HAT-P-32b is a planet orbiting theG-type orF-type starHAT-P-32, which is approximately 950 light years^[5] away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searchingHATNet Project in 2004, although difficulties in measuring itsradial velocity prevented astronomers from verifying the planet until after three years of observation. TheBlendanal program helped to rule out most of the alternatives that could explain what HAT-P-32b was, leading astronomers to determine that HAT-P-32b was most likely a planet. The discovery of HAT-P-32b and ofHAT-P-33b was submitted to a journal on 6 June 2011.

The planet is considered ahot Jupiter, and although it is slightly less massive than Jupiter, it is bloated to nearly twice Jupiter's size. At the time of its discovery, HAT-P-32b hadone of the largest radii known amongst extrasolar planets. This phenomenon, which has also been observed in planets likeWASP-17b andHAT-P-33b, has shown that something more than temperature is influencing why these planets become so large.^[1]

It had been suggested that a planet was orbiting HAT-P-32 as early as 2004; these observations were collected by the six-telescopeHATNet Project, an organization in search oftransiting planets, or planets that cross in front of their host stars as seen from Earth. However, attempts to confirm the planetary candidate were extremely difficult because of a high level ofjitter (a random, shaky deviation in the measurements of HAT-P-32'sradial velocity) present in the star's observations. High-level jitter prevented the most common technique, that of bisector analysis, from revealing the star's radial velocity with enough certainty to confirm the planet's existence.^[1]

Thespectrum of HAT-P-32 was collected using thedigital speedometer on Arizona'sFred Lawrence Whipple Observatory (FLWO). Analysis of the data found that HAT-P-32 was a single, moderately rotatingdwarf star. Some of its parameters were also derived, including itseffective temperature andsurface gravity.^[1]

Between August 2007 and December 2010, twenty-eight spectra were collected using theHigh Resolution Echelle Spectrometer (HIRES) at theW.M. Keck Observatory in Hawaii. Twenty-five of these spectra were used to deduce HAT-P-32's radial velocity. To compensate for jitter, a greater number of spectra than usual for planetary candidates was collected. From this, it was concluded that stellar activity (and not the presence of yet-undiscovered planets) was the cause of the jitter.^[1]

Because astronomers concluded that the use of radial velocity could not, alone, establish the existence of planet HAT-P-32b, theKeplerCam CCD instrument on FLWO's 1.2m telescope was used to takephotometric observations of HAT-P-32. The data collected using the KeplerCam CCD helped astronomers construct HAT-P-32'slight curve. The light curve displayed a slight dimming at a point where HAT-P-32b was believed to transit its star.^[1]

The astronomers utilizedBlendanal, a program used to eliminate the possibilities offalse positives. This process serves a similar purpose to theBlender technique, which was used to verify some planets discovered by theKepler spacecraft. In doing so, HAT-P-32's planet-like signature was found to not be caused by either ahierarchical triple star system or by a mixture of light between a bright single star and that of abinary star in the background. Although the possibility that HAT-P-32 is actually a binary star with a dim secondary companion nearly indistinguishable from the primary companion could not be ruled out, HAT-P-32b was confirmed as a planet based on the Blendanal analysis.^[1]

Because of the high jitter of the star, the best way to collect more data on HAT-P-32b would be to observe anoccultation of HAT-P-32b behind its star using theSpitzer Space Telescope.^[1]

HAT-P-32b's discovery was reported with that of HAT-P-33b in theAstrophysical Journal.^[1]

HAT-P-32, or GSC 3281–00800, is a double star; the primary is aG-type orF-typedwarf star,^[1] and the secondary is aM-typedwarf star.^[6] The system is located 292 parsecs (950 ly) away from Earth.^[5] With 1.176solar masses and 1.387solar radii, HAT-P-32A is both larger and more massive than the Sun. HAT-P-32A's effective temperature is 6,001K, making it slightly hotter than the Sun, although it is younger, at an estimated age of 3.8 billion years, thus beginningnuclear fusion in its core not long after theArchean eon started on Earth4.031±0.003 billion years ago.^[2] HAT-P-32A is metal-poor; its measuredmetallicity is [Fe/H] = -0.16, which means that it has 69% the iron content of the Sun.^[2] The star's surface gravity is determined to be 4.22, while itsluminosity suggests that it emits 2.43 times the amount of energy that the Sun emits.^[1] These parameters are adopted given the condition that the planet HAT-P-32b has an irregular (eccentric) orbit.^[1]

HAT-P-32 has anapparent magnitude of 11.197, which makes it invisible to the naked eye.^[7] A search for a binary companion star usingadaptive optics at theMMT Observatory discovered a companion at a distance of 2.9arcseconds that is 3.4 magnitudes dimmer than the primary star.^[8]

A very high level of jitter has been detected in the star's spectrum. There is a possibility that the jitter could be induced by the dimmer secondary companion. HAT-P-32's dimmer constituent probably has a mass that is under half of the Sun's mass,^[1] while it has a temperature of3565±82K.^[6]

Other planets withorbital periods that are smaller than that of HAT-P-32b's orbit may be present in this system. However, when the discovery of the planet was published, not enough radial velocity measurements had been collected to determine if this was the case.^[1]

HAT-P-32b is aHot Jupiter that has 0.941Jupiter masses and 2.037Jupiter radii. In other words, HAT-P-32b is slightly less massive than Jupiter is, although it is nearly twice Jupiter's size.^[2] The planet'saverage distance from its host star is 0.0344 AU, or approximately 3% of the mean distance between the Earth and the Sun. It completes an orbit every 2.150009 days (51.6 hours).^[2] HAT-P-32b has anequilibrium temperature of 1888 K,^[1] which is fifteen times hotter than Jupiter's equilibrium temperature.^[9] Nonetheless, limb temperature measured in 2020 was much cooler at 1248±92K.^[4]

Many of the described characteristics are derived on the assumption that HAT-P-32b has an orbit that is elliptical (eccentric). The best fit for HAT-P-32b's orbital eccentricity is 0.163, denoting a slightly elliptical orbit, although the jitter effect observed in its host star has made the planet's eccentricity difficult to accurately find. The discoverers have also derived the planet's characteristics assuming that the planet has a circular orbit, although they have given preference to the elliptical model.^[1]

Because HAT-P-32b'sorbital inclination with respect to Earth is 88.7º, the planet is seen almost edge-on with respect to Earth.^[2] It has been found to transit its host star.^[1]

A study in 2012, utilizing theRossiter–McLaughlin effect, has determined the planet is orbiting at nearly polar orbit relative to the rotation of the star, misalignment equal to 85±1.5°.^[10]

HAT-P-32b had one of the highest radii known amongst planets at the time of its discovery. Like planetsHAT-P-33b andWASP-17b, which are similarly inflated, the mechanism behind this is unknown; it is not solely related to temperature, which is known to have an effect. This is especially clear when compared toWASP-18b, a planet that is hotter than the aforementioned HAT and WASP planets, but despite its temperature its radius is far lower than that of its counterparts.^[1]

The planetary spectrum shows evidence ofRoche lobe overflow^[11] and rapid mass loss 13±7 million tons per second.^[12]

It was also found that the planet's radius, observed with planetary transits, varies with wavelength. Different radii for each wavelength could arise from an atmosphere where a Rayleigh scattering haze is combined with a grey cloud deck.^[13] The thick (clouds up to pressure level of 0.4-33 kPa) cloud deck and haze above it was indeed confirmed in 2020, along with the detection of water in the atmosphere of HAT-P-32b.^[4]

• Andromeda (constellation)
• Exoplanets discovered in 2011
• Transiting exoplanets
• Hot Jupiters
• Giant planets
• Exoplanets discovered by HATNet

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