Very Slow Rotators from Tidally Synchronized Binaries
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10422433" target="_blank" >RIV/00216208:11320/20:10422433 - isvavai.cz</a>
Výsledek na webu
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=R26reJZ5KF" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=R26reJZ5KF</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/2041-8213/ab8311" target="_blank" >10.3847/2041-8213/ab8311</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
Very Slow Rotators from Tidally Synchronized Binaries
Popis výsledku v původním jazyce
A recent examination of K2 lightcurves indicates that similar to 15% of Jupiter Trojans have very slow rotation (spin periods P-s > 100 hr). Here we consider the possibility that these bodies formed as equal-size binaries in the massive outer disk at similar to 20-30 au. Prior to their implantation as Jupiter Trojans, tight binaries tidally evolved toward a synchronous state with P-s similar to P-b, where P-b is the binary orbit period. They may have been subsequently dissociated by impacts and planetary encounters with at least one binary component retaining its slow rotation. Surviving binaries on Trojan orbits would continue to evolve by tides and spin-changing impacts over 4.5 Gyr. To explain the observed fraction of slow rotators, we find that at least similar to 15%-20% of outer disk bodies with diameters 15 D a(b)/R less than or similar to 30, where a(b) is the binary semimajor axis and R = D/2. The mechanism proposed here could also explain very slow rotators found in other small-body populations.
Název v anglickém jazyce
Very Slow Rotators from Tidally Synchronized Binaries
Popis výsledku anglicky
A recent examination of K2 lightcurves indicates that similar to 15% of Jupiter Trojans have very slow rotation (spin periods P-s > 100 hr). Here we consider the possibility that these bodies formed as equal-size binaries in the massive outer disk at similar to 20-30 au. Prior to their implantation as Jupiter Trojans, tight binaries tidally evolved toward a synchronous state with P-s similar to P-b, where P-b is the binary orbit period. They may have been subsequently dissociated by impacts and planetary encounters with at least one binary component retaining its slow rotation. Surviving binaries on Trojan orbits would continue to evolve by tides and spin-changing impacts over 4.5 Gyr. To explain the observed fraction of slow rotators, we find that at least similar to 15%-20% of outer disk bodies with diameters 15 D a(b)/R less than or similar to 30, where a(b) is the binary semimajor axis and R = D/2. The mechanism proposed here could also explain very slow rotators found in other small-body populations.
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
<a href="/cs/project/GA18-06083S" target="_blank" >GA18-06083S: Vývoj pevných těles v protoplanetárních discích a během kolizí</a><br>
Návaznosti
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)
Ostatní
Rok uplatnění
2020
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Astrophysical Journal Letters
ISSN
2041-8205
e-ISSN
—
Svazek periodika
893
Číslo periodika v rámci svazku
1
Stát vydavatele periodika
US - Spojené státy americké
Počet stran výsledku
5
Strana od-do
L16
Kód UT WoS článku
000526405000001
EID výsledku v databázi Scopus
2-s2.0-85085124431