OSSOS XX: The Meaning of Kuiper Belt Colors

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10422459" target="_blank" >RIV/00216208:11320/20:10422459 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mPt-3dZWz8" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mPt-3dZWz8</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/ab98fb" target="_blank" >10.3847/1538-3881/ab98fb</a>

Jazyk výsledku

angličtina

Název v původním jazyce

OSSOS XX: The Meaning of Kuiper Belt Colors

Popis výsledku v původním jazyce

Observations show that 100 km class Kuiper Belt objects (KBOs) can be divided into (at least) two color groups, red (R;g - i &lt; 1.2) and very red (VR;g - i &gt; 1.2), reflecting a difference in their surface composition. This is thought to imply that KBOs formed over a relatively wide range of radial distance,r. The cold classicals at 42 au r &lt; 47 au are predominantly VR, and known Neptune Trojans atr30 au are mostly R. Intriguingly, however, the dynamically hot KBOs show a mix of R and VR colors and no correlation of color withr. Here we perform migration/instability simulations where the Kuiper Belt is populated from an extended planetesimal disk. We find that the color observations can be best understood if R objects formed atr r* and VR objects atr &gt; r*, with 30 au r* r* &lt; 40 au would explain why the VR objects in the dynamically hot population have smaller orbital inclinations than the R objects, because the orbital excitation from Neptune weakens for orbits starting beyond 30 au. Possible causes of the R-VR color bimodality are discussed.

Název v anglickém jazyce

OSSOS XX: The Meaning of Kuiper Belt Colors

Popis výsledku anglicky

Observations show that 100 km class Kuiper Belt objects (KBOs) can be divided into (at least) two color groups, red (R;g - i &lt; 1.2) and very red (VR;g - i &gt; 1.2), reflecting a difference in their surface composition. This is thought to imply that KBOs formed over a relatively wide range of radial distance,r. The cold classicals at 42 au r &lt; 47 au are predominantly VR, and known Neptune Trojans atr30 au are mostly R. Intriguingly, however, the dynamically hot KBOs show a mix of R and VR colors and no correlation of color withr. Here we perform migration/instability simulations where the Kuiper Belt is populated from an extended planetesimal disk. We find that the color observations can be best understood if R objects formed atr r* and VR objects atr &gt; r*, with 30 au r* r* &lt; 40 au would explain why the VR objects in the dynamically hot population have smaller orbital inclinations than the R objects, because the orbital excitation from Neptune weakens for orbits starting beyond 30 au. Possible causes of the R-VR color bimodality are discussed.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

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)

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název periodika

The Astronomical Journal

ISSN

0004-6256

e-ISSN

—

Svazek periodika

160

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

13

Strana od-do

46

Kód UT WoS článku

000546813100001

EID výsledku v databázi Scopus

2-s2.0-85088030169