HIP 65426 b

Last updated
HIP 65426 b / Najsakopajk
The unusual exoplanet HIP 65426b -- SPHERE's first.jpg
HIP 65426 b is on the lower left of the image, with the circle representing what Neptune's orbit would look like around the star HIP 65426, represented by a small cross.
Discovery [1]
Discovered by SPHERE consortium [2]
Discovery date6 July 2017
Direct imaging
Designations
Najsakopajk [3]
Orbital characteristics
87+108
−31  AU [4]
Inclination 100° +15°
−6° [4]
Physical characteristics
1.44±0.03  RJ [4]
Mass 7.1±1.2  MJ [4]
3.93+0.07
−0.09 dex [4]
Temperature 1,283+25
−31  K [4]

    HIP 65426 b, formally named Najsakopajk, [3] is a super-Jupiter exoplanet orbiting the star HIP 65426. It was discovered on 6 July 2017 by the SPHERE consortium using the Spectro-Polarimetric High-Contrast Exoplanet Research (SPHERE) instrument belonging to the European Southern Observatory (ESO), [5] [6] being the first planet discovered by the SPHERE instrument. [7] It is 385 light-years from Earth in the Centaurus constellation. [8]

    Contents

    Nomenclature

    HIP 65426 b is a designation inherited from the host star's name, HIP 65426, following the exoplanet naming convention, where exoplanets receive lowercase letters. The designation HIP 65426 has its origin on the Hipparcos catalogue. [9]

    In August 2022, this planet and its host star were included among 20 systems to be named by the third NameExoWorlds project. [10] The approved names, proposed by a team from Mexico, were announced in June 2023. HIP 65426 b is named Najsakopajk and its host star is named Matza, after Zoque words for "Mother Earth" and "star". [3]

    Overview

    The exoplanet HIP 65426 b orbits its host star HIP 65426, an A-type main-sequence star with apparent magnitude 7.01, with a mass of 1.96±0.04  M☉ , a radius of 1.77±0.05  M☉ and an effective temperature of 8,840  K (8,570 °C). [11] This planetary system is located in the constellation Centaurus. The planet is around 14 million years old, much younger than the Solar System which is 4.5 billion years old, but is not associated with a debris disk, despite its young age, [6] [8] causing it to not fit current models for planetary formation. [12] It is around 92 AU from its parent star, with a possible dusty atmosphere. [13] It was discovered as part of the SHINE program, which aimed to find planetary systems around 600 new stars. [1]

    In September 2022, HIP 65426 b became the first exoplanet directly observed by the James Webb Space Telescope. [14]

    Planetary atmosphere

    The spectrum taken in 2020 has indicated that HIP 65426 b is carbon-poor and oxygen-rich compared to Solar System gas giants. [15]

    Spectral analysis of data from the James Webb Space Telescope revealed strong evidence of silicate clouds containing enstatite with no evidence of a dusty atmosphere. [16]

    James Webb Space Telescope observations

    In August 2022, a pre-print of the James Webb Space Telescope (JWST) observations was published. The JWST direct imaging observations between 2-16 μm of HIP 65426 b tightly constrained its bolometric luminosity to , which provides a robust mass constraint of 7.1±1.2  MJ . Evolutionary models suggest a radius 45% larger than that of Jupiter and an effective temperature of 1,283  K (1,010 °C). Atmospheric models suggest lower radii down to 0.9 RJ and higher temperatures, but these results are unreliable. The team also constrained the semi-major axis and the inclination of the planet, but the new JWST astrometry of the planet did not significantly improve the orbit of the planet, especially the eccentricity remains unconstrained. [4]

    HIP 65426 b is the first exoplanet to be imaged by JWST and the first to be detected in wavelengths beyond 5 μm. The observations [17] demonstrate that the James Webb Space Telescope will exceed its nominal predicted performance by a factor of 10 and that it will be able to image 0.3 MJ planets at 100 au for main-sequence stars, Neptune and Uranus-mass objects at 100-200 au for M-dwarfs and Saturn-mass objects at 10 au for M-dwarfs. For α Cen A JWST might be able to push the limit to a 5 R🜨 planet at 0.5 to 2.5 au. [4]

    HIP 65426-starmap.png
    HIP 65426 star map
    NASA's Webb Takes Its First-Ever Direct Image of Distant World.png
    HIP 65426 b viewed by the James Webb Space Telescope (August 2022)

    See also

    Related Research Articles

    <span class="mw-page-title-main">2M1207b</span> Planetary-mass object orbiting the brown dwarf 2M1207

    2M1207b is a planetary-mass object orbiting the brown dwarf 2M1207, in the constellation Centaurus, approximately 170 light-years from Earth. It is one of the first candidate exoplanets to be directly observed. It was discovered in April 2004 by the Very Large Telescope (VLT) at the Paranal Observatory in Chile by a team from the European Southern Observatory led by Gaël Chauvin. It is believed to be from 5 to 6 times the mass of Jupiter and may orbit 2M1207 at a distance roughly as far from the brown dwarf as Pluto is from the Sun.

    <span class="mw-page-title-main">Epsilon Eridani b</span> Gas giant orbiting Epsilon Eridani

    Epsilon Eridani b, also known as AEgir [sic], is an exoplanet approximately 10.5 light-years away orbiting the star Epsilon Eridani, in the constellation of Eridanus. The planet was discovered in 2000, and as of 2024 remains the only confirmed planet in its planetary system. It orbits at around 3.5 AU with a period of around 7.6 years, and has a mass around 0.6 times that of Jupiter. As of 2023, both the Extrasolar Planets Encyclopaedia and the NASA Exoplanet Archive list the planet as 'confirmed'.

    <span class="mw-page-title-main">Fomalhaut b</span> Extrasolar object orbiting Fomalhaut

    Fomalhaut b, formally named Dagon, is a former candidate planet observed near the A-type main-sequence star Fomalhaut, approximately 25 light-years away in the constellation of Piscis Austrinus. The object's discovery was initially announced in 2008 and confirmed in 2012 via images taken with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. Under the working hypothesis that the object was a planet, it was reported in January 2013 that it had a highly elliptical orbit with a period of 1,700 Earth years. The object was one of those selected by the International Astronomical Union as part of NameExoWorlds, their public process for giving proper names to exoplanets. The process involved public nomination and voting for the new name. In December 2015, the IAU announced the winning name was Dagon.

    <span class="mw-page-title-main">GJ 1214 b</span> Super-Earth orbiting GJ 1214

    GJ 1214 b is an exoplanet that orbits the star GJ 1214, and was discovered in December 2009. Its parent star is 48 light-years from the Sun, in the constellation Ophiuchus. At the time of its discovery, GJ 1214 b was the most likely known candidate for being an ocean planet. For that reason, scientists at that time often called the planet a "waterworld". However, a recent study of the planet's internal structure informed by observations taken with the James Webb Space Telescope suggests that a "waterworld" composition is implausible and the planet is more likely to host a thick gaseous envelope consisting of hydrogen, helium, water and other volatile chemicals such as methane or carbon dioxide.

    <span class="mw-page-title-main">WASP-43b</span> Extrasolar planet in the constellation Sextans

    WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

    <span class="mw-page-title-main">HD 95086 b</span> Exoplanet orbiting the young HD 95086

    HD 95086 b, formally named Levantes, is a confirmed, directly imaged exoplanet orbiting the young, 17 Myr A-class pre-main-sequence star HD 95086. It is roughly 5 times as massive as Jupiter and orbits about 70 AU away from the parent star. It was detected at thermal infrared wavelengths (3.8 μm) through direct imaging, using the NACO instrument on the VLT. A debris disk has been detected in this system at submillimeter wavelengths and has been resolved in the far-infrared from data obtained with the Herschel Space Observatory.

    Gliese 504 b is a jovian planet or a brown dwarf orbiting the solar analog 59 Virginis, discovered by direct imaging using HiCIAO instrument and AO188 adaptive optics system on the Subaru Telescope of Mauna Kea Observatory, Hawaii by Kuzuhara et al.

    <span class="mw-page-title-main">HD 106906 b</span> Candidate exoplanet in the constellation Crux

    HD 106906 b is a directly imaged planetary-mass companion and exoplanet orbiting the star HD 106906, in the constellation Crux at about 336 ± 13 light-years (103 ± 4 pc) from Earth. It is estimated to be about eleven times the mass of Jupiter and is located about 738 AU away from its host star. HD 106906 b is an oddity; while its mass estimate is nominally consistent with identifying it as an exoplanet, it appears at a much wider separation from its parent star than thought possible for in-situ formation from a protoplanetary disk.

    <span class="mw-page-title-main">Spectro-Polarimetric High-Contrast Exoplanet Research</span>

    Spectro-Polarimetric High-contrast Exoplanet REsearch (VLT-SPHERE) is an adaptive optics system and coronagraphic facility at the Very Large Telescope (VLT). It provides direct imaging as well as spectroscopic and polarimetric characterization of exoplanet systems. The instrument operates in the visible and near infrared, achieving exquisite image quality and contrast over a small field of view around bright targets.

    <span class="mw-page-title-main">51 Eridani b</span> Extrasolar planet

    51 Eridani b is a "Jupiter-like" planet that orbits the young F0 V star 51 Eridani, in the constellation Eridanus. It is 96 light years away from the solar system, and it is approximately 20 million years old.

    WASP-121, also known as CD-38 3220 and formally named Dilmun, is a magnitude 10.4 star located approximately 858 light-years away in the constellation Puppis. WASP-121 has a mass and radius similar to the Sun's. It hosts one known exoplanet.

    <span class="mw-page-title-main">WASP-39b</span> Exoplanet in constellation of Virgo

    WASP-39b, officially named Bocaprins, is a "hot Jupiter" extrasolar planet discovered in February 2011 by the WASP project, notable for containing a substantial amount of water in its atmosphere. In addition WASP-39b was the first exoplanet found to contain carbon dioxide in its atmosphere, and likewise for sulfur dioxide.

    <span class="mw-page-title-main">PDS 70</span> T Tauri-type star in the constellation Centaurus

    PDS 70 is a very young T Tauri star in the constellation Centaurus. Located 370 light-years from Earth, it has a mass of 0.76 M☉ and is approximately 5.4 million years old. The star has a protoplanetary disk containing two nascent exoplanets, named PDS 70b and PDS 70c, which have been directly imaged by the European Southern Observatory's Very Large Telescope. PDS 70b was the first confirmed protoplanet to be directly imaged.

    <span class="mw-page-title-main">HD 36112</span> Star in the constellation Taurus

    HD 36112, also known as MWC 758, is a young Herbig Ae star located in the constellation Taurus, surrounded by irregular rings of cosmic dust. The system is about 3.5 million years old. The disk has a cavity at 50 astronomical units and two spiral arms at 30-75 au that are seen in near-infrared scattered light, but only one spiral arm is seen in ALMA images.

    <span class="mw-page-title-main">Epsilon Indi Ab</span> Gas giant orbiting Epsilon Indi A

    Epsilon Indi Ab is a gas giant exoplanet orbiting the star Epsilon Indi A, about 11.9 light-years away in the constellation of Indus. The planet was confirmed to exist in 2018. It orbits at around 30 AU with a period of around 180 years and a relatively high eccentricity of 0.4, and has a mass around seven times that of Jupiter. It was directly imaged using the James Webb Space Telescope in 2023 and the image was released in 2024.

    <span class="mw-page-title-main">HD 95086</span> Star in the constellation Carina

    HD 95086, formally named Aiolos, is a pre-main-sequence star about 282 light-years away. Its surface temperature is 7,750±250 K. HD 95086 is somewhat metal-deficient in comparison to the Sun, with a metallicity Fe/H index of −0.25±0.5 (~55%), and is much younger at an age of 13.3 million years. It was originally thought to be part of the Lower Centaurus-Crux association, until it was found using Gaia data that the star may be instead part of the Carina association.

    <span class="mw-page-title-main">Gliese 486</span> Star in constellation of Virgo

    Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years away in the constellation Virgo. It hosts one known exoplanet.

    L 98-59 is a bright M dwarf star, located in the constellation of Volans, at a distance of 10.608 parsecs, as measured by the Gaia spacecraft.

    <span class="mw-page-title-main">WASP-96b</span> Gas giant exoplanet targeted for spectroscopy

    WASP-96b is a gas giant exoplanet. Its mass is 0.48 times that of Jupiter. It is 0.0453 AU from the class G star WASP-96, which it orbits every 3.4 days. It is about 1,140 light-years away from Earth, in the constellation Phoenix. It was discovered in 2013 by the Wide Angle Search for Planets (WASP).

    L 168-9 is a red dwarf star located 82.1 light-years away from the Solar System in the constellation of Tucana. The star has about 61% the mass and 60% the radius of the Sun. It has a temperature of 3,842 K and a rotation period of 29 days. L 168-9 is orbited by one known exoplanet.

    References

    1. 1 2 Chauvin, G.; Desidera, S.; Lagrange, A. -M.; Vigan, A.; Gratton, R.; Langlois, M.; Bonnefoy, M.; Beuzit, J. -L.; Feldt, M.; Mouillet, D.; Meyer, M.; Cheetham, A.; Biller, B.; Boccaletti, A.; d'Orazi, V.; Galicher, R.; Hagelberg, J.; Maire, A. -L.; Mesa, D.; Olofsson, J.; Samland, M.; Schmidt, T. O. B.; Sissa, E.; Bonavita, M.; Charnay, B.; Cudel, M.; Daemgen, S.; Delorme, P.; Janin-Potiron, P.; et al. (2017). "Discovery of a warm, dusty giant planet around HIP 65426". Astronomy and Astrophysics. 605: L9. arXiv: 1707.01413 . Bibcode:2017A&A...605L...9C. doi:10.1051/0004-6361/201731152. S2CID   102344893.
    2. ↑ "Odd planetary system around fast-spinning star doesn't quite fit existing models of planet formation". www.sphere.osug.fr. Retrieved 2017-07-06.
    3. 1 2 3 "2022 Approved Names". nameexoworlds.iau.org. IAU . Retrieved 7 June 2023.
    4. 1 2 3 4 5 6 7 8 Carter, Aarynn L.; Hinkley, Sasha; Kammerer, Jens; Skemer, Andrew; Biller, Beth A.; Leisenring, Jarron M.; Millar-Blanchaer, Maxwell A.; Petrus, Simon; Stone, Jordan M.; Ward-Duong, Kimberly; Wang, Jason J.; Girard, Julien H.; Hines, Dean C.; Perrin, Marshall D.; Pueyo, Laurent (2023-07-06). "The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2-16 μm". The Astrophysical Journal Letters. 951 (1): L20. arXiv: 2208.14990 . Bibcode:2023ApJ...951L..20C. doi: 10.3847/2041-8213/acd93e .
    5. ↑ "Scientists have found a planet that means everything they thought about planets isn't true". The Independent. 2017-07-08. Retrieved 2019-08-02.
    6. 1 2 "Astronomers Directly Image Super-Jupiter around HIP 65426 | Astronomy | Sci-News.com". Breaking Science News | Sci-News.com. Retrieved 2019-08-02.
    7. ↑ "ESO's SPHERE Unveils its First Exoplanet". www.eso.org. Retrieved 2017-07-07.
    8. 1 2 "Holiday Special: Eight nights of Exoplanet Light". Exoplanet Exploration: Planets Beyond our Solar System. NASA. Retrieved 2019-08-03.
    9. ↑ "Details on Acronym: HIP". SIMBAD . Retrieved 2025-01-08.
    10. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
    11. ↑ "The Extrasolar Planet Encyclopaedia — HIP 65426 b". Extrasolar Planets Encyclopaedia . Paris Observatory.
    12. ↑ "Odd planetary system around fast-spinning star doesn't quite fit existing models of planet formation". phys.org. Retrieved 2019-08-03.
    13. ↑ Johnson-Groh, Mara; July 12, 2017 (12 July 2017). "New exoplanet challenges formation models". Astronomy.com. Retrieved 2019-08-03.{{cite web}}: CS1 maint: numeric names: authors list (link)
    14. ↑ Fisher, Alise (2022-09-01). "NASA's Webb Takes Its First-Ever Direct Image of Distant World". NASA Blogs. NASA . Retrieved 2022-09-01.
    15. ↑ Petrus, S.; Bonnefoy, M.; Chauvin, G.; Charnay, B.; Marleau, G.-D.; Gratton, R.; Lagrange, A.-M.; Rameau, J.; Mordasini, C.; Nowak, M.; Delorme, P.; Boccaletti, A.; Carlotti, A.; Houllé, M.; Vigan, A.; Allard, F.; Desidera, S.; d'Orazi, V.; Hoeijmakers, H. J.; Wyttenbach, A.; Lavie, B. (2021), "Medium-resolution spectrum of the exoplanet HIP 65426 B", Astronomy & Astrophysics, 648: A59, arXiv: 2012.02798 , Bibcode:2021A&A...648A..59P, doi:10.1051/0004-6361/202038914, S2CID   227347064
    16. ↑ Wang 王, Ji 吉 (2023-11-01). "Spectral Retrieval with JWST Photometric data: a Case Study for HIP 65426 b". The Astronomical Journal. 166 (5): 203. arXiv: 2310.00089 . Bibcode:2023AJ....166..203W. doi: 10.3847/1538-3881/acfca0 . ISSN   0004-6256.
    17. ↑ "James Webb Discovery - First Direct Image of Exoplanet - HIP 65426 b". www.jameswebbdiscovery.com. Retrieved 2024-02-20.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.