Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F12%3A10129181" target="_blank" >RIV/00216208:11320/12:10129181 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/12:00388364

Výsledek na webu

<a href="http://dx.doi.org/10.1016/j.icarus.2011.11.026" target="_blank" >http://dx.doi.org/10.1016/j.icarus.2011.11.026</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.icarus.2011.11.026" target="_blank" >10.1016/j.icarus.2011.11.026</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries

Popis výsledku v původním jazyce

Our photometric observations of 18 main-belt binary systems in more than one apparition revealed a strikingly high number of 15 having positively re-observed mutual events in the return apparitions. Our simulations of the survey showed that it cannot bedue to an observational selection effect and that the data strongly suggest that poles of mutual orbits between components of binary asteroids in the primary size range 3-8 km are not distributed randomly: The null hypothesis of an isotropic distributionof the orbit poles is rejected at a confidence level greater than 99.99%. Binary orbit poles concentrate at high ecliptic latitudes, within 300 of the poles of the ecliptic. We propose that the binary orbit poles oriented preferentially up/down-right are due to either of the two processes: (i) the YORP tilt of spin axes of their parent bodies toward the asymptotic states near obliquities 0 degrees and 180 degrees (pre-formation mechanism) or (ii) the YORP tilt of spin axes of the primar

Název v anglickém jazyce

Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries

Popis výsledku anglicky

Our photometric observations of 18 main-belt binary systems in more than one apparition revealed a strikingly high number of 15 having positively re-observed mutual events in the return apparitions. Our simulations of the survey showed that it cannot bedue to an observational selection effect and that the data strongly suggest that poles of mutual orbits between components of binary asteroids in the primary size range 3-8 km are not distributed randomly: The null hypothesis of an isotropic distributionof the orbit poles is rejected at a confidence level greater than 99.99%. Binary orbit poles concentrate at high ecliptic latitudes, within 300 of the poles of the ecliptic. We propose that the binary orbit poles oriented preferentially up/down-right are due to either of the two processes: (i) the YORP tilt of spin axes of their parent bodies toward the asymptotic states near obliquities 0 degrees and 180 degrees (pre-formation mechanism) or (ii) the YORP tilt of spin axes of the primar

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

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)<br>Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2012

Kód důvěrnosti údajů

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

Název periodika

Icarus

ISSN

0019-1035

e-ISSN

—

Svazek periodika

218

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

19

Strana od-do

125-143

Kód UT WoS článku

000301637700011

EID výsledku v databázi Scopus

—