ESA’s CHEOPS satellite was launched to produce high-quality light-curves of exoplanet systems. A new paper led by Adrien Deline of the University of Geneva now reports CHEOPS observations around the orbit of the ultra-hot-Jupiter WASP-189b. The figure shows the transit (planet passing in front of the star), the eclipse (the planet passing behind the star) and a slower variation caused by the varying visibility of the heated face of the planet.
One notable feature of the transit of WASP-189b is that it is distinctly asymmetrical. This is caused by gravity darkening, which occurs when a star is rapidly rotating. The centrifugal forces cause the equatorial regions to be pushed outwards, producing an equatorial bulge. Since the bulge is then further from the star’s centre, the surface gravity will be lower, and that means that the surface will be cooler and thus dimmer.
The illustrations below show the asymmetry, where the dashed line in the lowest panel shows the difference between a transit model both with and without gravity darkening. The right-hand panel illustrates the polar orbit of the planet.
With ultra-hot Jupiters being so near to their star their shape is predicted to be distorted away from spherical by the tidal effects of the host-star’s gravity. The resulting “rugby-ball” shape (more technically called a “Roche lobe”) will then produce a transit profile that is slightly different from that produced by a spherical planet.
The CHEOPS team now report that they have detected this distortion in the case of WASP-103b. A press release presents the infographic:
The CHEOPS observations of transits of WASP-103b are shown below (grey points). The blue model is the expected profile for a deformed planet, while the green line (lowest panel) is the expected difference in transit profile between a deformed planet and a spherical planet. The CHEOPS team show statistically that the data prefer the deformed shape, at a confidence level of 3σ.
The authors, Susana Barros et al, explain that the degree of tidal deformation constrains the distribution of mass within the planet, since the gaseous hydrogen envelope is much easier to deform than the rocky core. ESA have produced an artist’s illustration showing the distorted shape of WASP-103b:
Once a planet is found to transit its star, astronomers often try to figure out whether the planet’s orbit is aligned with the spin of the star. This is called the “obliquity”, denoted by Ψ, the angle between the orbital and stellar-spin axes.
This angle Ψ can be measured if we have enough information , including the broadening of the stellar lines caused by the star’s rotation, the perturbation of the stellar line profiles as the planet transits the star (called the Rossiter–McLaughlin effect), and the star’s rotation period.
It has long been known that many hot-Jupiter exoplanets are in aligned orbits (where the star’s spin axis is perpendicular to the orbital plane), but that a significant fraction are misaligned. Now a new paper led by Simon Albrecht reports that the misaligned planets tend to be in polar orbits, where the planet passes directly over the star’s poles.
The plot shows values for all the hot Jupiters where Ψ can be measured — of which roughly half are WASP planets — and reveals that obliquity values (y-axis) imply that the planets tend to be either aligned (low values of Ψ) or in polar orbits (Ψ near 90 degrees).
In the illustration below the planets orbit in the equatorial plane (we look along the z axis), and the arrows point along the stellar spin axes. The arrows collected around the y axis are thus the aligned systems. The rest are not evenly distributed, but are preferentially close to the orbital plane.
Although the authors discuss several mechanisms that can be causing misaligned orbits, the reason for the preponderance of planets in polar orbits is not yet understood.
“Aerosols have a critical role in establishing energy budgets, thermal structure, and dynamics in planetary atmospheres”, declares a new paper by Raissa Estrela et al.
Aerosols make the planet’s atmosphere hazy, an effect which is more pronounced at the blue end of the spectrum. Here is the spectrum of hot-Jupiter exoplanet WASP-69b, combining Hubble Space Telescope data from several observations.
The steeply rising spectrum (the y-axis shows effective planet size, with a larger size indicating more atmospheric absorption) is modelled (blue line) by including haze from aerosol scattering. The aerosols are found to extend from millibar pressures to microbar pressures.
The authors don’t yet know the composition of the aerosols, but suggest possibilities including hydrocarbons or magnesium silicate condensates. Overall they conclude that: “These results are consistent with theoretical expectations based on microphysics of the aerosol particles that have suggested haze can exist at microbar pressures in exoplanet atmospheres”.
CHEOPS, the CHaracterising ExOPlanet Satellite is ESA’s Small-class mission dedicated to recording transits of exoplanets. A new paper led by Luca Borsato presents some early observations of transits of WASP, KELT and HATnet planets.
Here, for example, are the lightcurves of two transits of WASP-8b, both plotted against phase.
The paper focuses on the transit timing, which can be as good as timing a transit to an accuracy of 13 to 16 seconds, depending on the brightness of the host star and the amount of transit covered by the observations.
One aim of such work is to look for variations in the timing of transits, caused by the gravitational perturbations of additional unseen planets in the system.
Here’s a plot from a new paper by David Cont et al, of the University of Göttingen. The plot shows spectra of the WASP-33 system, obtained with the CARMENES near-infra-red spectrograph on the 3.5-m telescope at the Calar Alto Observatory.
The image shows features caused by iron absorption lines, as a function of time (y-axis). The spectra have all been adjusted so that zero velocity (RV) is centred on the host star, WASP-33. The star’s rotation then causes features over the spread of velocities marked by the dashed yellow lines.
One can clearly see the rippling effect of pulsations as they run around the star. The pulsations are likely being excited by the tidal pull of the planet.
In addition, though, and marked by yellow arrows, is a faint diagonal line. This is caused by the planet, WASP-33b, and is the effect of iron absorption lines in the planet’s atmosphere. It moves diagonally across the image owing to the orbital motion of the planet around the star.
By comparing their analysis of iron lines to a similar analysis for Titanium Oxide, the authors show that there is a temperature inversion (higher temperature at greater height) in the atmosphere of the planet.
Bloated hot-Jupiter WASP-79b, one of the largest known exoplanets with a radius near twice that of Jupiter, is among the planets scheduled to be observed with the keenly-awaited JWST. In a new paper, Alexander Rathcke et al report on observations made with Hubble. Here’s the spectrum:
The clearest spectral feature, in the range observed with the WFC3 G141 grating, is attributed to water vapour. The authors also interpret the spectrum as showing opacity due to H− ions and the effects of faculae on the host star, that are 500 K hotter than most of the star’s surface. They say that this “underscores the importance” of observing a wide wavelength range in order to “disentangle the influence of unocculted stellar heterogeneities from planetary transmission spectra”.
As you’ll likely know from flying in an aircraft above the weather, clouds are bright, they reflect a lot of sunlight. This means that if a hot-Jupiter exoplanet has a cloudy atmosphere, then it should also be relatively bright, and so we should be able to detect a discernible drop in light when it it eclipsed behind its host star.
A new paper by Jonathan Fraine et al analyses data obtained with the Hubble Space Telescope WFCS/UVIS instrument to look for the eclipse of WASP-43b. Here is the result (with the data compared to model eclipse profiles):
The authors find no significant eclipse, deriving only an upper limit to any drop in light of 67 parts-per-million, which means that the dayside face of the planet is reflecting less than 6% of the illuminating starlight. And that means “that we can rule out a high altitude, bright, uniform cloud layer”.
Fraine et al remark that “Because of its observational and atmospheric viability for spectroscopic detections, WASP-43b has become a benchmark planet for current and future hot Jupiter observations. Upcoming … JWST observations [will] map the thermal structure and chemical composition of this exoplanet with exquisite detail … We expect that no other exoplanet has or will be observed with this much precision and wavelength coverage for many years to come.”
The importance of cloud-free skies is that one can then see atomic and molecular spectral features much more readily, and so learn much more about the atmosphere’s composition.
Here’s a plot of the spectrum of the ultra-hot-Jupiter WASP-121b. It’s from a new paper led by Jamie Wilson of Queen’s University Belfast.
The plot compares results from different instruments at different times. In particular the green points are from the ground-based Gemini/GMOS instrument, and are fitted by the model in red. The light-blue points (and fitted purple model) are from the space-based HST/STIS instrument.
Clearly the two datasets are not consistent. One possible explanation would involve instrumental systematics that are not properly accounted for in the analysis. Such analyses are right at the edge of what can be done, pushing the instruments beyond their designed capabilities, and reducing the datasets to a properly calibrated spectrum is a demanding task.
The other possible explanation is that WASP-121b really was different on the two occasions, and that “weather” on the planet is affecting its atmosphere. Just as Earth’s atmosphere can change from clear to cloudy, we expect that the same could be occurring on exoplanets.
The authors say that: “WASP-121b is expected to have wind speeds of 7 km/s and a pressure–temperature profile which lies near the condensation curves of a number of species”, and thus: “It is therefore perhaps not all that surprising that small temperature fluctuations could result in significant spatial and temporal variations in atmospheric constituents and could lead to measurable variations in transit measurements.”