HD 189733 b
Jupiter and HD 189733 b compared
Discovery[1]
Discovered byBouchy et al.
Discovery siteHaute-Provence Observatory
Discovery dateOctober 5, 2005
Doppler spectroscopy
Transit
Orbital characteristics[2]
0.03100 ± 0.0006 AU (4,638,000 ± 90,000 km)
Eccentricity<0.0039
2.218575200(77) d
53.2458048 h
152.0 km/s
Inclination85.580°±0.060°
Semi-amplitude201.3±1.6 m/s
StarHD 189733
Physical characteristics[2]
Mean radius
1.138±0.027 RJ
Mass1.123±0.045 MJ
Mean density
0.943+0.081
−0.072 g/cm3
21.5 m/s2 (2.2 g)
Albedo0.40±0.12 (290–450 nm)[3]
<0.12 (450–570 nm)[3]
0.076±0.016 (geometric)[4]
Temperature1,192±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 our 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 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 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 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.[19] The Rayleigh effect is confirmed in other models,[20] 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.[21]

    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.[22]

    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.[23]

    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.[24]

    The atmosphere was at first predicted "pL class", lacking a temperature-inversion stratosphere; like L dwarfs which lack titanium and vanadium oxides.[25] Follow-up measurements, tested against a stratospheric model, yielded inconclusive results.[26] 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.[27] 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.[28] The potassium was also detected in 2020, although in significantly smaller concentrations.[29] HD 189733 is also the first extrasolar planet confirmed to have carbon dioxide in its atmosphere.[30]

    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 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]

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

    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.[31] 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.[32]

    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.[33] Follow-up observations made using the Hubble Space Telescope confirm the presence of water vapor, neutral oxygen and also the organic compound methane.[20][34][35] Later, Very Large Telescope observations also detected the presence of carbon monoxide on the day side of the planet.[36] 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.[34][37] 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.[38]

    Weather and rains of molten glass

    NASA Exoplanet Exploration Program "horror film poster" for HD 189733 b

    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.[39]

    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.[40]

    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,[41] misalignment equal to -0.5±0.4°.[42] 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 189733 b, HAT-P-12b, WASP-17b, WASP-19b, HAT-P-1b and HD 209458 b.

    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."[43] 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.[44]

    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.[45] 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[46] and potassium,[47] consistent with evaporating exomoons and/or their corresponding gas torus.[48][49] A follow-up study in 2022 did not find evidence for an exomoon around HD 189733 b.[50]

    See also

    References

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    2. 1 2 3 Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics. 602: A107. arXiv:1704.00373. Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID 118923163.
    3. 1 2 3 4 Evans, Thomas M.; Pont, Frédéric; et al. (August 2013). "The Deep Blue Color of HD 189733b: Albedo Measurements with Hubble Space Telescope/Space Telescope Imaging Spectrograph at Visible Wavelengths". The Astrophysical Journal Letters. 772 (2): L16. arXiv:1307.3239. Bibcode:2013ApJ...772L..16E. doi:10.1088/2041-8205/772/2/L16. S2CID 38344760.
    4. ↑ Krenn, A. F.; Lendl, M.; et al. (April 2023). "The geometric albedo of the hot Jupiter HD 189733b measured with CHEOPS". Astronomy & Astrophysics. 672: A24. arXiv:2301.07731. Bibcode:2023A&A...672A..24K. doi:10.1051/0004-6361/202245016. S2CID 255999905.
    5. ↑ Knutson, Heather A.; Lewis, Nikole; et al. (July 2012). "3.6 and 4.5 μm Phase Curves and Evidence for Non-equilibrium Chemistry in the Atmosphere of Extrasolar Planet HD 189733b". The Astrophysical Journal. 754 (1): 22. arXiv:1206.6887. Bibcode:2012ApJ...754...22K. doi:10.1088/0004-637X/754/1/22. S2CID 51760187.
    6. ↑ Pass, Emily K.; Cowan, Nicolas B.; et al. (October 2019). "Estimating dayside effective temperatures of hot Jupiters and associated uncertainties through Gaussian process regression". Monthly Notices of the Royal Astronomical Society. 489 (1): 941–950. arXiv:1908.02631. Bibcode:2019MNRAS.489..941P. doi:10.1093/mnras/stz2226.
    7. ↑ Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
    8. 1 2 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. S2CID 55263138.
    9. 1 2 Knutson, Heather A.; Charbonneau, David; et al. (May 2007). "A map of the day-night contrast of the extrasolar planet HD 189733b". Nature. 447 (7141): 183–186. arXiv:0705.0993. Bibcode:2007Natur.447..183K. doi:10.1038/nature05782. PMID 17495920.
    10. ↑ Majeau, Carl; Agol, Eric; Cowan, Nicolas B. (March 2012). "A Two-dimensional Infrared Map of the Extrasolar Planet HD 189733b". The Astrophysical Journal Letters. 747 (2): L20. arXiv:1202.1883. Bibcode:2012ApJ...747L..20M. doi:10.1088/2041-8205/747/2/L20. S2CID 118492172.
    11. 1 2 3 4 5 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. S2CID 59160192.
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    13. 1 2 "Press Release: NASA's Spitzer First To Crack Open Light of Faraway Worlds". Archived from the original on July 15, 2007.
    14. ↑ 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. S2CID 14366978.
    15. ↑ Powell, Devin (July 11, 2013). "First distant planet to be seen in colour is blue". Nature. doi:10.1038/nature.2013.13376. S2CID 130070356 – via www.nature.com.
    16. ↑ Wiktorowicz, Sloane J. (2009-04-22). "NONDETECTION OF POLARIZED, SCATTERED LIGHT FROM THE HD 189733b HOT JUPITER". The Astrophysical Journal. 696 (2): 1116–1124. arXiv:0902.0624. Bibcode:2009ApJ...696.1116W. doi:10.1088/0004-637X/696/2/1116. ISSN 0004-637X. S2CID 11384636.
    17. ↑ 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. S2CID 118086125.
    18. ↑ 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. arXiv:1603.05745. Bibcode:2016MNRAS.459L.109B. doi:10.1093/mnrasl/slw046. ISSN 1745-3925.
    19. ↑ 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. S2CID 18738916. Retrieved 2008-08-08.
    20. 1 2 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. S2CID 15867430.
    21. ↑ Boen, Brooke (May 20, 2015). "NASA's Chandra Sees Eclipsing Planet in X-rays for First Time". NASA.
    22. ↑ 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. S2CID 53408874.
    23. ↑ 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. S2CID 18293269.
    24. ↑ Polarization technique focuses limelight, 12/26/2007
    25. ↑ 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. S2CID 17502177.
    26. ↑ Ivan Hubeny; Adam Burrows (2008). "Spectrum and atmosphere models of irradiated transiting extrasolar giant planets". Proceedings of the International Astronomical Union. 4: 239–245. arXiv:0807.3588. Bibcode:2009IAUS..253..239H. doi:10.1017/S1743921308026458. S2CID 13978248.
    27. ↑ 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. S2CID 10831981.
    28. ↑ 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. S2CID 2028887.
    29. ↑ 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
    30. ↑ Robert Roy Britt (November 24, 2008). "Carbon Dioxide Detected on Faraway World". Space.com.
    31. ↑ Klotz, Irene (November 16, 2015). "Exoplanet's Global Winds Let Rip at 5,400 MPH". Space. Retrieved 2015-11-17.
    32. ↑ "First Map of Alien World". Spitzer Space Telescope. Jet Propulsion Laboratory. 2007-05-09. Retrieved 2009-09-30.
    33. ↑ "Press Release: NASA's Spitzer Finds Water Vapor on Hot, Alien Planet". Archived from the original on 2007-07-15. Retrieved 2007-07-11.
    34. 1 2 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. arXiv:0802.1030. Bibcode:2008Natur.452..329S. doi:10.1038/nature06823. PMID 18354477. S2CID 205212651.
    35. ↑ Ben-Jaffel, Lotfi; Ballester, Gilda (May 18, 2013). "Hubble Space Telescope detection of oxygen in the atmosphere of exoplanet HD189733b". Astronomy & Astrophysics. 553: A52. arXiv:1303.4232. Bibcode:2013A&A...553A..52B. doi:10.1051/0004-6361/201221014. S2CID 119311496.
    36. ↑ 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. S2CID 55266595.
    37. ↑ Stephen Battersby (2008-02-11). "Organic molecules found on alien world for first time". Retrieved 2008-02-12.
    38. ↑ Boucher, Anne; et al. (9 November 2021). "Characterizing Exoplanetary Atmospheres at High Resolution with SPIRou: Detection of Water on HD 189733 b". The Astronomical Journal. 162 (6). 233. arXiv:2108.08390. Bibcode:2021AJ....162..233B. doi:10.3847/1538-3881/ac1f8e.
    39. ↑ Loff, Sarah (2016-10-31). "Rains of Terror on Exoplanet HD 189733b". NASA. Retrieved 2019-12-13.
    40. ↑ "HD 189733 page". University of Geneva. 2007-03-05. Retrieved 2008-02-18.
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    42. ↑ Albrecht, Simon; Winn, Joshua N.; Johnson, John A.; Howard, Andrew W.; Marcy, Geoffrey W.; Butler, R. Paul; Arriagada, Pamela; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B.; Hirano, Teruyuki; Bakos, Gaspar; Hartman, Joel D. (2012), "Obliquities of Hot Jupiter Host Stars: Evidence for Tidal Interactions and Primordial Misalignments", The Astrophysical Journal, 757 (1): 18, arXiv:1206.6105, Bibcode:2012ApJ...757...18A, doi:10.1088/0004-637X/757/1/18, S2CID 17174530
    43. ↑ 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. S2CID 119350145.
    44. ↑ 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. S2CID 208158242.
    45. ↑ Ben-Jaffel, Lotfi; Ballester, Gilda (3 April 2014). "Transit of Exomoon Plasma Tori: New Diagnosis". The Astrophysical Journal. 785 (2): L30. arXiv:1404.1084. Bibcode:2014ApJ...785L..30B. doi:10.1088/2041-8205/785/2/L30. S2CID 119282630.
    46. ↑ Wyttenbach, A.; Ehrenreich, D.; Lovis, C.; Udry, S.; Pepe, F. (5 May 2015). "Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph". Astronomy & Astrophysics. 577: A62. arXiv:1503.05581. Bibcode:2015A&A...577A..62W. doi:10.1051/0004-6361/201525729. S2CID 54935174.
    47. ↑ Keles, Engin; Mallonn, Matthias; von Essen, Carolina; Carroll, Thorsten; Alexoudi, Xanthippi; Pino, Lorenzo; Ilyin, Ilya; Poppenhager, Katja; Kitzmann, Daniel; Nascimbeni, Valerio; Turner, Jake D; Strassmeier, Klaus G (October 2019). "The potassium absorption on HD189733b and HD209458b". Monthly Notices of the Royal Astronomical Society: Letters. 489 (1): L37-L41. arXiv:1909.04884. Bibcode:2019MNRAS.489L..37K. doi:10.1093/mnrasl/slz123. S2CID 202134796.
    48. ↑ Oza, Apurva V.; Johnson, Robert E.; Lellouch, Emmanuel; Schmidt, Carl; Schneider, Nick; Huang, Chenliang; Gamborino, Diana; Gebek, Andrea; Wyttenbach, Aurelien; Demory, Brice-Olivier; Mordasini, Christoph; Saxena, Prabal; Dubois, David; Moullet, Arielle; Thomas, Nicolas (2019-08-28). "Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets". The Astrophysical Journal. 885 (2): 168. arXiv:1908.10732. Bibcode:2019ApJ...885..168O. doi:10.3847/1538-4357/ab40cc. S2CID 201651224.
    49. ↑ Gebek, Andrea; Oza, Apurva (29 July 2020). "Alkaline exospheres of exoplanet systems: evaporative transmission spectra". Monthly Notices of the Royal Astronomical Society. 497 (4): 5271–5291. arXiv:2005.02536. Bibcode:2020MNRAS.497.5271G. doi:10.1093/mnras/staa2193. S2CID 218516741. Retrieved 8 December 2020.
    50. ↑ Narang, Mayank; Oza, Apurva V.; et al. (January 2023). "Radio-loud Exoplanet-exomoon Survey: GMRT Search for Electron Cyclotron Maser Emission". The Astronomical Journal. 165 (1): 1. arXiv:2210.13298. Bibcode:2023AJ....165....1N. doi:10.3847/1538-3881/ac9eb8.
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