Video Experimental Relacionado
Updated: May 7, 2026
07:46
Setting Limits on Supersymmetry Using Simplified Models
Published on: November 16, 2013
La supernova de tipo Ia SNLS-03D3bb proviene de una estrella enana blanca de masa super-Chandrasekhar
D Andrew Howell1, Mark Sullivan, Peter E Nugent
1Department of Astronomy and Astrophysics, University of Toronto, 60 St George Street, Toronto, Ontario M5S 3H8, Canada. howell@astro.utoronto.ca
Nature
|September 22, 2006
Resumen
Las observaciones de una supernova peculiar sugieren que algunas supernovas de tipo Ia pueden originarse de los progenitores de la masa super-Chandrasekhar. Este hallazgo desafía el modelo estándar y puede explicar los eventos de sobreluminosidad en poblaciones estelares jóvenes.
Área de la Ciencia:
- Cosmología Cosmología.
- La astrofísica es la astrofísica.
- Evolución Estelar Evolución Estelar
Sus antecedentes:
- Las supernovas de tipo Ia son cruciales para inferir la acelerada expansión del Universo y la existencia de la energía oscura.
- Generalmente se acepta que estas supernovas son las explosiones termonucleares de enanas blancas de carbono y oxígeno que alcanzan la masa de Chandrasekhar (1,4 masas solares).
- Este límite de masa se considera un disparador estándar, lo que los convierte en fiables indicadores de distancia cósmica.
Objetivo del estudio:
- Para investigar la naturaleza de una supernova de alto desplazamiento al rojo, SNLS-03D3bb, con propiedades inusuales.
- Para determinar si SNLS-03D3bb se originó de un progenitor que excede la masa de Chandrasekhar.
- Explorar las implicaciones de las supernovas de masa super-Chandrasekhar para la cosmología y las poblaciones estelares.
Principales métodos:
- Análisis de los datos de observación de la supernova de alto desplazamiento al rojo SNLS-03D3bb.bb.
- Comparación de la luminosidad y la energía cinética de SNLS-03D3bb con modelos teóricos.
- Examen de las implicaciones de la masa progenitora basado en las características observadas de supernovas.
Principales resultados:
- SNLS-03D3bb exhibe una luminosidad excepcionalmente alta y una baja energía cinética.
- Estas propiedades implican fuertemente una estrella progenitora con una masa que excede el límite de Chandrasekhar (super-Chandrasekhar-masa).
- Este tipo de supernova puede ocurrir preferentemente en poblaciones estelares jóvenes, lo que podría explicar los eventos superluminosos en dichos entornos.
Conclusiones:
- La existencia de supernovas de masa super-Chandrasekhar desafía la suposición de una masa progenitora uniforme para los eventos de tipo Ia.
- Estos eventos pueden no adherirse a relaciones estandarizables, lo que afecta su uso como indicadores de distancia.
- Los futuros estudios cosmológicos deben tener en cuenta la posible contaminación de estas supernovas inusuales.
Videos de Conceptos Relacionados
02:45Nuclear Fusion
The process of converting very light nuclei into heavier nuclei is also accompanied by the conversion of mass into large amounts of energy, a process called fusion. The principal source of energy in the sun is a net fusion reaction in which four hydrogen nuclei fuse and ultimately produce one helium nucleus and two positrons.
A helium nucleus has a mass that is 0.7% less than that of four hydrogen nuclei; this lost mass is converted into energy during the fusion. This reaction produces about...
A helium nucleus has a mass that is 0.7% less than that of four hydrogen nuclei; this lost mass is converted into energy during the fusion. This reaction produces about...
01:18Conservation of Angular Momentum: Application
A system's total angular momentum remains constant if the net external torque acting on the system is zero. Examples of such systems include a freely spinning bicycle tire that slows over time due to torque arising from friction, or the slowing of Earth's rotation over millions of years due to frictional forces exerted on tidal deformations. However in the absence of a net external torque, the angular momentum remains conserved. The conservation of angular momentum principle requires a change...
01:21Schwarzschild Radius and Event Horizon
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 velocity with the...
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 velocity with the...
01:10Detection of Black Holes
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
01:14Atomic Nuclei: Nuclear Spin State Population Distribution
Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
01:14Gravitation Between Spherically Symmetric Masses
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.