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Detailed Analysis of the Asteroid Pair (6070) Rheinland and (54827) 2001 NQ8

Identifikátory výsledku

  • Kód výsledku v IS VaVaI

    <a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10367523" target="_blank" >RIV/00216208:11320/17:10367523 - isvavai.cz</a>

  • Výsledek na webu

    <a href="http://dx.doi.org/10.3847/1538-3881/aa72ea" target="_blank" >http://dx.doi.org/10.3847/1538-3881/aa72ea</a>

  • DOI - Digital Object Identifier

    <a href="http://dx.doi.org/10.3847/1538-3881/aa72ea" target="_blank" >10.3847/1538-3881/aa72ea</a>

Alternativní jazyky

  • Jazyk výsledku

    angličtina

  • Název v původním jazyce

    Detailed Analysis of the Asteroid Pair (6070) Rheinland and (54827) 2001 NQ8

  • Popis výsledku v původním jazyce

    The existence of asteroid pairs, two bodies on similar heliocentric orbits, reveals an. ongoing process of rotational fission among asteroids. This newly found class of objects has not been studied in detail yet. Here we choose asteroids (6070) Rheinland and (54827) 2001 NQ8, the most suitable pair for an in-depth analysis. First, we use available optical photometry to determine their rotational state and convex shapes. Rotational pole of Rheinland is very near the south ecliptic pole with a latitude uncertainty of about 10 degrees. There are two equivalent solutions for the pole of 2001 NQ8, either (72 degrees, -49 degrees) or (242 degrees, -46 degrees) (ecliptic longitude and latitude). In both cases, the longitude values have about 10 degrees uncertainty and the latitude values have about 15 degrees uncertainty (both 3 sigma uncertainties). The sidereal rotation period of 2001 NQ8 is 5.877186 +/- 0.000002. hr. Second, we construct a precise numerical integrator to determine the past state vectors of the pair&apos;s components, namely their heliocentric positions and velocities, and orientation of their spin vectors. Using this new tool, we investigate the origin of the (6070) Rheinland and (54827) 2001 NQ8 pair. We find a formal age solution of 16.34 +/- 0.04 kyr. This includes effects of the most massive objects in the asteroid belt (Ceres, Pallas, and Vesta), but the unaccounted gravitational perturbations from other asteroids may imply that the realistic age uncertainty is slightly larger than its formal value. Analyzing results from our numerical simulation to 250 kya, we argue against a possibility that this pair would allow an older age. Initial spin vectors of the two asteroids, at the moment of their separation, were not collinear, but tilted by 38 degrees +/- 12 degrees.

  • Název v anglickém jazyce

    Detailed Analysis of the Asteroid Pair (6070) Rheinland and (54827) 2001 NQ8

  • Popis výsledku anglicky

    The existence of asteroid pairs, two bodies on similar heliocentric orbits, reveals an. ongoing process of rotational fission among asteroids. This newly found class of objects has not been studied in detail yet. Here we choose asteroids (6070) Rheinland and (54827) 2001 NQ8, the most suitable pair for an in-depth analysis. First, we use available optical photometry to determine their rotational state and convex shapes. Rotational pole of Rheinland is very near the south ecliptic pole with a latitude uncertainty of about 10 degrees. There are two equivalent solutions for the pole of 2001 NQ8, either (72 degrees, -49 degrees) or (242 degrees, -46 degrees) (ecliptic longitude and latitude). In both cases, the longitude values have about 10 degrees uncertainty and the latitude values have about 15 degrees uncertainty (both 3 sigma uncertainties). The sidereal rotation period of 2001 NQ8 is 5.877186 +/- 0.000002. hr. Second, we construct a precise numerical integrator to determine the past state vectors of the pair&apos;s components, namely their heliocentric positions and velocities, and orientation of their spin vectors. Using this new tool, we investigate the origin of the (6070) Rheinland and (54827) 2001 NQ8 pair. We find a formal age solution of 16.34 +/- 0.04 kyr. This includes effects of the most massive objects in the asteroid belt (Ceres, Pallas, and Vesta), but the unaccounted gravitational perturbations from other asteroids may imply that the realistic age uncertainty is slightly larger than its formal value. Analyzing results from our numerical simulation to 250 kya, we argue against a possibility that this pair would allow an older age. Initial spin vectors of the two asteroids, at the moment of their separation, were not collinear, but tilted by 38 degrees +/- 12 degrees.

Klasifikace

  • Druh

    J<sub>imp</sub> - Článek v periodiku v databázi Web of Science

  • CEP obor

  • OECD FORD obor

    10308 - Astronomy (including astrophysics,space science)

Návaznosti výsledku

  • Projekt

    Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

  • Návaznosti

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

Ostatní

  • Rok uplatnění

    2017

  • Kód důvěrnosti údajů

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

Údaje specifické pro druh výsledku

  • Název periodika

    The Astronomical Journal

  • ISSN

    0004-6256

  • e-ISSN

  • Svazek periodika

    153

  • Číslo periodika v rámci svazku

    6

  • Stát vydavatele periodika

    US - Spojené státy americké

  • Počet stran výsledku

    17

  • Strana od-do

  • Kód UT WoS článku

    000402902400003

  • EID výsledku v databázi Scopus