From astrobites: “I see skies of blue and clouds of white”

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Astrobites

July 21, 2017
Shang-Min Tsai

Title: A Cloudiness Index for Transiting Exoplanets Based on the Sodium and Potassium Lines: Tentative Evidence for Hotter Atmospheres Being Less Cloudy at Visible Wavelengths
Authors: K. Heng
First Author’s Institution: Center for Space and Habitability, University of Bern
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Status: Published on ApJL, open access

Background

Most astronomers hate clouds, except for those who study them. Not only our clouds on the sky ruin observing nights, clouds on other planets obscure everything underneath, too. When observing extra-solar planets during transit, different atoms, molecules or particles absorb light at certain wavelengths, making the apparent radii of the planets change as viewed with different colors — known as transmission spectroscopy. Although it is a powerful tool to infer the atmospheric composition of exoplanets, these clouds often hinder our efforts to understand such alien worlds. With clouds present at high altitude, only the atmosphere above the clouds can be seen and it is too thin to provide any spectral features (see this popular example). It turns out that a useful strategy for dealing with a problem is to avoid the problem. Valuable space telescope time could be saved if we could filter cloud-free objects from ground-based measurements. Today’s paper presents an index to quantify the degree of cloudiness for transiting planets.

Aim

The author first revisited how previous studies used the slope of transmission spectra caused by scattering (blue light is scattered more than red) to distinguish cloudy and dense atmospheres. Such dense atmospheres are more packed (with smaller scale height) and can produce flat spectra that are compatible with cloud-free hydrogen-dominated atmospheres. The author demonstrates that the scattering cross sections of gaseous molecules (e.g. hydrogen, nitrogen) and aerosols or condensates (cloud particles) have the same wavelength dependence. Measuring the spectral slope alone does not solve the ambiguity between clouds and atmospheric composition. With this motivation, the author proceeds to find a cloudiness index that does not depend on the spectral slope.

Methods

Sodium has large cross sections so it can produce a prominent spectral line without being abundant. It is, in fact, the first extrasolar atmospheric detection on HD 209458b. In a clear, cloud free atmosphere, the difference in transit radii between the line center and wing of sodium can be theoretically calculated. By measuring the actual difference in transit radii between the line center and wing (Δ Robs), the author constructs a dimensionless index (C) for the degree of cloudiness as the ratio of Δ R and Δ Robs. For an entirely cloud-free atmosphere, Δ R equals to Δ Robs and C = 1. Very cloudy atmospheres have C Gt 1. This cloudiness index is independent of the spectral slope, with the caveat that it is limited to planets with sodium or potassium line detections.

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Figure 1: Cloudiness index plotted against equilibrium temperature (top), surface gravity (middle), planetary mass (bottom). The labels “W6,” “W17,” “W31,” “W39,” “H1,” “H12,” and “HD189” refer to WASP-6b, WASP-17b, WASP-31b, WASP-39b, HAT-P-1b, HAT-P-12b, and HD 189733b, respectively [from the featured paper].

Application to data

Figure 1 plots the cloudiness index (C) versus equilibrium temperature, gravity, and mass of the planets. The uncertainty of the cloudiness basically stems from estimating the scale height with the equilibrium temperature in the calculation, which is larger for colder planets. An interesting trend of decreasingC with increasing equilibrium temperature (a proxy for stellar flux) is seen in the top panel. If the trend is real, it implies that more irradiated planets tend to be less cloudy. Future measurements of sodium lines at higher resolutions and for a larger sample will confirm or debunk the trend. If the trend holds, the author suggests that we can weed out cloudy objects for the detailed survey of JWST, to avoid spending lots of time (and money) for uninformative, featureless spectra.

See the full article here .

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