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WASP-76b

WASP-76b is an ultra-hot Jupiter exoplanet, a gas giant with a mass of 0.92 ± 0.03 Jupiter masses and a radius of 1.83 ± 0.06 Jupiter radii, orbiting the F7-type star WASP-76 every 1.81 days at a semi-major axis of 0.033 AU.^[1] Located approximately 637 light-years from Earth in the constellation Pisces, it is tidally locked, resulting in extreme temperature contrasts between its scorching dayside, where temperatures exceed 2400°C and vaporize iron, and its cooler night side, where iron condenses and falls as molten rain.^[2]^[3] The planet's atmosphere exhibits asymmetric chemistry, with depleted gaseous iron on the morning limb due to night-side condensation, and recent observations indicate a possible glory effect—a rainbow-like scattering phenomenon—potentially from uniform spherical droplets.^[4] Discovered in 2016 through the transit method by the Wide Angle Search for Planets (WASP) survey, confirmed by radial velocity measurements from the SOPHIE and CORALIE spectrographs, WASP-76b was identified as one of three bloated hot Jupiters receiving intense stellar irradiation that inflates its atmosphere.^[1] The host star WASP-76 has a mass of ≈1.43 M_⊙, a radius of 1.76 R_⊙, and an effective temperature of ≈6300 K (updated as of 2024), making it slightly hotter and larger than the Sun.^[4] Its proximity to the star—12 times closer than Mercury to the Sun—drives the planet's ultra-hot classification, with dayside temperatures around 2630 K and night-side temperatures inferred to be hundreds of Kelvin cooler.^[4] Subsequent observations have revealed a dynamic atmosphere dominated by metal vapors and strong winds carrying iron from the dayside to the night side at speeds of several km/s.^[3] High-resolution spectroscopy has indicated possible presence of titanium oxide (TiO) and vanadium oxide (VO) in the atmosphere, contributing to its opacity and thermal structure.^[4] Data from ESA's Cheops, NASA's Hubble Space Telescope, TESS, and Spitzer have confirmed atmospheric asymmetry and a geometric albedo of about 0.11, suggesting reflective properties possibly enhanced by the proposed glory.^[4] In 2025, observations with GIANO-B and HARPS-N detected CO and Fe I on the dayside, further probing atmospheric dynamics.^[5] WASP-76b serves as a benchmark for studying ultra-hot Jupiters, with future observations from the James Webb Space Telescope expected to probe deeper into its 3D atmospheric dynamics and composition.^[2]

Discovery and designation

Discovery

WASP-76b was discovered through the transit method as part of the Wide Angle Search for Planets (WASP) project, which employs wide-field photometric surveys to detect short-period giant planets orbiting bright stars. The SuperWASP survey, utilizing camera arrays at both northern and southern observatories, identified periodic dips in the light curve of the host star WASP-76, indicating the presence of a transiting exoplanet.^[6] Observations contributing to the initial detection spanned from July 2008 to December 2010 across the WASP-South and SuperWASP-North facilities.^[6] The discovery was announced in a preprint submitted on October 21, 2013, by R. G. West and collaborators, who analyzed data from the ongoing WASP survey focused on hot Jupiters—gas giants with orbital periods under 10 days receiving intense stellar irradiation.^[7] To confirm the planetary nature of the transiting object and determine its orbital period, follow-up radial velocity measurements were conducted using the SOPHIE spectrograph at the Haute-Provence Observatory from September to December 2011 and the CORALIE spectrograph on the Euler Telescope from February to December 2012.^[6] These observations revealed a Doppler signal consistent with a massive, short-period companion, ruling out false positives such as eclipsing binaries.^[6] The full results, including refined parameters from combined photometric and spectroscopic data, were published in Astronomy & Astrophysics in January 2016. This work highlighted WASP-76b as one of three newly identified inflated hot Jupiters, emphasizing the role of the WASP consortium in advancing the detection of such extreme exoplanets.^[6]

Nomenclature

WASP-76b is the provisional designation assigned to the exoplanet as the first and only confirmed planet orbiting its host star, WASP-76, under the naming convention of the Wide Angle Search for Planets (WASP) survey.^[7] This nomenclature follows the standard for transiting exoplanets detected by ground-based surveys, where the "b" suffix denotes the innermost known planet in the system.^[8] The planet is classified as a hot Jupiter, a category for gas giants with masses and radii comparable to Jupiter's but orbiting very close to their stars, leading to extreme temperatures from intense stellar irradiation.^[7] This classification was established upon its confirmation through photometric transits and radial velocity measurements.^[8] WASP-76b resides in the constellation Pisces, with its host star system located approximately 640 light-years from Earth.^[9] No alternative designations or International Astronomical Union (IAU)-approved proper names have been formally adopted for the planet as of 2025.

Host star system

Primary star properties

WASP-76 is an F7-type main-sequence star that serves as the primary host to the exoplanet WASP-76b. It has an effective temperature of 6250 ± 100 K, consistent with its spectral classification as a hot, yellow-white dwarf slightly hotter than the Sun.^[6] The star's surface gravity is log g = 4.4 ± 0.1 (cgs), reflecting its structure compared to solar values.^[6] The star possesses a mass of 1.46 ± 0.07 M⊙ and a radius of 1.73 ± 0.04 R⊙, making it more massive and larger than the Sun, with a corresponding luminosity approximately 4.1 L⊙.^[6] Its metallicity is slightly enhanced at [Fe/H] = +0.23 ± 0.10, indicating a higher abundance of heavy elements relative to hydrogen than in the Sun.^[6] Age estimates derived from gyrochronology, using the star's projected rotational velocity of v sin i = 3.3 ± 0.6 km/s and an assumed rotation period of about 17.6 days, place it at approximately 5.3^{+6.1}_{-2.9} Gyr.^[6] Observationally, WASP-76 is situated at a distance of 189 ± 3 pc from Earth, as determined from Gaia DR3 parallax measurements.^[10] It appears with an apparent visual magnitude of V = 9.5, rendering it accessible to ground-based telescopes for follow-up studies such as radial velocity monitoring and photometry.^[6]

Companion star

The companion star in the WASP-76 system, designated WASP-76 B, was identified through high-contrast imaging observations that resolved its presence relative to the primary star, with confirmation via Hubble Space Telescope (HST) spectroscopic imaging in 2020 revealing its impact on planetary spectra. The angular separation between WASP-76 A and B is 0.436 ± 0.003 arcseconds, corresponding to a projected physical separation of approximately 80 AU given the system's distance of about 189 pc from Gaia DR3. WASP-76 B is a late G- or early K-type dwarf with an effective temperature of 4824 ± 128 K, a mass of 0.79 ± 0.03 M⊙, and a radius of 0.83 R⊙. It is fainter than the primary by ΔK = 2.30 ± 0.05 magnitudes, contributing roughly 10–11% of the total system flux in the near-infrared bands relevant to HST Wide Field Camera 3 (WFC3) observations.^[11] This flux ratio implies a dilution factor of about 1.08–1.11 in transit depths, requiring wavelength-dependent corrections to accurately interpret the data.^[11] The presence of WASP-76 B complicates exoplanet characterization by blending its light with that of the primary, which initially distorted the transmission spectrum of WASP-76b in early HST data from 2020, artificially steepening the slope and influencing interpretations of atmospheric scattering or cloud properties.^[11] Post-correction analyses preserve key features like water absorption while eliminating the need for non-gray cloud models to explain the spectral shape.^[11] The companion orbits the primary on a wide binary trajectory, with common proper motion confirmed at greater than 5σ significance, ensuring no dynamical influence on the short-period orbit of WASP-76b at 0.033 AU. This configuration allows the planet's close-in dynamics to remain isolated from binary perturbations.

Orbital parameters

Orbital elements

WASP-76b orbits its host star at a semi-major axis of 0.03277 ± 0.00078 AU, placing it in an extremely close-in configuration typical of hot Jupiters. This distance results in intense stellar irradiation, contributing to the planet's ultra-hot nature. The orbital period is precisely measured as 1.80988132 ± 0.00012 days, equivalent to approximately 43.4 hours, enabling frequent transits observable from Earth. The orbit exhibits very low eccentricity, with a value of 0.00087 ± 0.00031, indicating a nearly circular path that minimizes variations in orbital speed and distance from the star. The orbital inclination relative to the sky plane is 87.88° ± 0.16°, a near-edge-on geometry essential for detecting the planet via the transit method. These parameters are governed by Kepler's third law, which relates the orbital period P to the semi-major axis a and the masses of the star M_\star and planet M_p through the proportionality P^2 \propto a^3 / (M_\star + M_p). Updated values for WASP-76b's orbital elements, refined through combined photometric and radial velocity analyses, are reported in Wang et al. (2025).

Transit characteristics

The transits of WASP-76b were initially detected through photometric monitoring by the Wide Angle Search for Planets (SuperWASP) survey in 2013, leading to its confirmation and publication in 2016. Follow-up high-precision photometry has since been obtained using space-based observatories, including the Hubble Space Telescope (HST) with the Space Telescope Imaging Spectrograph (STIS) and Wide Field Camera 3 (WFC3), the Spitzer Space Telescope with the Infrared Array Camera (IRAC), and the James Webb Space Telescope (JWST) for infrared light curves.^[12] These observations have enabled detailed characterization of the transit events, revealing a depth of approximately 1.18%, which corresponds to a planet-to-star radius ratio of R_p / R_\star \approx 0.109 and underscores the planet's inflated size relative to the host star.^[12] The full transit duration (T_{14}) is about 3.76 hours, occurring roughly every 1.81 days due to the planet's short orbital period.^[12] Ingress and egress phases each last on the order of 15-20 minutes, as inferred from the high-cadence light curves that resolve these contact points and facilitate precise modeling of the transit shape. Transit timing variations (TTVs) have been analyzed from multiple epochs spanning over a decade, revealing significant deviations consistent with apsidal precession or possible perturbing planets in the system (Wang et al. 2025).^[13] The host system's visual binary nature, with the fainter companion star WASP-76B separated by about 0.43 arcseconds, introduces third-light dilution that contaminates early transit measurements by contributing up to 10% of the total flux in optical bands. Post-2020 analyses, particularly from HST spectroscopy, have applied wavelength-dependent correction factors—such as multiplying observed depths by dilution ratios around 1.008 in the near-infrared—to recover accurate planet-to-star radius ratios, ensuring reliable photometric characterization.^[12]

Physical properties

Mass and radius

WASP-76b has a mass of 0.92 ± 0.03 Jupiter masses, determined through radial velocity measurements that detect the star's orbital wobble induced by the planet. These measurements were obtained using high-precision spectrographs such as SOPHIE and CORALIE, yielding a radial velocity semi-amplitude K = 0.098 \pm 0.002 km/s, which, combined with the orbital period and stellar mass, allows derivation of the planetary mass via Markov Chain Monte Carlo analysis. Uncertainties in the mass primarily stem from the stellar mass estimate of 1.46 ± 0.07 solar masses, as the planetary mass scales with the two-thirds power of the host star's mass.^[1] The planet's radius is measured at 1.83 ± 0.06 Jupiter radii (as of 2016 discovery), inferred from the transit depth observed in photometric data, which relates the planetary radius to the stellar radius via the formula for transit depth (R_p / R_*)^2. Transit observations were conducted with instruments including WASP, EulerCam, and TRAPPIST, providing the necessary light curve to model the planetary size after accounting for the host star's radius of 1.77 ± 0.16 solar radii. Like the mass, radius uncertainties are influenced by stellar parameter errors, particularly the stellar radius, which directly affects the scaling. Subsequent analyses, such as Fu et al. (2021), refine the radius to 1.845 ± 0.050 Jupiter radii using additional photometric data.^[1]^[14] From these dimensions, WASP-76b's mean density is calculated as approximately 0.18 ± 0.02 g/cm³, significantly lower than Jupiter's 1.33 g/cm³, reflecting an inflated gaseous envelope due to intense stellar irradiation. This low density, combined with the planet's larger size compared to Jupiter, highlights its classification as a bloated hot Jupiter, where heating expands the atmosphere without substantially altering the core mass.

Temperature and density

WASP-76b exhibits an equilibrium temperature of approximately 2230 K (as of 2025 analysis), computed via the formula T_{\rm eq} = T_{\star} \sqrt{\frac{R_{\star}}{2a}} (1 - A)^{1/4}, where T_{\star} is the stellar effective temperature, R_{\star} the stellar radius, a the semi-major axis, and A = 0 (zero Bond albedo) under the assumption of full longitudinal heat redistribution; earlier estimates from 2016 were ~2190 K.^[13]^[1] Phase-curve observations reveal a hotter dayside, with brightness temperatures reaching ~2470 K at 3.6 μm and ~2700 K at 4.5 μm, indicating inefficient heat transfer to the nightside and strong thermal dissociation of molecular species.^[15] The planet's low mean density of ~180 kg/m³, derived from its mass of 0.92 M_Jup and radius of 1.83 R_Jup, implies substantial atmospheric inflation and suggests deep convective heat circulation that deposits irradiation energy into the interior.^[16] This low density profile is consistent with a modest core mass of ~10–20 Earth masses in interior structure models, where the envelope dominates the total mass and radius.^[17] The primary inflation mechanism is irradiation-driven, with intense stellar flux heating the dayside and driving energy transport through vertical advection of potential temperature, as simulated in radiative general circulation models (GCMs).^[18]

Atmosphere

Chemical composition

The atmosphere of WASP-76b exhibits a complex chemical composition dominated by molecular and atomic species, primarily detected through transmission spectroscopy that reveals absorption features during planetary transits. Water vapor (H₂O) and titanium oxide (TiO) were first identified in the near-infrared transmission spectrum, indicating their presence in the upper atmosphere and contributing to thermal inversion layers.^[12] These detections stem from observations with the Hubble Space Telescope (HST) and Spitzer Space Telescope, spanning wavelengths from 0.8 to 5 μm, where TiO absorption is prominent between 0.4 and 1 μm and H₂O features appear around 1.4 μm.^[12] High-resolution ground-based spectroscopy has revealed a rich inventory of ionized and neutral metals, reflecting the planet's extreme temperatures that promote atomic dissociation. Using the ESPRESSO instrument on the Very Large Telescope (VLT), neutral iron (Fe I), sodium (Na I), calcium (Ca II), magnesium (Mg I), potassium (K I), manganese (Mn I), and lithium (Li I) were detected through strong absorption lines at optical wavelengths (e.g., Fe I at 4377 Å with depths up to 255 ppm).^[19] Complementary observations with Gemini North's MAROON-X spectrograph identified vanadium oxide (VO), along with chromium (Cr), vanadium (V), nickel (Ni), and other rock-forming elements, marking the first unambiguous detection of VO in an exoplanet atmosphere via high-resolution spectroscopy.^[20] These spectral features, observed across multiple transits from 2020 to 2024, highlight the planet's dayside chemistry, where high temperatures exceeding 2400 K enable metal vaporization.^[19] Abundance estimates indicate enhanced metallicity relative to solar values, with several elements showing supersolar enrichment that suggests efficient incorporation from the host star or planetesimal accretion. For instance, iron abundance aligns with the host star's [Fe/H] = 0.23 ± 0.10, but retrievals imply overall atmospheric metallicity consistent with or slightly above this level for refractory species.^[21] Barium (Ba⁺), the heaviest element detected to date in an exoplanet atmosphere, was observed in 2022 via VLT/ESPRESSO at high altitudes, with a detection significance of ~5σ, implying [Ba/H] potentially exceeding solar by factors linked to dynamical mixing.^[22] The atmosphere is shrouded in grey, hazy cloud layers formed from condensing metal vapors, which scatter light and mute spectral features at certain wavelengths. Atmospheric retrieval analyses from 2024, based on ESPRESSO data, reveal uniform longitudinal distributions of iron and magnesium across the planetary limbs, consistent with well-mixed condensates rather than localized depletions.^[23]

Dynamical and thermal phenomena

WASP-76b's atmosphere exhibits extreme dynamical phenomena driven by its tidally locked configuration and intense stellar irradiation, resulting in rapid day-to-nightside circulation. High-altitude winds transport material supersonically from the scorching dayside to the cooler nightside, with speeds reaching up to 5.5 km/s in the lower atmosphere and vertical winds approaching 22.7 km/s in the upper layers, facilitating efficient heat and chemical redistribution.^[24] These patterns lack strong evidence for latitude-dependent jets in early observations but indicate uniform day-to-night flow, potentially leading to high shear that could induce sideways molten flows of condensed materials.^[24] A prominent feature is the hypothesized "iron rain," where neutral iron vaporizes on the dayside at temperatures exceeding 2,000 K and condenses into droplets on the nightside around 1,800 K, transported by winds exceeding 10 km/s (over 36,000 km/h).^[3] This asymmetric iron absorption signature, blueshifted by -11 km/s, supports the scenario of evening vapor transport and morning condensation, though the exact mechanism remains debated.^[3] Alternative models suggest optically thick clouds of aluminum oxide, iron, or magnesium silicate could mimic the signal without requiring large-scale rain, highlighting unresolved tensions between observations and general circulation models.^[25] Extreme dayside heat promotes thermal dissociation, ionizing metals such as calcium while keeping iron primarily neutral, contributing to a complex upper atmosphere with strong vertical mixing.^[26] Detected ionized calcium signals indicate vigorous dynamics, potentially amplifying wind-driven transport of dissociated species.^[26] Optical effects include a potential "glory," a rainbow-like backscattering phenomenon observed as a flux increase in visible phase curves from the eastern hemisphere, requiring uniform spherical droplets or aerosols approximately 1 μm in size.^[4] This asymmetry aligns with wind patterns favoring cloud formation on one limb, though it challenges uniform atmospheric models.^[4] Recent 2025 phase-curve analyses using general circulation models reveal enhanced wind structures, including super-rotating equatorial jets up to ±10 km/s in drag-free scenarios, which sharpen dayside emission peaks and modulate chemical signals like iron across the orbit. These jets, suppressed by atmospheric drag, provide new constraints on circulation regimes, emphasizing the role of low-friction dynamics in ultra-hot Jupiter weather.

Hypothetical features

Possible exomoon

In 2019, researchers proposed the hypothesis of a hot, evaporating exomoon orbiting WASP-76b to explain observed features in the planet's transmission spectrum.^[27] This model draws an analogy to Jupiter's moon Io, where intense stellar irradiation could drive volcanic outgassing and atmospheric escape from the exomoon, forming a toroidal (doughnut-shaped) hydrogen envelope around the planet.^[27] The exomoon's material would be stripped by the planet's gravity and stellar winds, creating an extended, low-density exosphere detectable via absorption lines. The primary evidence stems from high-resolution spectroscopy revealing a broadened neutral sodium (Na I) absorption feature in WASP-76b's atmosphere, with a D2/D1 line ratio near 2 indicating optically thin gas consistent with a tenuous toroidal structure rather than a hydrostatic planetary atmosphere.^[27] Simulations suggest this sodium could originate from silicate grain desorption or direct outgassing in the exomoon's envelope, with mass loss rates on the order of 10³–10⁵ kg/s for atomic sodium alone.^[27] No direct photometric signatures, such as secondary eclipses or transit dips from the moon itself, have been identified, limiting detection to indirect spectral imprints. Challenges to this hypothesis include the low signal-to-noise ratio of the sodium lines and alternative interpretations attributing the broadened absorption to strong day-to-night atmospheric winds transporting metals across the planet's terminator. The intense irradiation on WASP-76b, with equilibrium temperatures exceeding 2000 K, would rapidly erode any exomoon, potentially destroying it within short timescales unless replenished by internal heating.^[27] As of 2025, the presence of an exomoon remains unconfirmed, with no dedicated follow-up observations resolving the ambiguity. Future high-precision spectroscopy using the James Webb Space Telescope (JWST) could probe the exosphere's dynamics and chemistry to test this model.^[27]

References

[1]
Three irradiated and bloated hot Jupiters: - WASP-76b, WASP-82b ...
We report on three new transiting hot Jupiter planets, discovered from the WASP surveys, which we combine with radial velocities from OHP/SOPHIE and Euler/ ...
[2]
ESA - First 'glory' on hellish distant world? - European Space Agency
Apr 5, 2024 · A hellish planet with lopsided limbs WASP-76b is an ultra-hot Jupiter-like planet. While it is 10% less massive than our striped cousin, it is ...
[3]
Nightside condensation of iron in an ultrahot giant exoplanet - Nature
Mar 11, 2020 · On WASP-76b and similarly hot planets, these clouds could be made out of iron droplets, because liquid iron is the most stable high-temperature ...
[4]
Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b | Astronomy & Astrophysics (A&A)
Summary of each segment:
[5]
Three irradiated and bloated hot Jupiters: - Astronomy & Astrophysics
The planets WASP-76b, WASP-82b, and. WASP-90b are all inflated, with radii of 1.7–1.8 RJup. All three orbit hot stars, of type F5–F7, with orbits of 1.8–3.9 d, ...
[6]
[1310.5607] Three irradiated and bloated hot Jupiters: WASP-76b ...
Oct 21, 2013 · We report three new transiting hot-Jupiter planets discovered from the WASP surveys combined with radial velocities from OHP/SOPHIE and Euler/CORALIE and ...
[7]
https://arxiv.org/abs/1310.5607
[8]
Astronomers Detect Rainbow-Like 'Glory' in Atmosphere of WASP-76b
Apr 5, 2024 · Image credit: ESA. WASP-76b is an ultra-hot Jupiter located 640 light-years away in the constellation of Pisces. First discovered in 2016, this ...
[9]
WASP-76 | NASA Exoplanet Archive
### Summary for WASP-76 b
[10]
ARES I: WASP-76 b, A Tale of Two HST Spectra - IOPscience
Accounting for a fainter stellar companion to WASP-76, we reanalyze this data and show that removing the effects of this background star changes the slope of ...
[11]
The Hubble PanCET Program: Transit and Eclipse Spectroscopy of ...
Aug 17, 2021 · We observed the ultra-hot Jupiter WASP-76b with seven transits and five eclipses using the Hubble Space Telescope and the Spitzer Space ...Missing: SuperWASP | Show results with:SuperWASP
[12]
Observations and Studies on the Transiting Systems HAT-P-36, XO ...
Jun 2, 2025 · We conducted photometric observations for transit events of three exoplanetary systems HAT-P-36, XO-2 and WASP-76 using the 1 m and 2.4 m telescopes.
[13]
Spitzer Phase-curve Observations and Circulation Models of the ...
Sep 22, 2021 · We find that WASP-76b has an ultrahot dayside and relatively cold nightside with brightness temperatures of 2471 ± 27 K/1518 ± 61 K at 3.6 μm and 2699 ± 32 K/ ...Abstract · Introduction · Spitzer Observations · Numerical Models of the...
[14]
Evidence of radius inflation in radiative GCM models of WASP-76b ...
Specifically, a recent study which explored the atmosphere of WASP-76b using a 3D non-grey GCM suggested that their models lacked radius inflation, and hence ...
[15]
Evidence of Radius Inflation in Radiative GCM Models of WASP-76b ...
Jun 21, 2023 · We thus conclude that the vertical advection of potential temperature alone is enough to explain the radius inflation of WASP-76b, and potentially other ...
[16]
ESPRESSO high-resolution transmission spectroscopy of WASP-76 b
4.1 Stellar atmospheric parameters. The stellar atmospheric parameters of WASP-76, namely effective temperature (Teff), surface gravity (logg), microturbulence ...
[17]
The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter ...
We observed two transits of WASP-76b (mass Mp = 0.92MJ , radius Rp = 1.83RJ , period P = 1.81 days, equilibrium temperature Teq = 2160 K) with Gemini-S ...
[18]
Together with new detections of Co and Sr+ on WASP-121b
Two of the best examples are WASP-76b and WASP-121b (West et al. 2016; Delrez et al. 2016). Both planets are inflated ultra-hot Jupiters on orbits with periods ...
[19]
High-resolution atmospheric retrievals of WASP-76b transmission spectroscopy with ESPRESSO: Monitoring limb asymmetries across multiple transits
### Summary of Cloud Layers, Grey Hazy Clouds, Metal Condensates, and Uniform Fe/Mg Distribution in WASP-76b Atmosphere (2024 Retrievals)
[20]
diving into the winds of the ultra-hot Jupiter WASP-76 b with HARPS ...
... WASP-76 b (Seidel et al. 2019), a close companion to the host star was detected by Bohn et al. (2020) with a separation of 0.436 ± 0.003 arcsec and a K-band ...
[21]
Confronting the Hypothesis of Iron Rain on WASP-76b with Post ...
Feb 15, 2022 · In this work, we forward model the atmosphere of WASP-76b with double-gray general circulation models (GCMs) and ray-striking radiative transfer ...
[22]
Detection of Ionized Calcium in the Atmosphere of the Ultra-hot ...
Orbital and Physical Parameters of the WASP-76 System Used in This Analysis ... 1.14 ${}_{-0.08}^{+0.09}$, ${185.6}_{-27.7}^{+12.2}$. (0.348 ± 0.046), (−3.015 ...
[23]
https://arxiv.org/abs/2404.10463