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La expansión de la bola de fuego de Nova Delphini 2013

G H Schaefer¹, T ten Brummelaar¹, D R Gies²

¹The CHARA Array of Georgia State University, Mount Wilson Observatory, Mount Wilson, California 91023, USA.

|November 4, 2014

Resumen

Las primeras observaciones de Nova Delphini 2013 revelan su estructura utilizando interferometría de infrarrojo cercano. El estudio sugiere una forma bipolar que se desarrolla rápidamente después de la fuga termonuclear en la enana blanca.

Área de la Ciencia:

La astronomía es la astronomía.
La astrofísica es la astrofísica.
Evolución Estelar Evolución Estelar

Sus antecedentes:

Las novas clásicas son el resultado de escapadas termonucleares en enanas blancas en acreción en sistemas binarios.
Las estructuras de eyección en etapa tardía pueden surgir de interacciones de envoltura común o explosiones bipolares intrínsecas.
Los estudios de estructura de nova en fase temprana son difíciles debido a la alta resolución espacial requerida.

Objetivo del estudio:

Para investigar la estructura de la fase temprana y la expansión de Nova Delphini 2013.
Para determinar la distancia a Nova Delphini 2013 utilizando su expansión angular y velocidad radial.

Principales métodos:

Mediciones interferométricas en el infrarrojo cercano del tamaño angular de Nova Delphini 2013, comenzando un día después de la explosión.
Monitoreo continuo durante los primeros 43 días para rastrear los cambios en la tasa de expansión aparente.
Combinando datos de expansión angular con mediciones de velocidad radial para la determinación de distancias.

Principales resultados:

Los cambios observados en la velocidad de expansión son consistentes con un modelo de un núcleo ópticamente grueso y una envolvente difusa.
Se detectó una elipticidad en la distribución de la luz, lo que indica una estructura prolata o bipolar para el segundo día.
Se obtuvo una distancia geométrica de 4,54 ± 0,59 kiloparsecs para Nova Delphini 2013.

Conclusiones:

Nova Delphini 2013 exhibió una estructura bipolar al principio de su evolución.
La profundidad óptica de la eyección en expansión cambia a medida que se dispersa.
La distancia derivada proporciona un parámetro crucial para la comprensión de este evento clásico de nova.

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