Probing the atmosphere of HD189733b with the Na i and K i lines

Keles, Engin; Kitzmann, Daniel; Mallonn, M.; Alexoudi, X.; Fossati, L.; Pino, L.; Seidel, J. V.; Carroll, T. A.; Steffen, M.; Ilyin, I.; Poppenhäger, Katja; Strassmeier, K. G.; Essen, C. von; Nascimbeni, V.; Turner, Jake D.

doi:10.1093/mnras/staa2435

Cited by 13 publications

(15 citation statements)

References 74 publications

(112 reference statements)

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“…Excess absorption has been observed at the Na doublet (e.g. Redfield et al 2008;Huitson et al 2012;Wyttenbach et al 2015;Louden & Wheatley 2015;Khalafinejad et al 2017), and there is evidence for a K absorption feature (Pont et al 2013;Keles et al 2019Keles et al , 2020. In the near-infrared, water (Birkby et al 2013;McCullough et al 2014;Brogi et al 2016Brogi et al , 2018 and CO (de Kok et al 2013;Rodler et al 2013;Brogi et al 2016) have both been detected.…”

Section: The Hd 189733 Systemmentioning

confidence: 99%

The near-UV transit of HD 189733b with the XMM–Newton optical monitor

King

Corrales

Wheatley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present analysis of XMM-Newton Optical Monitor observations in the near-ultraviolet of HD 189733, covering twenty primary transits of its hot Jupiter planet. The transit is clearly detected with both the UVW2 and UVM2 filters, and our fits to the data reveal transit depths in agreement with that observed optically. The measured depths correspond to radii of $1.05{9}^{+0.0{46}}_{-0.0{50}}$ and $0.9{4}^{+0.15}_{-0.17}$ times the optically-measured radius in the UVW2 and UVM2 bandpasses, respectively. We also find no statistically significant variation in the transit depth across the 8 year baseline of the observations. We rule out extended broadband absorption towards or beyond the Roche lobe at the wavelengths investigated, although observations with higher spectral resolution are required to determine if absorption out to those distances from the planet is present in individual near-UV lines.

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Section: The Hd 189733 Systemmentioning

confidence: 99%

The near-UV transit of HD 189733b with the XMM–Newton optical monitor

King

Corrales

Wheatley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Several works investigated and/or showed wind properties for transiting exoplanets using observations and modeling approaches e.g. Spiegel et al (2007), Snellen et al (2010), Miller-Ricci Kempton & Rauscher (2012), Showman et al (2012), Kempton et al (2014), Wyttenbach et al (2015), Louden & Wheatley (2015), Brogi et al (2016), Flowers et al (2019), Seidel et al (2019), Casasayas-Barris et al (2019), Cauley et al (2019), Seidel et al (2020), Gebek & Oza (2020), Keles et al (2020), Ehrenreich et al (2020), Cauley et al (2020) and more. Two categories seem to be of main interest for the majority of the studies investigating atomic and molecular lines: On the one side, the investigation of day-to-nightside winds by searching for the blueshift of spectral lines, where it is expected that most irradiated planets should show the strongest blueshifts (Miller-Ricci Kempton & Rauscher 2012;Showman et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Spectral signature of atmospheric winds in high-resolution transit observations

Keles

2021

Monthly Notices of the Royal Astronomical Society

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The study of exoplanet atmospheres showed large diversity compared to the planets in our Solar system. Especially Jupiter-type exoplanets orbiting their host star in close orbits, the so-called hot and ultra-hot Jupiters, have been studied in detail due to their enhanced atmospheric signature. Due to their tidally locked status, the temperature difference between the day- and nightside triggers atmospheric winds that can lead to various fingerprints in the observations. Spatially resolved absorption lines during transit such as sodium (Na) could be a good tracer for such winds. Different works resolved the Na absorption lines on different exoplanets which show different line widths. Assuming that this could be attributed to such zonal jet streams, this work models the effect of such winds on synthetic absorption lines. For this, transiting Jupiter-type planets with rotational velocities similar to hot and ultra-hot Jupiter are considered. The investigation shows that high wind velocities could reproduce the broadening of Na-line profiles inferred in different high-resolution transit observations. There is a tendency that the broadening values decrease for planets with lower equilibrium temperature. This could be explained by atmospheric drag induced by the ionization of alkali lines that slow down the zonal jet streams, favouring their existence on hot Jupiter rather than ultra-hot Jupiter.

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“…for HD189733 b and later confirmed via independent observations in Keles et al (2020). This vertical wind can either be an outwards expanding wind, where the material does not descend back towards lower atmospheric layers or the vertical parts of large cell-like structures, where the upper, zonal arm of the cell is in the thermosphere.…”

Section: Discussionmentioning

confidence: 60%

Into the Storm: Diving into the winds of the ultra hot Jupiter WASP-76 b with HARPS and ESPRESSO

Seidel,

Ehrenreich,

Allart

et al. 2021

Preprint

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Context. Despite swift progress in the characterisation of exoplanet atmospheres in composition and structure, the study of atmospheric dynamics has not progressed at the same speed. While theoretical models have been developed to describe the lower layers of the atmosphere and, disconnected, the exosphere, little is known about the intermediate layers up to the thermosphere. Aims. We aim to provide a clearer picture of atmospheric dynamics for the class of ultra hot Jupiters, highly-irradiated gas giants, on the example of WASP-76 b. Methods. We analysed two datasets jointly, obtained with the HARPS and ESPRESSO spectrographs, to interpret the resolved planetary sodium doublet. We then applied the MERC code, which retrieves wind patterns, speeds, and temperature profiles on the line shape of the sodium doublet. An updated version of MERC, with added planetary rotation, also provides the possibility to model the latitude dependence of the wind patterns. Results. We retrieve the highest Bayesian evidence for an isothermal atmosphere, interpreted as a mean temperature of 3389 ± 227 K, a uniform day-to-night side wind of 5.5 +1.4 −2.0 km s −1 in the lower atmosphere with a vertical wind in the upper atmosphere of 22.7 +4.9 −4.1 km s −1 , switching atmospheric wind patterns at 10 −3 bar above the reference surface pressure (10 bar). Conclusions. Our results for WASP-76 b are compatible with previous studies of the lower atmospheric dynamics of WASP-76 b and other ultra hot Jupiters. They highlight the need for vertical winds in the intermediate atmosphere above the layers probed by global circulation model studies to explain the line broadening of the sodium doublet in this planet. This work demonstrates the capability of exploiting the resolved spectral line shapes to observationally constrain possible wind patterns in exoplanet atmospheres, an invaluable input to more sophisticated 3D atmospheric models in the future.

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Probing the atmosphere of HD189733b with the Na i and K i lines

Cited by 13 publications

References 74 publications

The near-UV transit of HD 189733b with the XMM–Newton optical monitor

The near-UV transit of HD 189733b with the XMM–Newton optical monitor

Spectral signature of atmospheric winds in high-resolution transit observations

Into the Storm: Diving into the winds of the ultra hot Jupiter WASP-76 b with HARPS and ESPRESSO

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