In 2017, traces of water were discovered in the planet's atmosphere.[4] In 2019, the Nobel Prize in Physics was awarded in part for the discovery of 51 Pegasi b.[5]
The planet was discovered using a sensitive spectroscope that could detect the slight and regular velocity changes in the star's spectral lines of around 70 metres per second. These changes are caused by the planet's gravitational effects from just 7 million kilometres' distance from the star.
Promotional "Exoplanet Travel Bureau" poster from NASA
After its discovery, many teams confirmed the planet's existence and obtained more observations of its properties. It was discovered that the planet orbits the star in around four days. It is much closer to it than Mercury is to the Sun,[2] moves at an orbital speed of 136 km/s (300,000 mph), yet has a minimum mass about half that of Jupiter (about 150 times that of the Earth). At the time, the presence of a huge world so close to its star was not compatible with theories of planet formation and was considered an anomaly. However, since then, numerous other "hot Jupiters" have been discovered[2] (such as 55 Cancri and τ Boötis), and astronomers are revising their theories of planet formation to account for them by studying orbital migration.[3]
Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be 1,265 K (992 °C; 1,817 °F). This is between the predicted temperatures of HD 189733 b and HD 209458 b (1,180 K (910 °C; 1,660 °F)–1,392 K (1,119 °C; 2,046 °F)), before they were measured.[13]
In the report of the discovery, it was initially speculated that 51 Pegasi b was the stripped core of a brown dwarf of a decomposed star and was therefore composed of heavy elements, but it is now believed to be a gas giant. It is sufficiently massive that its thick atmosphere is not blown away by the star's solar wind.
51 Pegasi b probably has a greater radius than that of Jupiter despite its lower mass. This is because its superheated atmosphere must be puffed up into a thick but tenuous layer surrounding it. Beneath this, the gases that make up the planet would be so hot that the planet would glow red. Clouds of silicates may exist in the atmosphere.
The planet is tidally locked to its star, always presenting the same face to it.
The first ever direct detection of the visible light spectrum reflected from an exoplanet has been made by an international team of astronomers on 51 Pegasi b. The astronomers studied light from 51 Pegasi b using the High Accuracy Radial velocity Planet Searcher (HARPS) instrument at the European Southern Observatory's La Silla Observatory in Chile.[15] This detection allowed the inference of a mass of 0.46 Jupiter masses.[16] The optical detection could not be replicated in 2020, implying the planet has an albedo below 0.15.[17] Measurements in 2021 have marginally detected a polarized reflected light signal, which, while they cannot place limits on the albedo without assumptions made about the scattering mechanisms, could suggest a high albedo.[18]
^Martins, J. H. C.; Santos, N. C.; Figueira, P.; Faria, J. P.; Montalto, M.; Boisse, I.; Ehrenreich, D.; Lovis, C.; Mayor, M.; Melo, C.; Pepe, F.; Sousa, S. G.; Udry, S.; Cunha, D. (2015). "Evidence for a spectroscopic direct detection of reflected light from 51 Pegasi b". Astronomy & Astrophysics. 576: A134. arXiv:1504.05962. Bibcode:2015A&A...576A.134M. doi:10.1051/0004-6361/201425298. S2CID119224213.
^Scandariato, G.; Borsa, F.; Sicilia, D.; Malavolta, L.; et al. (2020). "The GAPS Programme at TNG. XXIX. No detection of reflected light from 51 Peg b using optical high-resolution spectroscopy". Astronomy & Astrophysics. 646: A159. arXiv:2012.10435. Bibcode:2021A&A...646A.159S. doi:10.1051/0004-6361/202039271.
^Bailey, Jeremy; Bott, Kimberly; Cotton, Daniel V.; Kedziora-Chudczer, Lucyna; Zhao, Jinglin; Evensberget, Dag; Marshall, Jonathan P.; Wright, Duncan; Lucas, P. W. (2021), "Polarization of hot Jupiter systems: A likely detection of stellar activity and a possible detection of planetary polarization", Monthly Notices of the Royal Astronomical Society, 502 (2): 2331–2345, arXiv:2101.07411, doi:10.1093/mnras/stab172
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