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In inductively coupled plasma–mass spectrometry (ICP–MS), an inductively coupled plasma (ICP) torch is used as an atomizer and ionizer. Solid samples are dissolved and volatilized before being introduced into the high-temperature argon plasma, while solution samples are nebulized and passed through the high-temperature argon plasma. Plasma dissociates the analytes and ionizes their component atoms to form a mixture of positive ions and molecular species. The positive ions are then passed on to...
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Scattering And Absorption of Light in Planetary Regoliths
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Cráteres de impacto en Venus: análisis inicial desde Magallanes.

R J Phillips, R E Arvidson, J M Boyce

    Science (New York, N.Y.)
    |April 12, 1991
    PubMed
    Resumen

    Venus Venus Venus es el nombre de Venus.

    Área de la Ciencia:

    • Ciencias planetarias Ciencias planetarias.
    • Geología Geología Geología.
    • El cráter de impacto es el cráter de impacto.

    Sus antecedentes:

    • Las características de la superficie de Venus proporcionan pistas sobre su historia geológica.
    • Las imágenes de radar son cruciales para estudiar la atmósfera opaca de Venus.
    • Comprender los cráteres de impacto ayuda a determinar la edad de la superficie y la actividad geológica.

    Objetivo del estudio:

    • Para analizar cráteres de impacto en Venus utilizando datos de radar de Magallanes.
    • Para investigar la influencia de la atmósfera de Venus en la formación de cráteres.
    • Para evaluar la actividad geológica y la edad de la superficie de Venus.

    Principales métodos:

    • Análisis de imágenes de radar de Magallanes que cubren el 15% de Venus.

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  • Identificación y caracterización de 135 probables cráteres de impacto.
  • Comparación de las características observadas del cráter con modelos de impacto.

    • Principales resultados:

    • Los cráteres de más de 15 km exhiben picos centrales o anillos de picos.
    • Los cráteres más pequeños muestran múltiples pisos o agrupaciones, lo que indica la ruptura atmosférica.
    • La atmósfera de Venus limita la formación de pequeños cráteres (<3 km) y reduce el número de cráteres intermedios (<25 km).
    • Los depósitos de eyección muestran características inesperadas, posiblemente debido al arrastre atmosférico y los flujos superficiales.
    • Las crateras están rodeadas de zonas de bajo albedo de radar, lo que sugiere una deformación de onda de choque.
    • La ausencia de cráteres en algunas regiones apunta a un resurgimiento volcánico.

    Conclusiones:

    • Venus exhibe un rango de edades superficiales (0-800 millones de años).
    • El planeta es geológicamente activo, con procesos de rejuvenecimiento en curso.
    • Las interacciones atmosféricas modifican significativamente los procesos de cráteres de impacto en Venus.