Category Archives: Hot Jupiters

Iron in the atmosphere of the ultra-hot-Jupiter WASP-33b

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.

The spectrum of hot Jupiter WASP-79b

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”.

No clouds on the dayside of WASP-43b

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.

Weather on ultra-hot-Jupiter WASP-121b?

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.”

The colours of the planets

Here is an interesting image from Donald Mitchell on Twitter. It shows the average colour of planets and moons in the Solar System.

It would be interesting to do the same for exoplanets. Here is Vivien Parmentier showing possible colours of hot Jupiters, depending on their atmospheric composition and temperature (Credit: NASA/JPL-Caltech/University of Arizona/V. Parmentier):

TESS observes the WASP-148 system

The hot Jupiter WASP-148b is rather unusual, since it has a sibling planet, WASP-148c in a 35-day orbit (Hébrard et al. 2020). The system was recently observed by TESS leading to a new paper by Gracjan Maciejewski et al. (Nicolaus Copernicus University and the Instituto de Astrofísica de Andalucía).

The gravitational tug of the outer planet WASP-148c perturbs the orbit of the hot Jupiter WASP-148b. Here are deviations in the timings of the hot-Jupiter’s transit (the green points are new timings from TESS, the blue points are from observations from the Sierra Nevada Observatory, the red line is a model based on the masses and orbits of the planets):

The great boon of transit-timing information is that it leads to measurements of the masses of the planets, which can be combined with radial-velocity measurements to give a better overall characterisation of the system.

Maciejewski et al. also searched the TESS data for transits of the outer planet. The yellow areas are the predicted time of transit, should the planet’s orbital inclination be sufficiently high (the red line is a model showing the predicted depth of the transit; the black triangle marks a transit of the hot Jupiter WASP-148b). There is no indication that WASP-148c transits.

Confirmation of the changing orbital period of WASP-12b

A new paper by Jake Turner et al (Cornell University) analyses TESS data on WASP-12b, showing that the transit timings confirm that the orbital period of the planet is getting shorter.

The orbit is changing on a timescale of 3 Myrs — if it continues the planet will spiral into its star on that timescale. The natural interpretation is that the orbital decay is being caused by tides that the gravitational pull of the planet arouses in the host star. We don’t yet properly understand the effect that tides have on the star, or how internal waves created by the tides then dissipate their energy. Thus the observations of WASP-12b point to the need for a better theoretical understanding of stellar interiors.

Of course the period change has only been measured over a decade, and this is vastly shorter than the orbital-decay timescale. Thus it could be that other mechanisms that we don’t know about can cause short-term changes in planet’s orbital periods. Ongoing monitoring of all the WASP hot Jupiters is thus needed to properly understand what is going on. The TESS satellite, which will observe most hot Jupiters every two years or so, on an ongoing basis, is the perfect tool for the task.

Update: Here’s a Twitter thread by the lead author, Jake Turner.

WASP-62b, in James Webb’s continuous-viewing zone, has a clear atmosphere

James Webb’s “Continuous Viewing Zone” is the patch of sky where the satellite can point continuously at a target and so observe it most efficiently. Exoplanets within the CVZ that are suitable for atmospheric characterisation are thus of high importance, and so far WASP-62b is the only gas giant known within the CVZ.

Munazza Alam et al have now pointed the Hubble and Spitzer space telescopes at WASP-62b to see what its atmosphere looks like. Importantly, they find that WASP-62b has clear skies. This matters since cloudy or haze-filled atmospheres tend to produce flat spectra lacking any spectral features, and so don’t tell us much.

Here, Alam et al plot the spectrum near the sodium (Na) line, showing that it has a broad base, akin to that in the clear-skied planet WASP-96b. The broad base of the line means that it is being widened by “pressure broadening”, and that can only happen deep in the planet’s atmosphere where the pressure is high. And we can only see deep into the atmosphere if it is clear rather than cloudy.

Clear skies mean that spectral features produced by the molecules in the atmosphere should be readily detectable with JWST. Here Alam et al simulate what we expect to see with JWST, showing that Na, H2O, NH3, FeH, SiH, CO, CO2, and CH4 can all be detected.

They conclude by saying that: “As the only transiting giant planet currently known in the JWST Continuous Viewing Zone, WASP-62b could prove a benchmark giant exoplanet for detailed atmospheric characterization in the James Webb era.

ESPRESSO looks at ultra-hot-Jupiter WASP-121b

ESPRESSO is ESO’s state-of-the-art spectrograph for the Very Large Telescope, specifically designed to get the best data possible on planetary systems.

Francesco Borsa et al have pointed ESPRESSO at transits of the ultra-hot-Jupiter WASP-121b, and the ESPRESSO team have put out a series of Tweets explaining the paper: