitter in cool stars

被引：0

作者：

Ruh, H. L. ^{[1
]}

Zechmeister, M. ^{[1
]}

Reiners, A. ^{[1
]}

Nagel, E. ^{[1
]}

Shan, Y. ^{[1
,2
]}

Cifuentes, C. ^{[3
]}

Jeffers, S. V. ^{[4
]}

Tal-Or, L. ^{[1
,5
]}

Bejar, V. J. S. ^{[6
,7
]}

Amado, P. J. ^{[8
]}

Caballero, J. A. ^{[3
]}

Quirrenbach, A. ^{[9
]}

Ribas, I. ^{[10
,11
]}

Aceituno, J. ^{[12
]}

Hatzes, A. P. ^{[13
]}

Henning, Th. ^{[14
]}

Kaminski, A. ^{[9
]}

Montes, D. ^{[15
,16
]}

Morales, J. C. ^{[10
,11
]}

Schofer, P. ^{[8
]}

Schweitzer, A. ^{[17
]}

Varas, R. ^{[8
]}

机构：

[1] Georg August Univ, Inst Astrophys & Geophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany

[2] Univ Oslo, Ctr Earth Evolut & Dynam, Dept Geosci, Sem Saelands Vei 2b, N-0315 Oslo, Norway

[3] Ctr Astrobiol CSIC INTA, Campus ESAC,Camino Bajo Castillo S-N, Madrid 28692, Spain

[4] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

[5] Ariel Univ, Dept Phys, IL-40700 Ariel, Israel

[6] Inst Astrofs Canarias IAC, San Cristobal la Laguna 38200, Tenerife, Spain

[7] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Tenerife, Spain

[8] Inst Astrofis Andalucia IAA CSIC, Granada 18008, Spain

[9] Heidelberg Univ, Landessternwarte, Zentrum Astron, Konigstuhl 12, D-69117 Heidelberg, Germany

[10] CSIC, Inst Ciencies Espai ICE, Campus UAB,C Can Magrans S-N, E-08193 Barcelona, Spain

[11] Inst Estudis Espacials Catalunya IEEC, C Gran Capita 2-4, E-08034 Barcelona, Spain

[12] Observ Calar Alto, Ctr Astronon Hispano Andalucia, Sierra Filabres, E-04550 Gergal, Spain

[13] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

[14] Max Planck Inst Astron, Konigstuhl 17, Heidelberg, Germany

[15] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra & Astrofis, Madrid 28040, Spain

[16] Univ Complutense Madrid, Fac Ciencias Fis, IPARCOS UCM Inst Fis Particulas & Cosmos UCM, Madrid 28040, Spain

[17] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 692卷

基金：

以色列科学基金会;

关键词：

techniques: radial velocities; stars: activity; stars: low-mass; stars: magnetic field; stars: rotation; PLANET-SEARCH; SURFACE CONVECTION; SPECTROMETER; SIMULATIONS; VARIABILITY; PERFORMANCE; CALIFORNIA; EMISSION; CATALOG; SYSTEM;

D O I：

10.1051/0004-6361/202450836

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Radial velocity (RV) jitter represents an intrinsic limitation on the precision of Doppler searches for exoplanets that can originate from both instrumental and astrophysical sources. Aims. We aim to determine the RV jitter floor in M dwarfs and investigate the stellar properties that lead to RV jitter induced by stellar activity. Methods. We determined the RV jitter in 239 M dwarfs from the CARMENES survey that are predominantly of mid to late spectral type and solar metallicity. We also investigated the correlation between stellar rotation and magnetic fields with RV jitter. Results. The median jitter in the CARMENES sample is 3.1 m s(-1), and it is 2.3 m s(-1) for stars with an upper limit of 2 km s(-1) on their projected rotation velocities. We provide a relation between the stellar equatorial rotation velocity and RV jitter in M dwarfs based on a subsample of 129 well-characterized CARMENES stars. RV jitter induced by stellar rotation dominates for stars with equatorial rotation velocities greater than 1 km s(-1). A jitter floor of 2 m s(-1) dominates in stars with equatorial rotation velocities below 1 km s(-1). This jitter floor likely contains contributions from stellar jitter, instrumental jitter, and undetected companions. We study the impact of the average magnetic field and the distributions of magnetic filling factors on the RV jitter. We find a series of stars with excess RV jitter and distinctive distributions of magnetic filling factors. These stars are characterized by a dominant magnetic field component between 2 to 4 kG. Conclusions. An RV jitter floor can be distinguished from RV jitter induced by activity and rotation based on the stellar equatorial rotation velocity. RV jitter induced by activity and rotation primarily depends on the equatorial rotation velocity. This RV jitter is also related to the distribution of magnetic filling factors, and this emphasizes the role of the magnetic field in the generation of RV jitter.

引用

页数：13

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