The CARMENES search for exoplanets around M dwarfs Radial-velocity variations of active stars in visual-channel spectra

被引：56

作者：

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

Zechmeister, M. ^{[1
]}

Reiners, A. ^{[1
]}

Jeffers, S., V ^{[1
]}

Schoefer, P. ^{[1
]}

Quirrenbach, A. ^{[2
]}

Amado, P. J. ^{[3
]}

Ribas, I ^{[4
,5
]}

Caballero, J. A. ^{[6
]}

Aceituno, J. ^{[3
,7
]}

Bauer, F. F. ^{[1
]}

Bejar, V. J. S. ^{[8
,9
]}

Czesla, S. ^{[10
]}

Dreizler, S. ^{[1
]}

Fuhrmeister, B. ^{[10
]}

Hatzes, A. P. ^{[11
]}

Johnson, E. N. ^{[1
]}

Kuerster, M. ^{[12
]}

Lafarga, M. ^{[4
,5
]}

Montes, D. ^{[13
,14
]}

Morales, J. C. ^{[4
,5
]}

Reffert, S. ^{[2
]}

Sadegi, S. ^{[2
]}

Seifert, W. ^{[2
]}

Shulyak, D. ^{[1
]}

机构：

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

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

[3] CSIC, IAA, Glorieta Astron S-N, E-18008 Granada 18008, Spain

[4] CSIC, ICE, Campus UAB,C Can Magrans S-N, Barcelona 08193, Spain

[5] IEEC, Barcelona 08034, Spain

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

[7] CSIC, Ctr Astron Hispano Aleman, MPG, Observ Astro Calar Alto, Gergal 04550, Almeria, Spain

[8] Inst Astrofis Canarias, Via Lactea S-N, Tenerife 38205, Spain

[9] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

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

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

[12] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[13] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra & Astrofis, E-28040 Madrid 28040, Spain

[14] Univ Complutense Madrid, Fac Ciencias Fis, UPARCOS, Unidad Fis Particulas & Cosmos, E-28040 Madrid 28040, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 614卷

关键词：

stars: late-type; stars: activity; stars: rotation; techniques: radial velocities; H-ALPHA EMISSION; PLANET; ROTATION; JITTER;

D O I：

10.1051/0004-6361/201732362

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Previous simulations predicted the activity-induced radial-velocity (RV) variations of M dwarfs to range from similar to 1 cm s(-1) to similar to 1 km s(-1), depending on various stellar and activity parameters. Aims. We investigate the observed relations between RVs, stellar activity, and stellar parameters of M dwarfs by analyzing CARMENES high-resolution visual-channel spectra (0.5-1 mu m), which were taken within the CARMENES RV planet survey during its first 20 months of operation. Methods. During this time, 287 of the CARMENES-sample stars were observed at least five times. From each spectrum we derived a relative RV and a measure of chromospheric Ha emission. In addition, we estimated the chromatic index (CRX) of each spectrum, which is a measure of the RV wavelength dependence. Results. Despite having a median number of only 11 measurements per star, we show that the RV variations of the stars with RV scatter of >10 m s(-1) and a projected rotation velocity upsilon sin i > 2 km s(-1) are caused mainly by activity. We name these stars "active RV-loud stars" and find their occurrence to increase with spectral type: from similar to 3% for early-type M dwarfs (M0.0-2.5 V) through similar to 30% for mid-type M dwarfs (M3.0-5.5 V) to >50% for late-type M dwarfs (M6.0-9.0 V). Their RV-scatter amplitude is found to be correlated mainly with upsilon sin i. For about half of the stars, we also find a linear RV-CRX anticorrelation, which indicates that their activity-induced RV scatter is lower at longer wavelengths. For most of them we can exclude a linear correlation between RV and H alpha emission. Conclusions. Our results are in agreement with simulated activity-induced RV variations in M dwarfs. The RV variations of most active RV-loud M dwarfs are likely to be caused by dark spots on their surfaces, which move in and out of view as the stars rotate.

引用

页数：17

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