Stellar activity of planetary host star HD 189 733

By I. Boisse, C. Moutou, A. Vidal-Madjar, F. Bouchy, F. Pont, G. Hébrard, X. Bonfils, B. Croll, X. Delfosse, M. Desort and 13 more. 2008

150 citations recorded by the source corpus.

Aims. Extra-solar planet search programs require high-precision velocity measurements. They need to determine how to differentiate between radial-velocity variations due to Doppler motion and the noise induced by stellar activity. Methods. We monitored the active K2V star HD 189733 and its transiting planetary companion, which has a 2.2-day orbital period. We used the high-resolution spectograph SOPHIE mounted on the 1.93-m telescope at the Observatoire de Haute-Provence to obtain 55 spectra of HD 189733 over nearly two months. We refined the HD 189733b orbit parameters and placed limits on both the eccentricity and long-term velocity gradient. After subtracting the orbital motion of the planet, we compared the variability in spectroscopic activity indices with the evolution in the radial-velocity residuals and the shape of spectral lines. Results. The radial velocity, the spectral-line profile, and the acti vity indices measured in He I (5875.62 A), Hα (6562.81 A), and both of the Ca II H&K lines (3968.47 A and 3933.66 A, respectively) exhibit a periodicity close to the stellar-rotation pe riod and the correlations between them are consistent with a spotted stellar surface in rotation. We used these correlations to corr ect for the radialvelocity jitter due to stellar activity. This results in ach ieving high precision in measuring the orbital parameters, with a semi-amplitude ◦ .

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f75608b89c3abe820fa948f197b83c2f2306acc8

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In Astronomy and Astrophysics

1. Jon Fortney
2. N. Madhusudhan
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In Instrumentation

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6. A. Showman
7. H. Knutson
8. D. Deming

Citations in the corpus

• THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET (2014, methodology): “…by the rotation period and harmonics (Dumusque et al. 2012; Boisse et al. 2011; Queloz et al. 2009), correlation with activity indicators (Boisse et al. 2009), velocity differences using multiple observations during the same night (Hatzes et al. 2010), correlation with photometric…”
• A Gaussian process framework for modelling stellar activity signals in radial velocity data (2015, methodology): “…of methods ranging from exploiting simple correlations between the radial velocity measurements and chromospheric activity or line shape indicators (Boisse et al. 2009; Tuomi et al. 2014; Robertson & Mahadevan 2014), pre-whitening of the RV time series (Queloz et al. 2009), and using red-noise…”
• Disentangling between stellar activity and planetary signals (2010, methodology): “Removing this anti-correlation to subtract the activity-induced RV may allow us to derive more accurate parameters of the planetary system (e.g. Melo et al. 2007; Boisse et al. 2009).”
• SOAP 2.0: A TOOL TO ESTIMATE THE PHOTOMETRIC AND RADIAL VELOCITY VARIATIONS INDUCED BY STELLAR SPOTS AND PLAGES (2014, background): “These correlations are often a powerful diagnostic to decide if the observed RV signal is of activity or planetary origin (e.g. Boisse et al. 2009; Bonfils et al. 2007; Queloz et al. 2001).”
• Hubble Space Telescope transmission spectroscopy of the exoplanet HD 189733b: high‐altitude atmospheric haze in the optical and near‐ultraviolet with STIS (2011, background): “…such as the space-based lightcurve with the MOST telescope (Croll et al. 2007) and intensive spectroscopic monitoring with the SOPHIE spectrograph (Boisse et al. 2009) show that the variability of the star can be well modeled both in flux and spectrum with cooler starspots modulated by stellar…”
• Searching for star–planet interactions within the magnetosphere of HD 189733 (2010, methodology): “A rotational modulation was also found by Moutou et al. 2007, Boisse et al. 2009, and Shkolnik et al. 2008.”
• Long-term magnetic activity of a sample of M-dwarf stars from the HARPS program I. Comparison of activity indices (2011, methodology): “Our Hα index was also computed as in Boisse et al. (2009) but using a slightly broader central band.”
• Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, unknown): “A new KA value is available from Boisse et al. (2009), supported by the value given by Triaud et al. (2009).”
• WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE TRANSIT (2014, background): “STAR SPOTS HD189733 is an active star (Boisse et al. 2009), and transit observations exhibit ubiquitous star spot crossings (Pont et al. 2007).”
• The Rossiter-McLaughlin effect of CoRoT-3b and HD 189733b (2009, unknown): “Also, HD 189733b has been extensively studied (Bouchy et al. (2005), Winn et al. (2006) (W06), Winn et al. (2007) (W07), Boisse et al. (2009) (B09)).”
• THE CLIMATE OF HD 189733b FROM FOURTEEN TRANSITS AND ECLIPSES MEASURED BY SPITZER (2010, methodology): “For the planet surface gravity, gp, we use the velocity semi-amplitude K = 200.56 ± 0.88 m s−1, derived by Boisse et al. (2009), and for the planet density, ρp, we use the stellar mass M∗ = 0.806 ± 0.048M⊙ given in Torres et al. (2008), propagating the uncertainties assuming they are uncorrelated…”
• The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “Indeed, stellar jitter, which is mostly caused by stellar activity (e.g. Boisse et al. 2009; Dumusque et al. 2011; Lanza et al. 2011a), can be more accurately estimated in RV data that are not dominated by photon noise or are dominated very little.”
• Evaporation of the planet HD 189733b observed in H I Lyman-α (2010, background): “This value is rather uncertain and might be underestimated (Landsman & Simon 1993), and this is strengthened by the particularly high chromospheric activity of this star (Henry & Winn 2008; Boisse et al. 2009).”
• 3.6 AND 4.5 μm PHASE CURVES AND EVIDENCE FOR NON-EQUILIBRIUM CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HD 189733b (2012, methodology): “…Fits We calculate our eclipse curve using the equations from Mandel & Agol (2002) assuming a circular orbit for the planet, as indicated by both radial velocity data (Bouchy et al. 2005; Triaud et al. 2009; Boisse et al. 2009) and secondary eclipse photometry (Agol et al. 2010; de Wit et al. 2012).”