Video Experimental Relacionado
Updated: Jul 8, 2026
07:46
Setting Limits on Supersymmetry Using Simplified Models
Published on: November 15, 2013
Los bariones faltantes y el medio intergaláctico caliente caliente
Fabrizio Nicastro1, Smita Mathur, Martin Elvis
1Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA. fnicastro@cfa.harvard.edu
Science (New York, N.Y.)
|January 5, 2008
Resumen
Los cosmólogos están buscando los bariones faltantes, que se cree que están en un medio intergaláctico cálido y caliente. Encontrar estos escurridizos ingredientes cósmicos es clave para validar nuestra comprensión del universo.
Área de la Ciencia:
- Cosmología Cosmología.
- La astrofísica es la astrofísica.
- El medio intergaláctico es el medio intergaláctico.
Sus antecedentes:
- El universo observable contiene sólo la mitad de la materia bariónica esperada.
- Se supone que la mayoría de los bariones existen en un medio intergaláctico cálido y caliente (WHIM).
- Se cree que esta materia faltante se calienta con el choque durante la formación de la estructura cósmica.
Objetivo del estudio:
- Para localizar los bariones que faltan en el universo.
- Para crear un inventario completo de la materia bariónica.
- Para probar el modelo cosmológico estándar.
Principales métodos:
- La astronomía observacional es la astronomía de las observaciones.
- Simulaciones cosmológicas de simulaciones.
- Análisis de las propiedades del gas intergaláctico.
Principales resultados:
- El estudio se centra en la distribución teórica de los bariones faltantes.
- Destaca las propiedades esperadas del medio intergaláctico cálido y caliente.
- Hace hincapié en la necesidad de evidencia observacional.
Conclusiones:
- Confirmar la existencia y distribución de los bariones faltantes es crucial.
- Esta investigación impacta nuestra validación del modelo cosmológico estándar.
- Se requieren más esfuerzos de observación para detectar el medio intergaláctico cálido y caliente.
Videos de Conceptos Relacionados
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...
04:01Real Gases: Effects of Intermolecular Forces and Molecular Volume Deriving Van der Waals Equation
Thus far, the ideal gas law, PV = nRT, has been applied to a variety of different types of problems, ranging from reaction stoichiometry and empirical and molecular formula problems to determining the density and molar mass of a gas. However, the behavior of a gas is often non-ideal, meaning that the observed relationships between its pressure, volume, and temperature are not accurately described by the gas laws.
01:23Heat Capacities of an Ideal Gas II
For a system that undergoes a thermodynamic process at a constant volume condition, the heat absorbed is used only to increase the system's internal energy and not for doing any kind of work. While for a system undergoing a thermodynamic process under a constant pressure condition, the amount of heat absorbed is used not only for increasing the internal energy (as a function of temperature) but also for doing some work. The molar heat capacity is the amount of heat required to increase the...
01:25Heat Capacities of an Ideal Gas III
The number of independent ways a gas molecule can move along straight line, rotate, and vibrate is called its degrees of freedom. Supposing d represents the number of degrees of freedom of an ideal gas, the molar heat capacity at constant volume of an ideal gas in terms of d is
01:17Radiation: Applications
The average temperature of Earth is the subject of much current discussion. Earth is in radiative contact with both the Sun and dark space; it receives almost all its energy from the radiation of the Sun and reflects some of it into outer space. Dark space is very cold, about 3 K, so Earth radiates energy into it. For instance, heat transfer occurs from soil and grasses, the rate of which can be so rapid that frost can occur on clear summer evenings, even in warm latitudes.
The average...
The average...
01:14Heat Capacities of an Ideal Gas I
Heat capacity is the ratio of heat absorbed by the substance corresponding to its temperature change. It is also called thermal capacity and the SI unit of heat capacity is J/K. Whereas, specific heat capacity is defined as the amount of heat necessary to change the temperature of 1 kg of a substance by 1 K and is also called massic heat capacity. Its SI unit is J/kg⋅K.
Molar heat capacity quantifies the ratio of the amount of heat added (or removed) to increase (or decrease) the temperature of...
Molar heat capacity quantifies the ratio of the amount of heat added (or removed) to increase (or decrease) the temperature of...