Activity-induced radial velocity variation of M dwarf stars

Publikation: Bidrag til tidsskrift › Konferenceartikel › Forskning › fagfællebedømt

Standard

Activity-induced radial velocity variation of M dwarf stars. / Andersen, Jan Marie; Korhonen, Heidi Helena.

I: Proceedings of the International Astronomical Union, Bind 8, Nr. S293, 08.2012, s. 197-200.

Publikation: Bidrag til tidsskrift › Konferenceartikel › Forskning › fagfællebedømt

Harvard

Andersen, JM & Korhonen, HH 2012, 'Activity-induced radial velocity variation of M dwarf stars', Proceedings of the International Astronomical Union, bind 8, nr. S293, s. 197-200. https://doi.org/10.1017/S1743921313012829

APA

Andersen, J. M., & Korhonen, H. H. (2012). Activity-induced radial velocity variation of M dwarf stars. Proceedings of the International Astronomical Union, 8(S293), 197-200. https://doi.org/10.1017/S1743921313012829

Vancouver

Andersen JM, Korhonen HH. Activity-induced radial velocity variation of M dwarf stars. Proceedings of the International Astronomical Union. 2012 aug.;8(S293):197-200. https://doi.org/10.1017/S1743921313012829

Author

Andersen, Jan Marie ; Korhonen, Heidi Helena. / Activity-induced radial velocity variation of M dwarf stars. I: Proceedings of the International Astronomical Union. 2012 ; Bind 8, Nr. S293. s. 197-200.

Bibtex

@inproceedings{79a2937553cf433b9ca615d5ae7d5236,
title = "Activity-induced radial velocity variation of M dwarf stars",
abstract = "Stellar magnetic activity manifests itself in a variety of ways including starspots-cool, dark regions on the stellar surface. Starspots can cause variations ('jitter') in spectral line-profiles which can mimic the radial velocity (RV) variations caused by an orbiting planet, or create RV noise that can drown out a planetary signature. Cool, low-mass M dwarf stars can be highly active, which can make detection of potentially habitable planets around these stars difficult. We investigate radial velocity variations caused by different activity (spot) patterns on M dwarf stars in order to determine the limits of detectability for small planets orbiting active M dwarfs. We report on our progress toward the aim of answering the following questions: What types of spot patterns are realistic for M dwarf stars? What effect will spots have on M dwarf RV measurements? Can jitter from M dwarf spots mimic planetary signals? What is the ideal observing wavelength to reduce M dwarf jitter?",
keywords = "atmospheres, low-mass, planetary systems, rotation, spots, stars: activity, techniques: radial velocities",
author = "Andersen, {Jan Marie} and Korhonen, {Heidi Helena}",
year = "2012",
month = aug,
doi = "10.1017/S1743921313012829",
language = "English",
volume = "8",
pages = "197--200",
journal = "Proceedings of the International Astronomical Union",
issn = "1743-9213",
publisher = "Cambridge University Press",
number = "S293",
note = "null ; Conference date: 27-08-2012 Through 31-08-2012",

}

RIS

TY - GEN

T1 - Activity-induced radial velocity variation of M dwarf stars

AU - Andersen, Jan Marie

AU - Korhonen, Heidi Helena

N1 - Conference code: 293

PY - 2012/8

Y1 - 2012/8

N2 - Stellar magnetic activity manifests itself in a variety of ways including starspots-cool, dark regions on the stellar surface. Starspots can cause variations ('jitter') in spectral line-profiles which can mimic the radial velocity (RV) variations caused by an orbiting planet, or create RV noise that can drown out a planetary signature. Cool, low-mass M dwarf stars can be highly active, which can make detection of potentially habitable planets around these stars difficult. We investigate radial velocity variations caused by different activity (spot) patterns on M dwarf stars in order to determine the limits of detectability for small planets orbiting active M dwarfs. We report on our progress toward the aim of answering the following questions: What types of spot patterns are realistic for M dwarf stars? What effect will spots have on M dwarf RV measurements? Can jitter from M dwarf spots mimic planetary signals? What is the ideal observing wavelength to reduce M dwarf jitter?

AB - Stellar magnetic activity manifests itself in a variety of ways including starspots-cool, dark regions on the stellar surface. Starspots can cause variations ('jitter') in spectral line-profiles which can mimic the radial velocity (RV) variations caused by an orbiting planet, or create RV noise that can drown out a planetary signature. Cool, low-mass M dwarf stars can be highly active, which can make detection of potentially habitable planets around these stars difficult. We investigate radial velocity variations caused by different activity (spot) patterns on M dwarf stars in order to determine the limits of detectability for small planets orbiting active M dwarfs. We report on our progress toward the aim of answering the following questions: What types of spot patterns are realistic for M dwarf stars? What effect will spots have on M dwarf RV measurements? Can jitter from M dwarf spots mimic planetary signals? What is the ideal observing wavelength to reduce M dwarf jitter?

KW - atmospheres

KW - low-mass

KW - planetary systems

KW - rotation

KW - spots

KW - stars: activity

KW - techniques: radial velocities

UR - http://www.scopus.com/inward/record.url?scp=84899875011&partnerID=8YFLogxK

U2 - 10.1017/S1743921313012829

DO - 10.1017/S1743921313012829

M3 - Conference article

AN - SCOPUS:84899875011

VL - 8

SP - 197

EP - 200

JO - Proceedings of the International Astronomical Union

JF - Proceedings of the International Astronomical Union

SN - 1743-9213

IS - S293

Y2 - 27 August 2012 through 31 August 2012

ER -

ID: 183471442