DETECTION OF THE YORP EFFECT FOR SMALL ASTEROIDS IN THE KARIN CLUSTER

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F16%3A10331707" target="_blank" >RIV/00216208:11320/16:10331707 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/0004-6256/151/6/164" target="_blank" >http://dx.doi.org/10.3847/0004-6256/151/6/164</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/0004-6256/151/6/164" target="_blank" >10.3847/0004-6256/151/6/164</a>

Jazyk výsledku

angličtina

Název v původním jazyce

DETECTION OF THE YORP EFFECT FOR SMALL ASTEROIDS IN THE KARIN CLUSTER

Popis výsledku v původním jazyce

The Karin cluster is a young asteroid family thought to have formed only similar or equal to 5.75 Myr ago. The young age can be demonstrated by numerically integrating the orbits of Karin cluster members backward in time and showing the convergence of the perihelion and nodal longitudes (as well as other orbital elements). Previous work has pointed out that the convergence is not ideal if the backward integration only accounts for the gravitational perturbations from the solar system planets. It improves when the thermal radiation force known as the Yarkovsky effect is accounted for. This argument can be used to estimate the spin obliquities of the Karin cluster members. Here we take advantage of the fast growing membership of the Karin cluster and show that the obliquity distribution of diameter D similar or equal to 1-2 km Karin asteroids is bimodal, as expected if the YORP effect acted to move obliquities toward extreme values (0 or 180). The measured magnitude of the effect is consistent with the standard YORP model. The surface thermal conductivity is inferred to be 0.07-0.2 W m(-1) K-1 (thermal inertia similar or equal to 300-500 J m(-2)K(-1) S-1/2). We find that the strength of the YORP effect is roughly of the nominal strength obtained for a collection of random Gaussian spheroids. These results are consistent with a surface composed of rough, rocky regolith. The obliquity values predicted here for 480 members of the Karin cluster can be validated by the light-curve inversion method.

Název v anglickém jazyce

DETECTION OF THE YORP EFFECT FOR SMALL ASTEROIDS IN THE KARIN CLUSTER

Popis výsledku anglicky

The Karin cluster is a young asteroid family thought to have formed only similar or equal to 5.75 Myr ago. The young age can be demonstrated by numerically integrating the orbits of Karin cluster members backward in time and showing the convergence of the perihelion and nodal longitudes (as well as other orbital elements). Previous work has pointed out that the convergence is not ideal if the backward integration only accounts for the gravitational perturbations from the solar system planets. It improves when the thermal radiation force known as the Yarkovsky effect is accounted for. This argument can be used to estimate the spin obliquities of the Karin cluster members. Here we take advantage of the fast growing membership of the Karin cluster and show that the obliquity distribution of diameter D similar or equal to 1-2 km Karin asteroids is bimodal, as expected if the YORP effect acted to move obliquities toward extreme values (0 or 180). The measured magnitude of the effect is consistent with the standard YORP model. The surface thermal conductivity is inferred to be 0.07-0.2 W m(-1) K-1 (thermal inertia similar or equal to 300-500 J m(-2)K(-1) S-1/2). We find that the strength of the YORP effect is roughly of the nominal strength obtained for a collection of random Gaussian spheroids. These results are consistent with a surface composed of rough, rocky regolith. The obliquity values predicted here for 480 members of the Karin cluster can be validated by the light-curve inversion method.

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA13-01308S" target="_blank" >GA13-01308S: Dynamika malých těles sluneční soustavy</a><br>

Návaznosti

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

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název periodika

Astronomical Journal

ISSN

0004-6256

e-ISSN

—

Svazek periodika

151

Číslo periodika v rámci svazku

6

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

11

Strana od-do

—

Kód UT WoS článku

000377990300031

EID výsledku v databázi Scopus

2-s2.0-84975478256