Shape of scoria cones on Mars: Insights from numerical modeling of ballistic pathways

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F14%3A10283575" target="_blank" >RIV/00216208:11320/14:10283575 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985530:_____/14:00432104 RIV/00216208:11310/14:10283575

Výsledek na webu

<a href="http://dx.doi.org/10.1016/j.epsl.2014.09.002" target="_blank" >http://dx.doi.org/10.1016/j.epsl.2014.09.002</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1016/j.epsl.2014.09.002" target="_blank" >10.1016/j.epsl.2014.09.002</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Shape of scoria cones on Mars: Insights from numerical modeling of ballistic pathways

Popis výsledku v původním jazyce

Morphological observations of scoria cones on Mars show that their cross-sectional shapes are different from those on Earth. Due to lower gravity and atmospheric pressure on Mars, particles are spread over a larger area than on Earth. Hence, erupted volumes are typically not large enough for the flank slopes to attain the angle of repose, in contrast to Earth where this is common. The distribution of ejected material forming scoria cones on Mars, therefore, is ruled mainly by ballistic distribution andnot by redistribution of flank material by avalanching after the static angle of repose is reached. As a consequence, the flank slopes of the Martian scoria cones do not reach the critical angle of repose in spite of a large volume of ejected material. Therefore, the topography of scoria cones on Mars is governed mainly by ballistic distribution of ejected particles and is not influenced by redistribution of flank material by avalanching. The growth of a scoria cone can be studied numeri

Název v anglickém jazyce

Shape of scoria cones on Mars: Insights from numerical modeling of ballistic pathways

Popis výsledku anglicky

Morphological observations of scoria cones on Mars show that their cross-sectional shapes are different from those on Earth. Due to lower gravity and atmospheric pressure on Mars, particles are spread over a larger area than on Earth. Hence, erupted volumes are typically not large enough for the flank slopes to attain the angle of repose, in contrast to Earth where this is common. The distribution of ejected material forming scoria cones on Mars, therefore, is ruled mainly by ballistic distribution andnot by redistribution of flank material by avalanching after the static angle of repose is reached. As a consequence, the flank slopes of the Martian scoria cones do not reach the critical angle of repose in spite of a large volume of ejected material. Therefore, the topography of scoria cones on Mars is governed mainly by ballistic distribution of ejected particles and is not influenced by redistribution of flank material by avalanching. The growth of a scoria cone can be studied numeri

Druh

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

CEP obor

DE - Zemský magnetismus, geodesie, geografie

OECD FORD obor

—

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2014

Kód důvěrnosti údajů

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

Název periodika

Earth and Planetary Science Letters

ISSN

0012-821X

e-ISSN

—

Svazek periodika

406

Číslo periodika v rámci svazku

November

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

10

Strana od-do

14-23

Kód UT WoS článku

000344211200003

EID výsledku v databázi Scopus

—