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HD 189733 b

Coordinates: Sky map 20h 00m 43.7133s, +22° 42′ 39.07″
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HD 189733 b
Size comparison of Jupiter with HD 189733 b.
Discovery
Discovered byBouchy et al.
Discovery siteHaute-Provence Observatory
Discovery date5 October 2005
Doppler spectroscopy
Transit
Orbital characteristics
Apastron0.03102 AU (4,641,000 km)
Periastron0.03096 AU (4,632,000 km)
0.03099 ± 0.0006 AU (4,636,000 ± 90,000 km)
Eccentricity0.0010 ± 0.0002
2.2185733 ± 0.00002 d
53.245759 h
152.5
Inclination85.76 ± 0.29
Semi-amplitude205 ± 6
StarHD 189733 A
Physical characteristics
1.138 ± 0.027 RJ
Mass1.162+0.058
−0.039[1] MJ
21.2 m/s2 (70 ft/s2)
Albedo0.40 ± 0.12 (290–450 nm)
< 0.12 (450–570 nm)
Temperature1117 ± 42 K

HD 189733 b is an exoplanet approximately 64.5 light-years away[2] from the Solar System in the constellation of Vulpecula. The planet was discovered orbiting the star HD 189733 on October 5, 2005, when astronomers in France observed the planet transiting across the face of the star.[3] With a mass 13% higher than that of Jupiter, HD 189733 b orbits its host star once every 2.2 days at an orbital speed of 152.5 kilometres per second (341,000 mph), making it a hot Jupiter with poor prospects for extraterrestrial life. Being the closest transiting hot Jupiter to Earth, HD 189733 b is a subject for extensive atmospheric examination. The atmosphere of HD 189733b has been extensively studied through high- and low-resolution instruments, both from ground and space.[4] HD 189733 b was the first extrasolar planet for which a thermal map was constructed, possibly to be detected through polarimetry[5], to have its overall color determined (deep blue),[5][6] to have a transit detected in X-ray spectrum and to have carbon dioxide detected in its atmosphere.

In July 2014, NASA announced finding very dry atmospheres on three exoplanets (HD 189733b, HD 209458b, WASP-12b) orbiting Sun-like stars.[7]

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.[5]

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.[8] In 2006, a team led by Drake Deming announced a detection of strong infrared thermal 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 13% 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 km/s.

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.[9] 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.[10] This result seemed to be confirmed and refined by the same team in 2011.[5] 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.[5] The blue color of the planet was subsequently confirmed in 2013,[11] which would have made HD 189733 the first planet to have its overall color determined by two different techniques. These measurements in polarized light have since been disputed by two separate teams using more sensitive polarimeters[12][13][14], with upper limits of the polarimetric signal provided therein.

The blueness of the planet 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.[15] The Rayleigh effect is confirmed in other models,[16] 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.[4]

X-ray spectrum

In July 2013, NASA reported the first observations of planet transit studied in X-ray spectrum. It was found that the planet's atmosphere blocks three times more X-rays than visible light.[17]

Evaporation

Short narrated video about the evaporation of HD 189733 b's atmosphere.

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.[18]

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 north-south in our sky. It and HD 209458 b were the first two planets to be directly spectroscopically observed.[9] The parent stars of these two planets are the brightest transiting-planet host stars, so these planets will continue to receive the most attention by 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.[19]

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.[20]

The atmosphere was at first predicted "pL class", lacking a temperature-inversion stratosphere; like L dwarfs which lack titanium and vanadium oxides.[21] Follow-up measurements, tested against a stratospheric model, yielded inconclusive results.[22] Atmospheric condensates form a haze 1000 km above the surface as viewed in the infrared. A sunset viewed from that surface would be red.[23] 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.[24] HD 189733 is also the first extrasolar planet confirmed to have carbon dioxide in its atmosphere.[25]

Map of the planet

An artist's conception of HD 189733 b following the 2013 confirmation of the planet's blue color by the Hubble Space Telescope. The appearance of HD 189733 b beyond the blue color is unknown.

In 2007, the Spitzer space telescope was used to map the planet's temperature emissions. The planet+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 day side 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.[26]

An artist's impression of HD 189733 b showing rapid evaporation of the atmosphere

Scientists at the University of Warwick determined that it has winds of up to 8,700 km/h (5,400 mph) blowing from the day side to the night side.[27] 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.[28]

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.[29] Follow-up observations made using the Hubble Space Telescope confirm the presence of water vapor, neutral oxygen and also the organic compound methane.[16][30][31] Later, Very Large Telescope observations also detected the presence of carbon monoxide on the day side of the planet.[1] 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.[30][32]

Weather and rains of molten glass

NASA Exoplanet Exploration Program "travel poster" for HD 189733 b

The weather on HD 189733b is deadly. The winds, composed of silicate particles, blow up to 8700 km/h (5400 mp/h, 2 km/s and Mach 7). Observations of this planet have also found evidence that it rains molten glass.[33]

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.[34]

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.[35] 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.

Comparison of "hot Jupiter" exoplanets (artist concept).

From top left to lower right: WASP-12b, WASP-6b, WASP-31b, WASP-39b, HD 189733b, HAT-P-12b, WASP-17b, WASP-19b, HAT-P-1b and HD 209458b.

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."[36] 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.[37]

See also

References

  1. ^ a b de Kok, R. J.; et al. (2013). "Detection of carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b". Astronomy and Astrophysics. 554. A82. arXiv:1304.4014. Bibcode:2013A&A...554A..82D. doi:10.1051/0004-6361/201321381.
  2. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. ^ Bouchy, F.; et al. (2005). "ELODIE metallicity-biased search for transiting Hot Jupiters II. A very hot Jupiter transiting the bright K star HD 189733". Astronomy and Astrophysics. 444 (1): L15–L19. arXiv:astro-ph/0510119. Bibcode:2005A&A...444L..15B. doi:10.1051/0004-6361:200500201.
  4. ^ a b Khalafinejad, S.; Essen, C. von; Hoeijmakers, H. J.; Zhou, G.; Klocová, T.; Schmitt, J. H. M. M.; Dreizler, S.; Lopez-Morales, M.; Husser, T.-O. (2017-02-01). "Exoplanetary atmospheric sodium revealed by orbital motion". Astronomy & Astrophysics. 598: A131. arXiv:1610.01610. Bibcode:2017A&A...598A.131K. doi:10.1051/0004-6361/201629473. ISSN 0004-6361.
  5. ^ a b c d e Berdyugina, S.V.; Berdyugin, A.V.; Fluri, D.M.; Piirola, V. (2011). "Polarized reflected light from the exoplanet HD189733b: First multicolor observations and confirmation of detection". Astrophysical Journal Letters. 726 (1): L6–L9. arXiv:1101.0059. Bibcode:2011ApJ...728L...6B. doi:10.1088/2041-8205/728/1/L6.
  6. ^ Kramer, Miriam (11 July 2013). "Strange Blue World: Alien Planet's True Color Revealed, a First". Space.com. TechMediaNetwork. Retrieved 11 July 2013.
  7. ^ Harrington, J.D.; Villard, Ray (July 24, 2014). "RELEASE 14-197 - Hubble Finds Three Surprisingly Dry Exoplanets". NASA. Retrieved July 25, 2014.
  8. ^ https://www.aanda.org/articles/aa/abs/2005/46/aahi291/aahi291.html
  9. ^ a b Press Release: NASA's Spitzer First To Crack Open Light of Faraway Worlds Archived 2007-07-15 at the Wayback Machine
  10. ^ Berdyugina, Svetlana V.; Andrei V. Berdyugin; Dominique M. Fluri; Vilppu Piirola (20 January 2008). "First detection of polarized scattered light from an exoplanetary atmosphere" (PDF). The Astrophysical Journal. 673 (1): L83–L86. arXiv:0712.0193. Bibcode:2008ApJ...673L..83B. doi:10.1086/527320.[permanent dead link]
  11. ^ First distant planet to be seen in colour is blue Nature 11 July 2013
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  13. ^ Wiktorowicz, Sloane J.; Nofi, Larissa A.; Jontof-Hutter, Daniel; Kopparla, Pushkar; Laughlin, Gregory P.; Hermis, Ninos; Yung, Yuk L.; Swain, Mark R. (2015-10-27). "A GROUND-BASED ALBEDO UPPER LIMIT FOR HD 189733b FROM POLARIMETRY". The Astrophysical Journal. 813 (1): 48. arXiv:1507.03588. Bibcode:2015ApJ...813...48W. doi:10.1088/0004-637X/813/1/48. ISSN 1538-4357.
  14. ^ Bott, Kimberly; Bailey, Jeremy; Kedziora-Chudczer, Lucyna; Cotton, Daniel V.; Lucas, P. W.; Marshall, Jonathan P.; Hough, J. H. (2016-03-20). "The polarization of HD 189733" (PDF). Monthly Notices of the Royal Astronomical Society: Letters. 459 (1): L109–L113. Bibcode:2016MNRAS.459L.109B. doi:10.1093/mnrasl/slw046. ISSN 1745-3925.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  15. ^ A. Lecavelier des Etangs; F. Pont; A. Vidal-Madjar; D. Sing (2008). "Rayleigh scattering in the transit spectrum of HD 189733b". Astronomy & Astrophysics. 481 (2): L83–L86. arXiv:0802.3228. Bibcode:2008A&A...481L..83L. doi:10.1051/0004-6361:200809388. Retrieved 2008-08-08.
  16. ^ a b Eric Agol; et al. (2008). "Transits and secondary eclipses of HD 189733 with Spitzer". Proceedings of the International Astronomical Union. 4: 209–215. arXiv:0807.2434. doi:10.1017/S1743921308026422.
  17. ^ NASA's Chandra Sees Eclipsing Planet in X-rays for First Time
  18. ^ Lecavelier des Etangs; et al. (2010-03-10). "Evaporation of the planet HD189733b observed in HI Lyman-alpha" (PDF). Astronomy & Astrophysics. 1003: 2206. arXiv:1003.2206. Bibcode:2010A&A...514A..72L. doi:10.1051/0004-6361/200913347.
  19. ^ Frédéric Pont; et al. (2008). "Hubble Space Telescope time-series photometry of the planetary transit of HD189733: no moon, no rings, starspots". Astronomy and Astrophysics. 476 (3): 1347–1355. arXiv:0707.1940. Bibcode:2007A&A...476.1347P. doi:10.1051/0004-6361:20078269.
  20. ^ Polarization technique focuses limelight, 12/26/2007
  21. ^ Fortney, J. J.; Lodders, K.; Marley, M. S.; Freedman, R. S. (2008). "A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres". Astrophysical Journal. 678 (2): 1419–1435. arXiv:0710.2558. Bibcode:2008ApJ...678.1419F. doi:10.1086/528370.
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  23. ^ F. Pont; et al. (2008). "Detection of atmospheric haze on an extrasolar planet: The 0.55 – 1.05 micron transmission spectrum of HD189733b with the Hubble Space Telescope". Monthly Notices of the Royal Astronomical Society. 385 (1): 109–118. arXiv:0712.1374. Bibcode:2008MNRAS.385..109P. doi:10.1111/j.1365-2966.2008.12852.x.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  24. ^ 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.
  25. ^ Robert Roy Britt (November 24, 2008). "Carbon Dioxide Detected on Faraway World". Space.com.
  26. ^ Iro, Nicolas; Bruno Bezard; T. Guillot (June 2005). "A time-dependent radiative model of HD 209458b". Astronomy and Astrophysics. 436 (2): 719–727. arXiv:astro-ph/0409468. Bibcode:2005A&A...436..719I. doi:10.1051/0004-6361:20048344.
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  29. ^ Press Release: NASA's Spitzer Finds Water Vapor on Hot, Alien Planet
  30. ^ a b Swain, Mark R.; Vasisht, Gautam; Tinetti, Giovanna (2008-03-20). "The presence of methane in the atmosphere of an extrasolar planet". Nature. 452 (7185): 329–331. Bibcode:2008Natur.452..329S. doi:10.1038/nature06823. PMID 18354477. arXiv.org link
  31. ^ Hubble Space Telescope detection of oxygen in the atmosphere of exoplanet HD189733b: Lotfi Ben-Jaffel, Gilda Ballester
  32. ^ Stephen Battersby (2008-02-11). "Organic molecules found on alien world for first time". Retrieved 2008-02-12.
  33. ^ Loff, Sarah (2016-10-31). "Rains of Terror on Exoplanet HD 189733b". NASA. Retrieved 2019-12-13.
  34. ^ "HD 189733 page". University of Geneva. 2007-03-05. Retrieved 2008-02-18.
  35. ^ Gregory W. Henry; et al. (2008). "The Rotation Period of the Planet-Hosting Star HD 189733". The Astronomical Journal. 135 (1): 68–71. arXiv:0709.2142. Bibcode:2008AJ....135...68H. doi:10.1088/0004-6256/135/1/68.
  36. ^ Route, Matthew (February 10, 2019). "The Rise of ROME. I. A Multiwavelength Analysis of the Star-Planet Interaction in the HD 189733 System". The Astrophysical Journal. 872 (1): 79. arXiv:1901.02048. Bibcode:2019ApJ...872...79R. doi:10.3847/1538-4357/aafc25.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  37. ^ Route, Matthew; Looney, Leslie (December 20, 2019). "ROME (Radio Observations of Magnetized Exoplanets). II. HD 189733 Does Not Accrete Significant Material from Its Exoplanet Like a T Tauri Star from a Disk". The Astrophysical Journal. 887 (2): 229. arXiv:1911.08357. Bibcode:2019ApJ...887..229R. doi:10.3847/1538-4357/ab594e.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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