Q302964
Sign in to saveAlso known as HAT-P-32 b
HAT-P-32b is a planet orbiting the G-type or F-type star HAT-P-32, which is approximately 950 light years away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searching HATNet Project in 2004, although difficulties in measuring its radial velocity prevented astronomers from verifying the planet until after three years of observation. 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. The discovery of HAT-P-32b and of HAT-P-33b was submitt
Wikidata facts
- Radius
- 1.98
- Mass
- 0.75
- Orbital period
- 2.15000825
Show 13 more facts
- catalog code
- TIC 292152376b
- time of discovery or invention
- 2011-11-00
- right ascension
- 31.04282310740376
- M sin i
- 0.68
- orbital inclination
- 89
- argument of periapsis
- 50
- angular distance
- 0.000108
- orbital eccentricity
- 0.159
- right ascension component of proper motion
- -9.825
- declination component of proper motion
- 3.477
- semi-major axis of an orbit
- 0.03427
- declination
- 46.68783621743084
- parallax
- 3.4305
Sources (1)
via Wikidata · CC0
~8 min read
Article
4 sectionsContents
- Discovery
- Host star
- Characteristics
- References
HAT-P-32b is a planet orbiting the G-type or F-type star HAT-P-32, which is approximately 950 light years away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searching HATNet Project in 2004, although difficulties in measuring its radial velocity prevented astronomers from verifying the planet until after three years of observation. 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. The discovery of HAT-P-32b and of HAT-P-33b was submitted to a journal on 6 June 2011.
The planet is considered a hot 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 had one of the largest radii known amongst extrasolar planets. This phenomenon, which has also been observed in planets like WASP-17b and HAT-P-33b, has shown that something more than temperature is influencing why these planets become so large.