Status Report

Helium in the eroding atmosphere of an exoplanet

By SpaceRef Editor
May 4, 2018
Filed under , , ,

J. J. Spake, D. K. Sing, T. M. Evans, A. Oklopčić, V. Bourrier, L. Kreidberg, B. V. Rackham, J. Irwin, D. Ehrenreich, A. Wyttenbach, H. R. Wakeford, Y. Zhou, K. L. Chubb, N. Nikolov, J. M. Goyal, G. W. Henry, M. H. Williamson, S. Blumenthal, D. R. Anderson, C. Hellier, D. Charbonneau, S. Udry, N. Madhusudhan
(Submitted on 3 May 2018)

Helium is the second-most abundant element in the Universe after hydrogen and is one of the main constituents of gas-giant planets in our Solar System. Early theoretical models predicted helium to be among the most readily detectable species in the atmospheres of exoplanets, especially in extended and escaping atmospheres. Searches for helium, however, have hitherto been unsuccessful. Here we report observations of helium on an exoplanet, at a confidence level of 4.5 standard deviations. We measured the near- infrared transmission spectrum of the warm gas giant WASP-107b and identified the narrow absorption feature of excited metastable helium at 10,833 angstroms. The amplitude of the feature, in transit depth, is 0.049 +/- 0.011 per cent in a bandpass of 98 angstroms, which is more than five times greater than what could be caused by nominal stellar chromospheric activity. This large absorption signal suggests that WASP-107b has an extended atmosphere that is eroding at a total rate of 10^10 to 3 x 10^11 grams per second (0.1-4 per cent of its total mass per billion years), and may have a comet-like tail of gas shaped by radiation pressure.

Comments:    Accepted in Nature
Subjects:    Earth and Planetary Astrophysics (astro-ph.EP)
DOI:    10.1038/s41586-018-0067-5
Cite as:    arXiv:1805.01298 [astro-ph.EP] (or arXiv:1805.01298v1 [astro-ph.EP] for this version)
Submission history
From: Jessica Spake 
[v1] Thu, 3 May 2018 13:31:16 GMT (3039kb)

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