Shape and spin distributions of asteroid populations from brightness variation estimates and large databases

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10367524" target="_blank" >RIV/00216208:11320/17:10367524 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201629850" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201629850</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201629850" target="_blank" >10.1051/0004-6361/201629850</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Shape and spin distributions of asteroid populations from brightness variation estimates and large databases

Popis výsledku v původním jazyce

We model the observed brightness variation of a target population by considering its cumulative distribution function (CDF) caused by the joint distribution function of two fundamental shape and spin indicators. These are the shape elongation and the spin latitude of a simple ellipsoidal model. The main advantage of the model is that we can derive analytical basis functions that yield the observed CDF as a function of the shape and spin distribution. The inverse problem can be treated linearly. Even though the inaccuracy of the model is considerable, databases of thousands of targets should yield some information on the distribution. We employ numerical simulations to establish this and analyse photometric databases that provide sufficiently large numbers of data points for reliable brightness variation estimates.

Název v anglickém jazyce

Shape and spin distributions of asteroid populations from brightness variation estimates and large databases

Popis výsledku anglicky

We model the observed brightness variation of a target population by considering its cumulative distribution function (CDF) caused by the joint distribution function of two fundamental shape and spin indicators. These are the shape elongation and the spin latitude of a simple ellipsoidal model. The main advantage of the model is that we can derive analytical basis functions that yield the observed CDF as a function of the shape and spin distribution. The inverse problem can be treated linearly. Even though the inaccuracy of the model is considerable, databases of thousands of targets should yield some information on the distribution. We employ numerical simulations to establish this and analyse photometric databases that provide sufficiently large numbers of data points for reliable brightness variation estimates.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA15-04816S" target="_blank" >GA15-04816S: Celkový obraz hlavního pásu planetek - fyzikální vlastnosti planetek odvozené inverzí optické a infračervené fotometrie</a><br>

Návaznosti

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

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Astronomy &amp; Astrophysics [online]

ISSN

1432-0746

e-ISSN

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Svazek periodika

601

Číslo periodika v rámci svazku

květen

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

16

Strana od-do

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Kód UT WoS článku

000402313500139

EID výsledku v databázi Scopus

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