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Desalineación de la órbita del agujero negro en el binario de rayos X MAXI J1820+070
Juri Poutanen1,2,3, Alexandra Veledina1,2,3, Andrei V Berdyugin1
1Department of Physics and Astronomy, FI-20014 University of Turku, Finland.
Science (New York, N.Y.)
|February 24, 2022
Resumen
La desalineación de la órbita del agujero negro en los binarios de rayos X puede exceder los 40 °. Esta desalineación significativa, observada en MAXI J1820+070, puede sesgar las mediciones de masa y espín del agujero negro de los datos de rayos X.
Área de la Ciencia:
- La astrofísica
- Astronomía de rayos X
- Física de los agujeros negros
Sus antecedentes:
- Las firmas observacionales de los agujeros negros en binarios de rayos X están influenciadas por la masa, el giro, la tasa de acreción y la desalineación de la órbita de giro.
- Comprender estos parámetros es crucial para la caracterización precisa de los agujeros negros.
Objetivo del estudio:
- Para restringir el ángulo de desalineación de la órbita del agujero negro en el binario de rayos X MAXI J1820+070.
- Investigar las implicaciones de tales desalineaciones en las mediciones de parámetros de agujeros negros.
Principales métodos:
- Se utilizaron observaciones polarimétricas ópticas para determinar el ángulo de posición orbital binario.
- Combinado con los datos existentes sobre la orientación del chorro (rastreando el giro del agujero negro) y la inclinación orbital.
Principales resultados:
- Se determinó un límite inferior de 40° para el ángulo de desalineación de la órbita de giro en MAXI J1820+070.
- Esta desalineación significativa sugiere orígenes en la evolución binaria o la formación de agujeros negros.
Conclusiones:
- Las grandes desalineaciones de la órbita de espín están presentes en los binarios de rayos X de agujeros negros.
- Tales desalineaciones pueden introducir sesgos en la masa del agujero negro y las mediciones de espín derivadas de las observaciones de rayos X.
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