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Schwarzschild Radius and Event Horizon

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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
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Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
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The gravitational potential energy between two spherically symmetric bodies can be calculated from the masses and the distance between the bodies, assuming that the center of mass is concentrated at the respective centers of the bodies.
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In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
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Second Order systems I01:20

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A servo system exemplifies a second-order system, featuring a proportional controller and load elements that ensure the output position aligns with the input position. The relationship between these components is described by a second-order differential equation. Applying the Laplace transform under zero initial conditions yields the transfer function, showing how inputs are converted to outputs in the system.
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Second Order systems II01:18

Second Order systems II

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In an underdamped second-order system, where the damping ratio ζ is between 0 and 1, a unit-step input results in a transfer function that, when transformed using the inverse Laplace method, reveals the output response. The output exhibits a damped sinusoidal oscillation, and the difference between the input and output is termed the error signal. This error signal also demonstrates damped oscillatory behavior. Eventually, as the system reaches a steady state, the error diminishes to zero.
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Setting Limits on Supersymmetry Using Simplified Models
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Un candidato a un sistema de agujero negro binario supermasivo de subparsec.

Todd A Boroson1, Tod R Lauer

  • 1National Optical Astronomy Observatory, Tucson, Arizona 85726, USA. tyb@noao.edu

Nature
|March 6, 2009
PubMed
Resumen
Este resumen es generado por máquina.

Los astrónomos descubrieron un cuásar único, SDSS J153636.22+044127.0, que es probablemente un sistema binario de agujero negro supermasivo. Este hallazgo apoya la teoría de que tales sistemas son comunes en el universo.

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Área de la Ciencia:

  • La astrofísica es la astrofísica.
  • Cosmología Cosmología.
  • Evolución de la galaxia Evolución de la galaxia.

Sus antecedentes:

  • Las fusiones de galaxias son un mecanismo primario para la formación y el crecimiento de galaxias.
  • Se sabe que la mayoría de las galaxias grandes albergan agujeros negros supermasivos (SMBH) en sus centros.
  • La prevalencia de SMBH sugiere que los sistemas binarios SMBH deberían ser comunes debido a las fusiones de galaxias.

Objetivo del estudio:

  • Para identificar y caracterizar sistemas potenciales de agujeros negros supermasivos binarios.
  • Para investigar las propiedades inusuales de los cuásares que pueden indicar la presencia de un binario SMBH.

Principales métodos:

  • Análisis espectroscópico del cuásar SDSS J153636.22+044127.0.0 en el que se encuentra.
  • Identificación de distintos sistemas de líneas de emisión y absorción dentro del espectro del cuásar.
  • Análisis de separación por velocidad de las características espectrales.

Principales resultados:

  • El cuásar SDSS J153636.22+044127.0 exhibe dos sistemas de emisión de línea ancha con una separación de velocidad de 3.500 km/s.
  • Se detectó un tercer sistema de líneas de absorción no resueltas a una velocidad intermedia.
  • Estas características espectrales son únicas entre todos los cuásares conocidos.

Conclusiones:

  • Las características espectrales observadas sugieren fuertemente que SDSS J153636.22+044127.0 es un sistema binario de agujero negro supermasivo.
  • Las masas estimadas de los agujeros negros son 10^7.3 y 10^8.9 masas solares.
  • Se predice que el sistema binario tendrá un período orbital de aproximadamente 100 años y una separación de aproximadamente 0,1 parsec.