1,192±9
K (919 °C; 1,686 °F)[5] 1,490±68 K (1,220 °C; 2,220 °F)[6]
HD 189733 b is an
exoplanet in the constellation of
Vulpecula approximately 64.5
light-years (19.8
parsecs) away[7] from the
Solar System. Astronomers in France discovered the planet orbiting the star
HD 189733 on October 5, 2005, by observing its
transit across the star's face.[1] With a mass 11.2% higher than that of
Jupiter and a radius 11.4% greater, HD 189733 b orbits its host star once every 2.2 days at an
orbital speed of 152.0 kilometers per second (152,000 meters per second; 340,000 miles per hour), making it a
hot Jupiter with poor prospects for
extraterrestrial life.[2]
The closest transiting hot Jupiter to Earth, HD 189733 b has been the subject of close atmospheric observation. Scientists have studied it with high- and low-resolution instruments, both from the ground and from space.[8] Researchers have found that the planet's weather includes raining molten glass. HD 189733 b was also the first exoplanet to have its
thermal map constructed,[9][10] possibly to be detected through
polarimetry,[11] its overall color determined (deep blue),[11][3] its transit viewed in the X-ray spectrum, and to have
carbon dioxide confirmed as being present in its atmosphere.
In July 2014,
NASA announced the discovery of very dry
atmospheres on three exoplanets that orbited Sun-like stars: HD 189733 b,
HD 209458 b, and
WASP-12b.[12]
Detection and discovery
Transit and Doppler spectroscopy
The infrared spectrum of HD 189733 b
A global temperature map of HD 189733 b
The planet's blue color was revealed using polarimetry.[11]
On October 6, 2005, a team of astronomers announced the discovery of transiting planet HD 189733 b. The planet was then detected using
Doppler spectroscopy. Real-time
radial velocity measurements detected the
Rossiter–McLaughlin effect caused by the planet passing in front of its star before photometric measurements confirmed that the planet was transiting.[1] In 2006, a team led by
Drake Deming announced detection of strong
infraredthermal emission from the transiting exoplanet planet HD 189733 b, by measuring the flux decrement (decrease of total light) during its prominent secondary
eclipse (when the planet passes behind the star).
The mass of the planet is estimated to be 16% larger than
Jupiter's, with the planet completing an orbit around its host star every 2.2 days and an
orbital speed of 152.5 kilometres per second (341,000 mph).
Infrared spectrum
On February 21, 2007,
NASA released news that the
Spitzer Space Telescope had measured detailed
spectra from both HD 189733 b and
HD 209458 b.[13] The release came simultaneously with the public release of a new issue of Nature containing the first publication on the spectroscopic observation of the other exoplanet, HD 209458 b. A paper was submitted and published by the Astrophysical Journal Letters. The spectroscopic observations of HD 189733 b were led by Carl Grillmair of NASA's
Spitzer Science Center.
Visible color
In 2008, a team of astrophysicists appeared to have detected and monitored the planet's visible light using
polarimetry, which would have been the first such success.[14] This result seemed to be confirmed and refined by the same team in 2011.[11] They found that the planet
albedo is significantly larger in blue light than in the red, most probably due to
Rayleigh scattering and molecular absorption in the red.[11] The blue color of the planet was subsequently confirmed in 2013,[3][15] which would have made HD 189733 the first planet to have its overall color determined by two different techniques. The measurements in polarized light have since been disputed by two separate teams using more sensitive polarimeters,[16][17][18] with upper limits of the polarimetric signal provided therein.
The rich
cobalt blue[19][20] colour of HD 189733 b may be the result of
Rayleigh scattering. In mid January 2008, spectral observation during the planet's transit using that model found that if molecular
hydrogen exists, it would have an
atmospheric pressure of 410 ± 30
mbar of 0.1564 solar radii. The Mie approximation model also found that there is a possible condensate in its atmosphere,
magnesium silicate (MgSiO3) with a
particle size of approximately 10−2 to 10−1 μm. Using both models, the planet's temperature would be between 1340 and 1540 K.[21] The Rayleigh effect is confirmed in other models,[22] and by the apparent lack of a cooler, shaded
stratosphere below its outer atmosphere. In the visible region of the spectrum, thanks to their high absorption cross sections, atomic sodium and potassium can be investigated. For example, using high-resolution
UVES spectrograph on
VLT, sodium has been detected on this atmosphere and further physical characteristics of the atmosphere such as temperature has been investigated.[8]
X-ray spectrum
In July 2013, NASA reported the first observations of planet transit studied in the X-ray spectrum. It was found that the planet's atmosphere blocks three times more X-rays than visible light.[23]
Evaporation
In March 2010, transit observations using HI Lyman-alpha found that this planet is evaporating at a rate of 1-100 gigagrams per second. This indication was found by detecting the extended
exosphere of atomic hydrogen. HD 189733 b is the second planet after
HD 209458 b for which atmospheric evaporation has been detected.[24]
Physical characteristics
This planet exhibits one of the largest
photometric transit depth (amount of the parent star's light blocked) of
extrasolar planets so far observed, approximately 3%. The apparent
longitude of ascending node of its orbit is 16 degrees +/- 8 away from the north–south in our sky. It and
HD 209458 b were the first two planets to be directly
spectroscopically observed.[13] The parent stars of these two planets are the brightest transiting-planet host stars, so these planets will continue to receive the most attention from astronomers. Like most hot Jupiters, this planet is thought to be tidally locked to its parent star, meaning it has a permanent day and night.
The planet is not
oblate, and has neither satellites with greater than 0.8 the radius of Earth nor a ring system like that of Saturn.[25]
The international team under the direction of Svetlana Berdyugina of Zurich University of Technology, using the Swedish 60-centimeter telescope KVA, which is located in Spain, was able to directly see the polarized light reflected from the planet. The polarization indicates that the scattering atmosphere is considerably larger (> 30%) than the opaque body of the planet seen during transits.[26]
The atmosphere was at first predicted "pL class", lacking a temperature-inversion
stratosphere; like
L dwarfs which lack titanium and vanadium oxides.[27] Follow-up measurements, tested against a stratospheric model, yielded inconclusive results.[28] Atmospheric condensates form a haze 1,000 kilometres (620 mi) above the surface as viewed in the infrared. A sunset viewed from that surface would be red.[29] Sodium and potassium signals were predicted by Tinetti 2007. First obscured by the haze of condensates, sodium was eventually observed at three times the concentration of
HD 209458 b's sodium layer.[30] The potassium was also detected in 2020, although in significantly smaller concentrations.[31] HD 189733 is also the first extrasolar planet confirmed to have carbon dioxide in its atmosphere.[32]
Map of the planet
In 2007, the
Spitzer Space Telescope was used to map the planet's temperature emissions. The planet and star system was observed for 33 consecutive hours, starting when only the night side of the planet was in view. Over the course of one-half of the planet's orbit, more and more of the dayside came into view. A temperature range of 973 ± 33 K to 1,212 ± 11 K was discovered, indicating that the absorbed energy from the parent star is distributed fairly evenly through the planet's atmosphere. The region of peak temperature was offset 30 degrees east of the substellar point, as predicted by theoretical models of hot Jupiters taking into account a parameterized day to night redistribution mechanism.[9]
Scientists at the
University of Warwick determined that HD 189733 b has winds of up to 8,700 km/h (5,400 mph) blowing from the day side to the night side.[33] NASA released a brightness map of the surface temperature of HD 189733 b; it is the first map ever published of an extra-solar planet.[34]
Water vapor, oxygen, and organic compounds
On July 11, 2007, a team led by
Giovanna Tinetti published the results of their observations using the Spitzer Space Telescope concluding there is solid evidence for significant amounts of water vapor in the planet's atmosphere.[35] Follow-up observations made using the
Hubble Space Telescope confirm the presence of water vapor, neutral oxygen and also the organic compound
methane.[22][36][37] Later,
Very Large Telescope observations also detected the presence of
carbon monoxide on the day side of the planet.[38] It is currently unknown how the methane originated as the planet's high 700 °C temperature should cause the water and methane to react, replacing the atmosphere with carbon monoxide.[36][39] Nonetheless, the presence of roughly 0.004% of water vapour fraction by volume in atmosphere of HD 189733 b was confirmed with high-resolution emission spectra taken in 2021.[40]
Weather and rains of molten glass
The weather on HD 189733b is deadly. The winds, composed of silicate particles, blow up to 8,700 kilometres per hour (5,400 mph). Observations of this planet have also found evidence that it rains molten glass, horizontally.[41]
Evolution
While transiting the system also clearly exhibits the
Rossiter–McLaughlin effect, shifting in
photospheric spectral lines caused by the planet occulting a part of the rotating stellar surface. Due to its high mass and close orbit, the parent star has a very large
semi-amplitude (K), the "wobble" in the star's
radial velocity, of 205 m/s.[42]
The Rossiter–McLaughlin effect allows the measurement of the angle between the planet's orbital plane and the equatorial plane of the star. These are well aligned,[43] misalignment equal to -0.5±0.4°.[44] By analogy with
HD 149026 b, the formation of the planet was peaceful and probably involved interactions with the
protoplanetary disc. A much larger angle would have suggested a violent interplay with other protoplanets.
Star-planet interaction controversy
In 2008, a team of astronomers first described how as the exoplanet orbiting HD 189733 A reaches a certain place in its orbit, it causes increased
stellar flaring. In 2010, a different team found that every time they observe the exoplanet at a certain position in its orbit, they also detected
X-ray flares. Theoretical research since 2000 suggested that an exoplanet very near to the star that it orbits may cause increased flaring due to the interaction of their
magnetic fields, or because of
tidal forces. In 2019, astronomers analyzed data from
Arecibo Observatory,
MOST, and the Automated Photoelectric Telescope, in addition to historical observations of the star at radio, optical, ultraviolet, and X-ray wavelengths to examine these claims. They found that the previous claims were exaggerated and the host star failed to display many of the brightness and spectral characteristics associated with stellar flaring and solar
active regions, including sunspots. Their statistical analysis also found that many stellar flares are seen regardless of the position of the exoplanet, therefore debunking the earlier claims. The magnetic fields of the host star and exoplanet do not interact, and this system is no longer believed to have a "star-planet interaction."[45] Some researchers had also suggested that HD 189733 accretes, or pulls, gas from its orbiting exoplanet at a rate similar to those found around young
protostars in
T Tauri Star systems. Later analysis demonstrated that very little, if any, gas was accreted from the "hot Jupiter" companion.[46]
Possible exomoons
Some studies have proposed candidate
exomoons around HD 189733 b. A 2014 study proposed a moon based on studying periodic increases and decreases in light given off from HD 189733 b. This moon would be outside of the planet's
Hill sphere, making its existence implausible.[47] Two studies by the same team in 2019 and 2020 proposed exo-
Io candidates around a number of hot Jupiters, including HD 189733 b and
WASP-49b, based on detected
sodium[48] and
potassium,[49] consistent with evaporating exomoons and/or their corresponding
gas torus.[50][51] A follow-up study in 2022 did not find evidence for an exomoon around HD 189733 b.[52]
^Berdyugina, Svetlana V.; Andrei V. Berdyugin; Dominique M. Fluri; Vilppu Piirola (20 January 2008). "First detection of polarized scattered light from an exoplanetary atmosphere". The Astrophysical Journal. 673 (1): L83–L86.
arXiv:0712.0193.
Bibcode:
2008ApJ...673L..83B.
doi:
10.1086/527320.
S2CID14366978.
^Redfield; Endl, Michael; Cochran, William D.; Koesterke, Lars (2008). "Sodium Absorption from the Exoplanetary Atmosphere of HD 189733b Detected in the Optical Transmission Spectrum". The Astrophysical Journal Letters. 673 (1): L87–L90.
arXiv:0712.0761.
Bibcode:
2008ApJ...673L..87R.
doi:
10.1086/527475.
S2CID2028887.
^Keles, E.; Kitzmann, D.; Mallonn, M.; Alexoudi, X.; Fossati, L.; Pino, L.; Seidel, J. V.; Carroll, T. A.; Steffen, M.; Ilyin, I.; Poppenhäger, K.; Strassmeier, K. G.; Von Essen, C.; Nascimbeni, V.; Turner, J. D. (2020), "Probing the atmosphere of HD189733b with the Na i and K i lines", Monthly Notices of the Royal Astronomical Society, 498: 1023–1033,
arXiv:2008.04044,
doi:
10.1093/mnras/staa2435