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El agua en Betelgeuse y Antares
1Planetary Systems Branch, Code 693, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.
Science (New York, N.Y.)
|February 28, 1998
Resumen
Las líneas de absorción de agua caliente detectadas en las atmósferas de las estrellas Betelgeuse y Antares revelan la abundancia de agua molecular. Este hallazgo proporciona información sobre la composición atmosférica de las estrellas frías.
Área de la Ciencia:
- La astronomía y la astrofísica.
- La espectroscopia es una técnica de espectroscopia.
Sus antecedentes:
- El análisis del espectro infrarrojo es crucial para comprender las atmósferas estelares.
- Estudios anteriores han explorado especies moleculares en entornos estelares.
Objetivo del estudio:
- Identificar y caracterizar las líneas de absorción de agua caliente en los espectros infrarrojos de Betelgeuse y Antares.
- Para determinar el origen y la abundancia de agua en las atmósferas de estas estrellas frías.
Principales métodos:
- Análisis de los espectros infrarrojos obtenidos para Betelgeuse y Antares.
- Identificación de las líneas de absorción cerca de 12,3 micrómetros (811-819 cm-1).
- Comparación de las características espectrales con los espectros de manchas solares umbrales.
Principales resultados:
- Detección de líneas de absorción de agua caliente originadas en las atmósferas estelares.
- Los espectros exhiben similitudes con los espectros umbrales de las manchas solares.
- El límite superior de temperatura en la región de formación de la línea es de 2800 K.
- La densidad de la columna de agua es (3 ± 2) x 1018 moléculas/cm2.
- La abundancia de agua en relación con el hidrógeno es de aproximadamente 10−7.
Conclusiones:
- Las moléculas de agua caliente están presentes en las atmósferas de Betelgeuse y Antares.
- Estas líneas de agua son indicativas de las condiciones que se encuentran en las estrellas frías y manchas solares.
- Los hallazgos contribuyen a comprender la composición química y la estructura térmica de las atmósferas estelares.
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