The Blendanal 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.
However, attempts to confirm the planetary candidate were extremely difficult because of a high level of jitter (a random, shaky deviation in the measurements of HAT-P-32's radial 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] The spectrum of HAT-P-32 was collected using the digital speedometer on Arizona's Fred Lawrence Whipple Observatory (FLWO).
[1] Between August 2007 and December 2010, twenty-eight spectra were collected using the High Resolution Echelle Spectrometer (HIRES) at the W.M.
[1] Because astronomers concluded that the use of radial velocity could not, alone, establish the existence of planet HAT-P-32b, the KeplerCam CCD instrument on FLWO's 1.2m telescope was used to take photometric observations of HAT-P-32.
This process serves a similar purpose to the Blender technique, which was used to verify some planets discovered by the Kepler spacecraft.
HAT-P-32A's effective temperature is 6,001 K, making it slightly hotter than the Sun, although it is younger, at an estimated age of 3.8 billion years, thus beginning nuclear fusion in its core not long after the Archean eon started on Earth 4.031±0.003 billion years ago.
[9] Nonetheless, limb temperature measured in 2020 was much cooler at 1248±92 K.[4] Many of the described characteristics are derived on the assumption that HAT-P-32b has an orbit that is elliptical (eccentric).
[1] The planetary spectrum shows evidence of Roche lobe overflow[11] and rapid mass loss 13±7 million tons per second.
Different radii for each wavelength could arise from an atmosphere where a Rayleigh scattering haze is combined with a grey cloud deck.