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An advanced multipole model for (216) Kleopatra triple system

The result's identifiers

  • Result code in IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F21%3A10437340" target="_blank" >RIV/00216208:11320/21:10437340 - isvavai.cz</a>

  • Result on the web

    <a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=rjN_oBObaC" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=rjN_oBObaC</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.1051/0004-6361/202140901" target="_blank" >10.1051/0004-6361/202140901</a>

Alternative languages

  • Result language

    angličtina

  • Original language name

    An advanced multipole model for (216) Kleopatra triple system

  • Original language description

    Aims. To interpret adaptive-optics observations of (216) Kleopatra, we need to describe an evolution of multiple moons orbiting an extremely irregular body and include their mutual interactions. Such orbits are generally non-Keplerian and orbital elements are not constants. Methods. Consequently, we used a modified N-body integrator, which was significantly extended to include the multipole expansion of the gravitational field up to the order l = 10. Its convergence was verified against the &apos;brute-force&apos; algorithm. We computed the coefficients C-lm, S-lm for Kleopatra&apos;s shape, assuming a constant bulk density. For Solar System applications, it was also necessary to implement a variable distance and geometry of observations. Our chi(2) metric then accounts for the absolute astrometry, the relative astrometry (second moon with respect to the first), angular velocities, and silhouettes, constraining the pole orientation. This allowed us to derive the orbital elements of Kleopatra&apos;s two moons. Results. Using both archival astrometric data and new VLT/SPHERE observations (ESO LP 199.C-0074), we were able to identify the true periods of the moons, P-1 = (1.822359 +/- 0.004156) d, P-2 = (2.745820 +/- 0.004820) d. They orbit very close to the 3:2 mean-motion resonance, but their osculating eccentricities are too small compared to other perturbations (multipole, mutual), meaning that regular librations of the critical argument are not present. The resulting mass of Kleopatra, m(1) = (1.49 +/- 0.16) x 10(-12) M-circle dot or 2.97 x 10(18) kg, is significantly lower than previously thought. An implication explained in the accompanying paper is that (216) Kleopatra is a critically rotating body.

  • Czech name

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • OECD FORD branch

    10308 - Astronomy (including astrophysics,space science)

Result continuities

  • Project

    Result was created during the realization of more than one project. More information in the Projects tab.

  • Continuities

    P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Others

  • Publication year

    2021

  • Confidentiality

    S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Data specific for result type

  • Name of the periodical

    Astronomy &amp; Astrophysics

  • ISSN

    0004-6361

  • e-ISSN

  • Volume of the periodical

    653

  • Issue of the periodical within the volume

    září

  • Country of publishing house

    FR - FRANCE

  • Number of pages

    9

  • Pages from-to

    A56

  • UT code for WoS article

    000694212400004

  • EID of the result in the Scopus database

    2-s2.0-85114801327