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WASP-189 b: The Hottest Planet We Know

Scientists uncover details about extreme winds and atmosphere of WASP-189 b.

F. Lesjak, L. Nortmann, D. Cont, F. Yan, A. Reiners, N. Piskunov, A. Hatzes, L. Boldt-Christmas, S. Czesla, A. Lavail, E. Nagel, A. D. Rains, M. Rengel, U. Seemann, D. Shulyak

― 5 min read


WASP-189 b: Extreme WASP-189 b: Extreme Conditions Revealed atmosphere emerge. New findings on WASP-189 b's winds and
Table of Contents

WASP-189 b is a fascinating place. Imagine a gas giant so hot that it could give a pizza oven a run for its money! This planet orbits very close to its star, making it a prime example of what scientists call an ultra-hot Jupiter.

What's So Special About WASP-189 b?

First things first, what makes this planet stand out? It reaches Temperatures above 2000 K! For context, that's hotter than many stars. Because of its extreme heat, it's thought that the Atmosphere is largely free of clouds, allowing scientists to study its features in detail.

Typical hot Jupiters like WASP-189 b have very strong day-night temperature differences. This creates super-fast Winds in the atmosphere. Picture the winds we feel on Earth during a storm, but much stronger and in the form of jets or flows pushing materials from one side of the planet to another.

The Mission to Study the Planet's Atmosphere

In an effort to understand these winds better, scientists used a special telescope called CRIRES, which is designed for observing the universe in infrared light. They focused on the dayside of WASP-189 b to see what they could find.

After cleaning up the data by removing unwanted Signals from stars, scientists looked for signs of different molecules like carbon monoxide (CO) and iron (Fe) in the planet's atmosphere. They found strong signals of these molecules and even managed to calculate how these gases behaved under the planet's extreme conditions.

The Importance of Speed

One of the interesting findings from this study was the speed of the winds. They detected a notable shift in the velocity of the traced signals from CO and Fe, hinting that winds were zipping across the planet's surface at about 6 km/s. This hints at fast-moving day-to-night winds, which transport materials from the bright, sunlit side to the cooler, dark side of the planet.

High-Speed Winds: What Does It Mean?

The data suggested a strong day-to-night wind with a speed that could be impressive, but there wasn't enough evidence for a powerful equatorial jet. It's kind of like finding a really fast car but not enough data to claim there’s a race track involved. The winds seemed to be responsible for the red-shifts noticed in the data, which is when light gets stretched into longer wavelengths.

Revealing the Planet's Secrets

By analyzing the temperature and pressure patterns in the atmosphere, scientists were able to establish a model of how the atmosphere behaves. They noticed an inverted temperature-pressure profile, meaning that temperatures increased at higher altitudes instead of decreasing like what we see on Earth.

In simpler terms, the higher you go in the atmosphere of WASP-189 b, the hotter it gets! That might sound a bit strange, but it’s a result of the intense heat and radiation from the nearby star.

The Chemistry of WASP-189 b

Next on the agenda was the chemistry. Based on what they observed, it seems likely that the planet has a carbon-to-oxygen (C/O) ratio similar to that found on Earth. They found that the abundance of heavy elements was higher than in the star it orbits. This could mean that the planet formed by accumulating icy material from farther out in the solar system.

In the quest to uncover the full composition of the atmosphere, scientists looked for other elements that could tell them more about the planet. However, the detection of other molecules like water was elusive. This could either mean they are missing or simply that the conditions make them hard to find.

Drawing Conclusions about the Winds

As the study progressed, it became clear that winds played a critical role in shaping the observed signals. The researchers tackled this by developing a model that included different wind patterns and their effects on the spectra they observed.

They eventually determined that the atmosphere was primarily influenced by fast day-to-night winds. While the equatorial jet's influence was much weaker, they were still able to conclude that strong winds were a defining characteristic of WASP-189 b's atmosphere.

What’s Next for WASP-189 b?

The journey doesn't stop here. There are still many questions left unanswered. Scientists hope to conduct further observations that will cover a broader range of the planet’s orbit. By gathering more data over time, they will be able to get a clearer picture of how the atmosphere behaves.

Combining different types of observations can also help fill in the gaps. For example, looking at the planet’s atmosphere from different angles could reveal more about its dynamics and thermal structure.

Summary of Findings

To wrap things up, here’s what we have learned about WASP-189 b:

  • It’s one of the hottest planets known, making it an exciting target for scientists.
  • The winds in its atmosphere are rapid, with notable day-to-night flows and a weaker equatorial jet.
  • The temperature and chemical composition tell us a lot about its unique atmosphere.
  • While much has been uncovered, there’s still more to explore, and future studies promise to shine a light on this intriguing exoplanet.

In short, WASP-189 b is like a hot summer day gone wild, and scientists are just getting started on the journey to understand its wild winds!

Original Source

Title: Retrieving wind properties from the ultra-hot dayside of WASP-189b with CRIRES$^+$

Abstract: The extreme temperature gradients from day- to nightside in the atmospheres of hot Jupiters generate fast winds in the form of equatorial jets or day-to-night flows. Observations of blue-shifted and red-shifted signals in the transmission and dayside spectra of WASP-189b have sparked discussions about the nature of winds on this planet. To investigate the structure of winds in the atmosphere of the ultra-hot Jupiter WASP-189b, we studied its dayside emission spectrum with CRIRES$^+$ in the spectral K band. We used the cross-correlation method to detect emission signals of CO and Fe, and employed a Bayesian framework to retrieve the atmospheric parameters relating to the temperature-pressure structure and chemistry. The retrieval incorporated a numerical model of the line profile influenced by various dynamic effects to determine the wind structure. The cross-correlation signals of CO and Fe showed a velocity offset of ~6km/s, which could be caused by a fast day-to-night wind in the atmosphere of WASP-189b. The atmospheric retrieval showed that the line profile of the observed spectra is best fitted by the presence of a day-to-night wind of 4.4km/s, while the retrieved equatorial jet velocity of 1.0km/s is consistent with the absence of such a jet. Such a wind pattern is consistent with the observed line broadening and can explain the majority of the velocity offset, while uncertainties in the ephemerides and the effects of a hot spot could also contribute to this offset. We further retrieved an inverted temperature-pressure profile and determined the C/O ratio and metallicity. We showed that red-shifts of a few km/s in the dayside spectra could be explained by day-to-night winds. Further studies combining transmission and dayside observations could advance our understanding of WASP-189b's atmospheric circulation by improving the uncertainties in the velocity offset and wind parameters.

Authors: F. Lesjak, L. Nortmann, D. Cont, F. Yan, A. Reiners, N. Piskunov, A. Hatzes, L. Boldt-Christmas, S. Czesla, A. Lavail, E. Nagel, A. D. Rains, M. Rengel, U. Seemann, D. Shulyak

Last Update: 2024-11-29 00:00:00

Language: English

Source URL: https://arxiv.org/abs/2411.19662

Source PDF: https://arxiv.org/pdf/2411.19662

Licence: https://creativecommons.org/licenses/by/4.0/

Changes: This summary was created with assistance from AI and may have inaccuracies. For accurate information, please refer to the original source documents linked here.

Thank you to arxiv for use of its open access interoperability.

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