HD 95086 b

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HD 95086 b / Levantes
VLT image of the star HD 95086 and its planetary companion, seen here as a blue smudge.
Discovery[1]
Discovered byRameau et al.
Discovery siteVery Large Telescope
Discovery date2013
Direct imaging
Designations
Levantes[2]
Orbital characteristics
51-73 AU[3]
Eccentricity≤ 0.18[3]
Inclination144+18
−4°[3]
2004+105
−45 d[3]
StarHD 95086
Physical characteristics
Mass5.0 ± 2.0 MJ
3.85 ± 0.5 m/s2 (12.6 ± 1.6 ft/s2)
Spectral type
L7–L9[4]

HD 95086 b, formally named Levantes,

μm) through direct imaging, using the NACO instrument on the VLT.[1] 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.[7]

The host star was considered a highly probable member of the Lower Centaurus Crux star forming region,

parsecs away in the constellation of Carina.[10]

Nomenclature

In August 2022, this planet and its host star were included among 20 systems to be named by the third NameExoWorlds project.[11] The approved names, proposed by a team from Greece, were announced in June 2023. HD 95086 b is named Levantes, from a modern Greek word referring to easterly Mediterranean winds, and its host star is named Aiolos after a Greek mythological figure.[2]

Discovery

The planet was initially detected in data taken in 2012 at a separation from the parent star of 623.9 ± 7.4

brown dwarfs
.

Spatially resolved images of the system from the Herschel Space Observatory[7] show evidence for a possible 2 belt system with a large clearing between the belts, similar to HR 8799. HD 95086 b is probably responsible for carving the sharp inner edge of the outer disk, but additional planets in this system occupying the rest of the gap may be a strong possibility.[5]

Physical properties

HD 95086 b is a massive planet that exists at a large orbital radius, therefore it is a viable candidate for a planet that formed close to its host star and was later scattered outwards via gravitational interactions with other massive particles in orbit around the star. In a debris disk, these particles are of the form of other orbiting planets or

planetesimals. This scattering mechanism has been investigated for particles of the form of over-dense fluid elements like those found in a protoplanetary disk containing a planet.[13]
It has been proposed that scattering events could explain observed massive planets at large orbital radii.

The atmosphere of HD 95086 b contains large amounts of dust,[14] probably small, sub-micrometer forsterite grains.[4] The planet is very red in color, possibly due to the presence of the circumplanetary disk.[3]

References

  1. ^
    S2CID 56062429
    .
  2. ^ a b c "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
  3. ^
    S2CID 248874069
    .
  4. ^
    arXiv:1801.05850
  5. ^
    S2CID 28985252.{{cite journal}}: CS1 maint: multiple names: authors list (link
    )
  6. ^ Eric E. Mamajek. "Post-T Tauri Stars in the Nearest OB Association". Retrieved 2002-05-20.
  7. ^
    S2CID 55592599
    .
  8. ^ P. T. De Zeeuw (1998-09-14). "A Hipparcos census of the nearby OB associations".
  9. doi:10.1093/mnras/staa3631
  10. ^ F. van Leeuwen. "Validation of the new Hipparcos reduction". Archived from the original on 2013-11-01. Retrieved 2007-08-08.
  11. ^ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  12. S2CID 59583242
    .
  13. doi:10.1093/mnras/stt1047
    .
  14. S2CID 55041736
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