Millimetre image of the disk from the REASONS survey[9]
In 2003,Michel Mayor's team announced the discovery of a new planet,HD 10647 b, in Paris at the XIX IAP ColloquiumExtrasolar Planets: Today & Tomorrow.[10] TheAnglo-Australian Planet Search team initially did not detect the planet in 2004,[11] though a solution was made by 2006.[12] TheCORALIE data was finally published in 2013.[4]
The inclination of the disk is relatively high,[15] and the disk is asymmetrical, being more extended in the northeast direction than the southwest.[14] It extends from 34astronomical units (AU) at the inner edge to 134 AU at the outer edge. The inner edge is sharp, suggesting the existence of a planet that carved out the edge. HD 10647 b, with a semimajor axis of about 2 AU, is too far to be responsible. However, other potential planets may be responsible for this feature.[14]
If HD 10647 b shares the same orbital inclination as the disk (76.7°±1.0°), its mass should be about 1.07Jupiter masses, close to its minimum mass of 0.90 Jupiter masses.[16]
There is some evidence for an additional, warmasteroid belt-like component further in, at 3 to 10 AU away from the star.[14]
^Matrà, L.; Marino, S.; Wilner, D. J.; Kennedy, G. M.; Booth, M.; Krivov, A. V.; Williams, J. P.; Hughes, A. M.; Burgo, C. del (2025-01-15). "REsolved ALMA and SMA Observations of Nearby Stars (REASONS): A population of 74 resolved planetesimal belts at millimetre wavelengths".Astronomy and Astrophysics.693.arXiv:2501.09058.Bibcode:2025A&A...693A.151M.doi:10.1051/0004-6361/202451397.
^Jones, H. R. A.; et al. (2004). "HD10647 and the Distribution of Exoplanet Properties with Semi-major Axis".Extrasolar Planets: Today and Tomorrow.321: 298.Bibcode:2004ASPC..321..298J.
^Stencel, Robert E.; Backman, Dana E. (1991). "A Survey for Infrared Excesses among High Galactic Latitude SAO Stars".The Astrophysical Journal Supplement Series.75: 905.Bibcode:1991ApJS...75..905S.doi:10.1086/191553.
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