Chromospheric activity of stars with planets

@article{Martins2011ChromosphericAO,
  title={Chromospheric activity of stars with planets},
  author={B. L. Canto Martins and Maria Lidu{\'i}na das Chagas and Sanzia Alves and I. C. Le{\~a}o and L. P. de Souza Neto and J. R. De Medeiros},
  journal={Astronomy and Astrophysics},
  year={2011},
  volume={530}
}
Context. Signatures of chromospheric activity enhancement have been found for a dozen stars, pointing to a possible star-planet interaction. Nevertheless in the coronal activity regime, there is no conclusive observational evidence of such an interaction. Does star-planet interaction manifest itself only for a few particular cases, without having a major effect on stars with planets in general? Aims. We aim to add additional observational constraints to support or reject the major effects of… 

Figures and Tables from this paper

Search for the Star-Planet Interaction

Abstract We analyse the chromospherical activity of stars with extrasolar planets and search for a possible correlation between the equivalent width of the core of the Ca II K line and orbital

ON THE DETECTABILITY OF STAR–PLANET INTERACTION

Magnetic (or tidal) interactions between “hot Jupiters” and their host stars can potentially enhance chromospheric and coronal activity. An ideal test bed for investigating this effect is provided by

A Statistical Search for Star–Planet Interaction in the Ultraviolet Using GALEX

Most (∼82%) of the over 4000 confirmed exoplanets known today orbit very close to their host stars, within 0.5 au. Planets at such small orbital distances can result in significant interactions with

The effect of ISM absorption on stellar activity measurements and its relevance for exoplanet studies

Past ultraviolet and optical observations of stars hosting close-in Jupiter-mass planets have shown that some of these stars present an anomalously low chromospheric activity, significantly below the

A COMPREHENSIVE STATISTICAL ASSESSMENT OF STAR–PLANET INTERACTION

We investigate whether magnetic interaction between close-in giant planets and their host stars produce observable statistical enhancements in stellar coronal or chromospheric activity. New Chandra

AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS

Using the far-UV (FUV) and near-UV (NUV) photometry from the NASA Galaxy Evolution Explorer (GALEX), we searched for evidence of increased stellar activity due to tidal and/or magnetic star–planet

Star-planet magnetic interaction and activity in late-type stars with close-in planets

Context. Late-type stars interact with their close-in planets through their coronal magnetic fields. Aims. We introduce a theory for the interaction between the stellar and planetary fields focussing

Evidence for enhanced chromospheric Ca II H and K emission in stars with close-in extrasolar planets

The planet-star interaction is manifested in many ways. It has been found that a close-in exoplanet causes small but measurable variability in the cores of a few lines in the spectra of several

A BIMODAL CORRELATION BETWEEN HOST STAR CHROMOSPHERIC EMISSION AND THE SURFACE GRAVITY OF HOT JUPITERS

The chromospheric activity index log R HK ′ ?> of stars hosting transiting hot Jupiters appears to be correlated with the planets’ surface gravity. One of the possible explanations is based on the

The Effects of Close-in Exoplanets on Their Host Stars

In analogy to the RS CVn stars, it is expected that close-in planets can induce stellar activity due to tidal and magnetic interaction between the star and the planet. The tidal and/or magnetic

References

SHOWING 1-10 OF 21 REFERENCES

Coronal properties of planet-bearing stars

Context. Do extrasolar planets affect the activity of their host stars? Indications for chromospheric activity enhancement have been found for a handful of targets, but in the X-ray regime,

Extrasolar Giant Planets and X-Ray Activity

We have carried out a survey of X-ray emission from stars with giant planets, combining both archival and targeted surveys. Over 230 stars have been currently identified as possessing planets, and

On the rotational behaviour of parent stars of extrasolar planets

We analysed the behaviour of the rotational velocity in the parent stars of extrasolar planets. Projected rotational velocity v sin i and angular momentum were combined with stellar and planetary

Evidence for Planet-induced Chromospheric Activity on HD 179949

We have detected the synchronous enhancement of Ca II H and K emission with the short-period planetary orbit in HD 179949. High-resolution spectra taken on three observing runs extending over more

An extrasolar planet that transits the disk of its parent star

Planets orbiting other stars could in principle be found through the periodic dimming of starlight as a planet moves across—or ‘transits’—the line of sight between the observer and the star.

The On/Off Nature of Star-Planet Interactions

Evidence suggesting an observable magnetic interaction between a star and its hot Jupiter appears as a cyclic variation of stellar activity synchronized to the planet's orbit. In this study we

A planet around the evolved intermediate-mass star HD 110014 ,

Context. We found evidence for a sub–stellar companion around the K giant star HD 110014. This cool evolved star, with a spectral type K2III and an estimated mass between 1.9 and 2.4 M� , is slightly

Chromospheric Ca II Emission in Nearby F, G, K, and M Stars

We present chromospheric Ca II H and K activity measurements, rotation periods, and ages for ∼1200 F, G, K, and M type main-sequence stars from ∼18,000 archival spectra taken at Keck and Lick

Rotation, convection, and magnetic activity in lower main-sequence stars

Rotation periods are reported for 14 main-sequence stars, bringing the total number of such stars with well-determined rotation periods to 41. It is found that the mean level of their Ca n H and K

A Planet Orbiting 47 Ursae Majoris

The G0 V star 47 UMa exhibits very low amplitude radial velocity variations having a period of 2.98 yr, a velocity amplitude of K = 45.5 m s-1, and small eccentricity. The residuals scatter by 11 m